XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes clporeiso eoatpaeayssesand systems planetary be stability. resonant their can of problem proprieties dynam- this of ical understanding of initial an visualization to important The very time. short-period a of exoplanets over resonance and mean-motion 2:1 system the in Neptune-Pluto the the of the of on orbits animations Based present we systems. platform, Mathematica two-planet the in resonance power. due analysis worldwide great used its soft- increasingly to a been Mathematica, has chose that We ware configurations worlds. unusual new these such of of investigation importance the great advanced of for of be So- can implementation own techniques the manipulation our Thus, to System. compared are lar when exoplanets diverse that more learned much for have waiting We still them confirmation. and 3000 of over most known identified candidates, recently are additional has exoplanets satellite 1000 Kepler the over Sys- systems, Today, Solar planetary the of of tem. observation features the from the chang- drawn on decades, mainly break- view past major the our the of ing of astronomy or- one in been planets throughs has extra-solar inves- stars of dynamics other discovery biting planetary The in used tigations. be Math- pro- can software techniques manipulation ematica how algebraic on the by study vided a presents work This ie ca tofeia aUiesdd eSa al (ta- Paulo S˜ao de [email protected]). Universidade da Atmosf´ericas Ciˆencias (nfa 2 Paulo S˜ao [email protected]). de Universidade Atmosf´ericas da Ciˆencias 1 Conferencias) de (Serie RevMexAA OTAEI H TD FPLANETARY OF STUDY THE IN SOFTWARE A-S nttt eAtooi,Go´sc e Geof´ısica Astronomia, de e Instituto Geof´ısica - Astronomia, IAG-USP de Instituto - IAG-USP h aeta efcsi h / mean-motion 2/1 the is focus we that case The .F Aguero F. N. H S FTEMATHEMATICA THE OF USE THE LNTR SYSTEMS PLANETARY 1 DYNAMICS n .A Michtchenko A. T. and , 44 2–2 (2014) 129–225 , 2 ABSTRACTS - o8% fteclassical the of 80%) to LHB the (after stage while migration phase). final resonances its both in is escape Neptune would particles the of .I .Brasil O. I. P. ON/GPA. - SwRI/DSSSO. - Operations 3 Space and ies INPE/DMC. - 2 Controle e Mecˆanica Espacial 1 a active, is mechanism all this of once But, percent few hibernating mode. the a access only would planetesimals that scattered show We resonance. mode resonance ing a that, access After may well. planetesimals as some resonance Kozai be the then into and trapped Neptune mean with exterior (MMR) resonance scattered some motion into that captured requires are re- mechanism planetesimals trans-Neptunian main The the to in gion. disk orbits planetesimal inclinations primordial high the from pathway supposedly bodies System formed). eclip- Solar have all the (where to of plane existence respect itc the with note orbits we high-inclined them, many now Among are and up. models showing theoretical past features in physical predicted not and dynamical unpredicted Many ihNpuea,freape 2004 example, for as, Neptune with 01 crs25 6) ehv eemndthe determined space elements have orbital We the ( in regions, 661). probable most 215, Icarus 2011, : n : Ms(rsl oe ors 03- 2013 Soares, & A&A Gomes to (Brasil, submitted MMRs 1:3 and 2:5 ytmojcsbyn etn.Tedsoeyof discovery (TNO) The object trans-Neptunian Solar first Neptune. the small beyond of objects formation System dynamical the discuss We ieyt omthe most the form is to mechanism this likely that indicate results ous lt n Charon and Pluto ,e i e, a, 2:3 YAIA EHNS OPRODUCE TO MECHANISM DYNAMICAL A bevtoi ainl rp ePsus mAstromomia em Pesquisa de Grupo Observat´orio Nacional, otws eerhIsiue eatet fSaeStud- Space of Departments Institute, Research Southwest nttt ainld eqia saii,Dvsa de Divis˜ao Espaciais, Pesquisas de Nacional Instituto u eut ol xli tlataprin(up portion a least at explain could results Our h i fti oki oso dynamical a show to is work this of aim The a < a < ,weedtce bet ol omcoeto close form would objects detached where ), nwihtepaeia sbrl okdin locked barely is planesimal the which in IHICIAIN TNOS HIGH-INCLINATIONS 1,2 1:2 .S Gomes S. R. , , ). − > i eahdobjects detached srltvl eet(1992 recent relatively is 5 hot o and , ouain endby defined population, 2,3 n .Nesvorn´y D. and , > q XR ls oMMR to close 36 − 190 au xetfor except hibernat- Previ- . (Gomes, ∼ QB 100% 129 1 ). 2 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes le oftr pc isost ayee Ac- Ganymede. ap- to be missions to (processes FAPESP space convenient knowledgments: future are or- to orbits Another such plied ampli- small Thus, stable. with tudes. variating are behaved orbits elements polar bital km) 150 argument (100 low-altitude and the However, show circulating. results pericenter The of eccentric- devel- in inclination. are expansions and avoid motion ity arti- to form of the closed equations of in oped motion The orbital satellite. the equations ficial describe planetary to Lagrange used The pertur- are these used. for is model bations dynamic simplified A body. h oyei etrain ietoedet non- to ( due mass those of distribution like uniform perturbations the and polygenic of attraction) the influence gravitational satel- the (Jupiter’s artificial under satel- of third-body Ganymede artificial orbits around of considers lites study orbits The of stability with lites. the around, plan- conducted to the be in respect to useful missions be space is can of low- it emphasis ning and for orbits An search polar mission. in a Ganymede. given of perform around type to orbits this aims altitude of work success this the Thus, for dy- satellite planetary essential the this is around of orbits comprehension these into of This namics Orbiter) the Ganymede orbit. a insert Ganymedes (Jupiter is to that JGO ESA Mission and spacecraft NASA System between Jupiter cooperation Ganymede Europa visit the to planned like being are missions Some ˜ oPuo(NFS) ˜oJsedsCmo,Brazil. Campos, S˜ao Jos´e (UNIFESP), dos S˜ao Paulo Brazil. Guaratinguet´a, (UNESP), 2 University ([email protected]). State Paulo 1 130 ,21/23- n 2012/21023-6). and 2012/12539-9 5, .CroodsSantos dos Cardoso J. XPAESI H AIAL OEOF ZONE HABITABLE THE IN EXOPLANETS AYEECNIEIGADISTURBING A CONSIDERING GANYMEDE TBELWATTD RISAROUND ORBITS LOW-ALTITUDE STABLE nttt fSineadTcnlg,FdrlUiest of University Federal Technology, and Science of Institute ru nObtlDnmc n lntlg,S˜ao Planetology, and Dynamics Orbital on Group IA,TEMLADMAGNETIC AND THERMAL TIDAL, VLTO FTERRESTRIAL OF EVOLUTION OYI ICLRORBIT CIRCULAR A IN BODY W R STARS DWARF .d Moraes de V. 1 .P .Carvalho S. P. J. , J 2 2 and n J ◦ 3 ftemain the of ) 2011/05671- 2 n R. and , ABSTRACTS pdadnmclmdlo h oino asteroids of motion devel- the have of we model context, dynamical a this oped In off- determination. for set done observations and observations available period. re- certain offset a the over that constant assumes mains method the This and observations observations recent ephemeris. between off- difference most The mean the the from as ephemeris. calculated JPL is to set compared offset stant and stars of ephemeris. occulta- astrometry accurate stellar accurate both of even- requires prediction an tions The or multiplicity atmosphere. the tual shape/size, objects, the these deter- as of precisely such characteristics to physical way some only occulta- mine and the Stellar currently, faint are objects. tions system distant, solar known are poorly Objects Trans-Neptunian Medell´ın, Colombia. 3 Argentina. Aires, 2 Medell´ın, Colombia. 1 H OTX FSELROCCULTATIONS STELLAR OF CONTEXT THE antcfil rwt nupoetdplanet. unprotected an with planetary or protective and field evo- stable magnetic planetary an the with of finish stages to lution first model very evolution this thermal how a planets know with of this We evolution combine tidal star. and and host af- rotation the most of the the time activity calculate is same magnetic history the the planet by At the fected of Myr. period espe- first first planet, this very the the of during locking period cially tidal rotation the final by or the affected (resonance) determines rays. tidally this cosmic are host, and stars their wind dwarf stellar orbiting the Planets the of reservoir against its action protected keep water, erosive to inten- like planet material its a volatile and for of crucial dynamo is planetary This the evolu- sity. like of field properties regime magnetic determines the period planetary rotation the The in tion. plays role planet main a of a evolution thermal and rotation The .Desmars J. .Cuartas-Restrepo P. eatmnod inisBaia,Uiesddd Medell´ı B´asicas, de Ciencias Universidad de Departamento nttt eAtoo´ayFıiadlEpco-IF,Buenos IAFE, - Astronom´ıa F´ısica Espacio de y del Instituto MRVMN FTOSEHMRSIN EPHEMERIS TNO’S OF IMPROVEMENT nttt eFıia-FE,Uiesddd Antioquia, de Universidad FCEN, - F´ısica de Instituto nti td,w efr e peei with ephemeris new a perform we study, this In con- a use prediction of methods current The .I .Camargo B. I. J. 1 Hoyos .Braga-Ribas F. , 3 n .Sucerquia M. and , 1 .Melita M. , 1 n .Assafin M. and , 1 .Vieira-Martins R. , 2 .Zuluaga J. , 1 2 1 J. , 1 n, , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes nteipoeeto N’ ephemerides. TNO’S of improvement the occultations previous in of motion. contribution TNO’s the the analyze We on positions constraints astrometric new occul- therefore accurate Finally, and provide predictions. also make tations to ephemerides used new Consequently, be should future. dif- the predic- the in inaccurate offset’s tions making TNOs, the increases other sharply when For ference or observa- small. short remain between is variations time may occultation method and the offset secu- tions when the a accurate objects, and some remain term For one-year term. periodic time, ob- lar over a of varies date to then the according difference at this offset but the servations to close is ephemerides a determined and observations ephemeris. new to fitted (NIMA), 2 1 h hlais vn r icse.A eutwe result a As discussed. are explain event could Chelyabinsk that the changes orbital is the and Earth addressed planet dy- with This encounter interesting fragments. DA14, namically smaller to the companions, similar its fragment, the and asteroid study an to of model a dynamics a developed from we fragment impact, isolated remaining previous an biggest not the is but DA14 asteroid, 2012 dis- that long Assuming by and other tances. orbit each from same separated the being in possibly fragments, practically which smaller space, fragment, in other scattered by asteroids small. accompanied very an usually is considered is meters, be 45 can of It diameter 2012 a Asteroid with DA14 The 2012 DA14, discarded. Asteroid completely the be of mete- cannot companion the a of possibility being the orite However from north. DA14, to asteroid south to Moreover, similarly traveling, Earth. not to was close as- it passed the hours asteroid sixteen from the happened away before collision far the too rea- because was teroid, main meteorite two The for spe- asteroid hypothesis sons: Some this day. discarded same that cialists on passed Earth which smaller to DA14, a close 2012 be Asteroid could the it of companion think nat- people Russia, many Chelyabinsk, made in urally fell that meteorite The bevtoi oVlnoUR,Brazil. Valongo/UFRJ, Observat´orio do Brazil. Observat´orio Nacional/MCTI, h ieec ewe IAadJPL and NIMA between difference The ML SEODFAMNSIN FRAGMENTS ASTEROID SMALL AT-RSIGORBITS EARTH-CROSSING .Duha J. 1 n .B Afonso B. G. and 2 ABSTRACTS lnt rm0t 00a.Rlvn eut o the objects for presented. transneptunian results be Relevant and will asteroids au. of 1000 the population to all involving 0 and TBRs from located of planets TBRs are thousands the are where al- strong of showing how This System atlas Solar an the orbit. obtain in to arbitrary and us an orbits allowed in coplanar gorithm particle circular be- massless TBRs in a numer- arbitrary planets to of two algorithm strength tween an the propose estimate of We ically relevance dynamical strength TBRs. the width, us these the give obtain that to whatever nominal is or the challenge near The a very in them one. split all account resonances resonances into body of three family taken nominal are the When of motions each planets. secular per- perturbing slow the the of these of motion nodes secular and the ihelion ignore we the simple, very if is of specially planets of axis pairs arbitrary semimajor taking TBRs in localization approximate and rtclangle critical being atcewt nabtayobtadtoplanets two and orbit massless arbitrary a an between with (TBRs) particle resonances body Three et lo ls otelre rget,mr easily frag- more asteroid fragments, larger found. for the to look it close to also, Therefore, ments interesting meteorite very days. with be several would happens last can that pass- way which DA14 showers, same 2012 the Asteroid by, the be- ing after meteorite a or of during, collision a fore, be could there that, find 2 edu.br). 1 Uruguay. 1 TA FTETREBD RESONANCES BODY THREE THE OF ATLAS eea nttt fPrn FR Brazil(jania.duha@ifpr IFPR, - Parana of Institute Federal eea nttt fAaoa FM Brazil. IFAM, - Amazonas of Institute Federal IFRNITDATRI FAMILIES ASTEROID DIFFERENTIATED autdd inis nvria el Rep´ublica, la de Universidad Ciencias, de Facultad P 2 .S Martins-Filho S. W. k i ncrua olnrobt cu hnthe when occur orbits coplanar circular in YAIA VLTO OF EVOLUTION DYNAMICAL neesi siltn vrtm.The time. over oscillating is integers Mothe-Diniz NTESLRSYSTEM SOLAR THE IN σ = k 0 .Gallardo T. λ 0 + k 2 1 n .Roig F. and , λ 1 1 .Carvano J. , + k 1 2 λ 2 − ( k 1 0 + 1 T. , k 1 + k 2 ) 131 ̟ P 0 1 . XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 1 of distribution families. the asteroid with real compared integra- result the simpletic and the a tor, of using evolution implemented orbital nucleus is the the fragments Finally, of mantle. fragments the the distri- and for and isotropic velocities Stewart an of assuming by bution and described (2009) formalism Leinhardt the is energy by accomplished disruption was given catastrophic That the synthetic that a break-up. assuming of the step elements next after orbital The family the three calculate bodies. or to metal twice was for is than in bodies greater changes silicate times the for physi- that axis each showing semi-major for clearly individually variation parameter, axis the above cal semi-major study of the closely derivation to of The us allowed 2006 equations al., therein). et references Bottke (i.e., and formal- effect Yarkovsky original the the for albedo). on ism based bond was and development obliquity This heat, mo- specific pa- mean rameter, thermal conductivity, the rotation, as in of (such frequency directly tion, properties axis physical equa- semi-major of the the terms of expressed variation We of some tions as resonances. such motion motions space, mean near-Earth orbital it to into the routes asteroids bodies, in transport bringing System changes eventually Solar 1976), cause (Peterson, In radiation to solar known body. the is irregular of an re-radiation by caused thermal force the non-conservative by a The semi- is effect. Yarkovsky the effect the Yarkovsky in by den- caused inertia in drift thermal axis variations major and mantle. of by albedo, effects rocky formed bond the a sity, body study by a we surrounded of Initially, nucleus up metallic break a the is from what with expected consistent with properties members physical family different differenti- considering fully body, a evolution parent from formed ated dynamical asteroids the of family study a to of aims project The 132 meddi naclctdi h igo Saturn. of ring G the in located is arc across, an 1km in than embedded less Aegaeon, satellite small The 2 ([email protected]). Brazil Janeiro/RJ, Crist´ov˜ao, de Rio NE H FET FTERESONANCE THE OF EFFECTS THE UNDER IHMMSADTESLRRADIATION SOLAR THE AND MIMAS WITH bevtoi oValongo/UFRJ. Observat´orio do bevtoi ainl u eea o´ rsio7,S˜a 77, Jos´e Cristino General Rua Observat´orio Nacional, .C Mour˜ao C. D. H VLTO FTEGRN ARC RING G THE OF EVOLUTION THE 1 .M ilat Winter Giuliatti M. S. , FORCE Sfair 1 1 n R. and , ABSTRACTS o osattesse 0 er eoeteencounter the before years 100 system integration encounter the backward close a start all performed to of at we elements Then integration orbital of the events. the each in save For we objects follows: runs, all as basic done satel- 101 regular is the its This with but included. was orbit lites giant same gas the a on encountered in started that giant integrations ice numerical the which Subsequently additional cases. performed of Jupiter we planets, jumping all were kept 24 which which runs the successful ob- 101 used we We tained and 1999) 2009). (Chambers al. integrator MERCURY et jumping (Brasser a scenario in to simulations Jupiter model according Nice Saturn, of evolution and the ice Jupiter an between placed in we the conditions planet initial with the For encounters giants. experienced gas when planets systems two satellite the these of in- to evolution simulations the numerical of vestigate used phase we instability model, the satel- Nice during regular the planets the ice of the behavior of the lites explain to order In iepno 0ys h eann atce stay ring. particles G in remaining the The arc in the confined 100yrs. from of particles timespan smallest a with of collision most by of remove Aegaeon effects pressure the radiation Mimas, initially solar with the are resonance particles corotation the a Our in despite surface. that, Aegaeon’s show the to results close ring, and Aegaeon, the of These along both pressure. spread about radiation initially effects solar were gravitational the particles the rang- and under (sizes Mimas 100m) particles of to tiny 1 of from orbital sample ing the a study against we of work, ring evolution this re- G In is the arc, forces. of this dissipative maintenance in along the located Aegaoen, for particles large sponsible that of proposed set a been with also has satellite is It the Aegaeon with Mimas. resonance corotation by 7:6 arcs. a formed in in locked is immersed which satellites im- spacecraft, structures small Cassini of the class by new a aged to belong satellite This vAiet eer aCna 3 E 12516-410, CEP , 333 Cunha, da ([email protected]). Pereira Brazil. Guaratinguet´a, SP, Ariberto Av 1 .C Nogueira C. E. H EAIRO EUA SATELLITES REGULAR OF BEHAVIOR THE nv saulPuit NS,Cmu Guaratinguet´a, Campus UNESP, - Paulista Estadual Univ. UIGTENC OE’ PLANETARY MODEL’S NICE THE DURING ± 0k rmtesmmjrai resonance axis semimajor the from km 20 LS ENCOUNTERS CLOSE 1,2 .S Gomes S. R. , 2 n .Brasser R. and , 3 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes iclrzdb ie uigte50mlinyears was million orbit 500 its LHB. and the the 2011) during before tides al. by et circularized Nogueira Hamil- cap- and 2006, was (Agnor ton Triton disruption to that binary LHB assume through the semi-major tured also from actual We decay tidal the time. the present than for larger account to or- 15% axis an a with Triton with introduced or- bit gas we present Neptune a their Ariel, For with with bits. Miranda, Oberon encounters satellites and Titania had the Umbriel, considered that we planet giant, ice Uranus that the assume we the is the If for to or- integration encounter. the respect planetary final restart next with to The used satellites were planet the giant. ice of ice elements the bital around reg- the satellites with ular integration forward the re-enacted and 3 2 1 wr tr,snetehge rqec fteperi- tempera- considerably. the surface variation the of ture dampens frequency forcing higher radiative odic the M since around planets stars, HZs for ther- dwarf of particularly atmospheric range orbits, the The shorter expand for also stars. could capacitance dwarf mal plan- Habit- K be around their would targets ets encompasses optimum the dwarfs (HZ), Zone M able tidal- of the radius since works but technique lock periods, The orbital shorter planets. habit- for of the better class of this understanding of better ability a with us would capabilities, enable infrared thermal ob- stars, with ground-based and servatories their space from planned by planets allowed both resolved of de- atmospheric analysis spectro- the of the scopic with for limit together technique, lower method This robust thickness. simple a a of with in termination researchers future provide near may stars, the parent their forc- of radiative the ing to atmospheric subjected their capacitance, that thermal suggested is com- subgroup it the more rotators, For a fast of Universe. be the may in Earth, phenomenon the mon than drier or- and eccentric following bits, planets rocky However, and content orbit. volatile mass, focused of has conditions Earth-like planets on habitable for search current The H OTCMO AIAL PLANETS HABITABLE COMMON MOST THE cdmaSnc,Taiwan. Sinica, Academia Brasil. Observat´orio Nacional, Brasil. Fluminense, Federal Universidade TOPEI HRCEIAINOF CHARACTERIZATION ATMOSPHERIC H UGOPO ATROTATORS FAST OF SUBGROUP THE .Pinotti R. 1 ABSTRACTS ih,Aeia2 ,11 E 30-0,RoCao S˜ao Claro, Rio 13506-900, CEP 1515 Brazil. A, Paulo, 24 Avenida Filho, Rio 13506-900, CEP 1515, 2 (fi[email protected]). A, Brazil S˜ao 24 Paulo, Claro, Avenida Filho, Mesquita de aer,LdiaPdoAtno4,Rod aer,Brasil, Janeiro, de Rio 43, ([email protected]). Antonio 20080-090 Pedro Ladeira Janeiro, 1 1 dsubdb elr1 ) O-5b(disturbed and KOI-961b b KOI-961d). by KOI-55 (disturbed KOI-961c c), c), KOI-55 Kepler-11 by Kepler-11 by of (disturbed cases phe- the b This in observed space. been has phase nomenon such rotational in of insta- expected to regions not lead are regular which can rotation planet its the on of bilities figure the cen- the on of star torque tral the by induced librations domain, stable synchronous the on the Depending inside conditions initial rotation. the synchronous res- the motion super-Earths. mean on the the onance of free of role the one the investigate we of of Thus, rotation period the the particular of a to libration to close associated have is we commensurability period cases the some that In observed of commensurable. pairs several are of planets motions of mean and the cases where KOI-55 the KOI-961, Kepler-11, in systems given multi-planetary is the Emphasis spin- and resonances. rotation orbit body mean-motion rigid this of on effects In commensurabilities dynamical checked. the be study we are must work planets problem in giant that present and or present, are terrestrial prob- other Super-Earths two-body where the many the systems of However, around rules motion the lem. by whose governed planet is star con- single is a and it papers, Callegari sidered referred (2012), the In Rodr´ıguez (2013)). al. et (Rodr´ıguez tidal spin evolution and resonance these spin-orbit in of including rotation done planets, of dynamics been the 10 have understand Super- to than efforts them order call several orbits less Recently, (2006) magnitude close-in al. Earths. of in et Valencia order planets mass. on of Earth mass deal low great and a is There PNOBTRSNNE NSUPER-EARTH IN RESONANCES SPIN-ORBIT EA,Uiesdd saulPuit ´lod Mesquita J´ulio de Paulista Estadual Universidade DEMAC, hsc eatet nvriaeEtda alsaJ´uli Paulista Estadual Universidade Department, Physics bevtrod aog,Uiesdd eea oRode Rio do Federal Universidade Valongo, do Observatorio YTM LS OMEAN-MOTION TO CLOSE SYSTEMS .B Ribeiro B. F. COMMENSURABILITIES 1 n .CleaiJr. Callegari N. and 2 133 o XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes (ICATE). 1 134 lsoscnb osdrdrlal ape fthe of in- trapped. samples these originally reliable was whether that considered arises fluid/melt be then crystalliza- can question closed-system clusions The of result tion. the are these al. that objects et assumption (Varela the constrain inclusions that these 2007-2013) compositional of many extreme in will of variations I identification glass-bearing phases. the of mineral discuss study different the by which is hosted to inclusions exposed, processes was secondary recon- rock the to the or used phases formation the early is during of that prevailing condition tool, the useful struct A primary the ma- obscure information. produce and can compositions that in 2013) changes jor al., et processes, Goresy (El secondary metamor- phism pressure-induce of or presence re-equilibration impor- as the such is check it these Thus, to on 2005-2009). tant percolation al., et fluid by (Bouvier chronometers or rocks these impacts of strong resetting a could either of shergottites ( result in the old age be very young the or However, 330-475Ma), 4Ga). and rocks (180Ma these young that indicate are evidences debates. ongoing of of lines matter the Different a old, is shergottites -1.3Ga the events consensus being of age broad chassignites impact a and several is nakhlites in there for or Although impact 2006). giant (Meyer ei- a surface Martian Pos- in the ther 1994). from McSween, ejected were (e.g. they sibly, believed Mars are from the meteorites originate SNC to to the similar lan- 1976), Viking very Owen, the ders, by be analyzed to (as atmosphere (e.g., out Martian melts turned shock 1985) from glasses Pepin, of in patterns trapped abundance gases the rare and (Clayton Because body these 1983). planetary that Mayeda, single Oxy- a indicate from meteorites are basalt. SNC rocks extraterrestrial in an isotopes as gen rock iden- (1872) this Tschermak, tified when ago be- years abun- Shergotty several of most gan study the petrographic The are rec- shergottites group. dant meteorites date, to SNC up all ognized Of are meteorites. achondritic group, (Shergotty-Nakhla-Chassigny) SNC The TUTRSO OE PHLE 90II 1910 1P/HALLEY COMET OF STRUCTURES OPOOIA NLSSO H TAIL THE OF ANALYSIS MORPHOLOGICAL nttt eCeca srnoiad aTer e Espaci del y Tierra Astron´omica la Ciencias de de Instituto .R Voelzke R. M. H N METEORITES SNC THE .E Varela E. M. 1 n .S Izaguirre S. L. and 1 1 ABSTRACTS > o aerudmrhlge.Terao h h PNe the why 20% reason and The bipolars and morphologies. About ellipticals round star. are have physical PNe central the the and us- of determine nebula 70% By to both: able of gas. are properties we nebular tool, the this with ing radiation cen- the star’s of interactions tral the Photoionization of reproduce to evolution intent stars. codes the intermediate-mass understand and extremely to low- is order (PNe) in nebulae important planetary of study The aysrcue ie bv)i qa o(1.4 70 to same equal 10 the is x above) in cited (measured structures wave wavy the of A amplitude aysrcue seult (168 to different equal 20 is in structures measured wavy Vpc velocity phase centric un tet88 10-0,Sa al,S,Brazil. SP, Paulo, S˜ao 01506-000, 868, ([email protected]). Street Bueno 1 iha vrg ftecretdvlcte cequal Vc velocities corrected onsets (57 the to Both of passage average perihelion an the DEs. after with of determined were onsets allowed The DEs two images of different of true. 26 derivation not in the is documented reverse DEs the the 26 with but association in structures, occur possible wavy solitons also the the is but that It say knot, independently. to a occur of may one occurrence last the and/or DE with a Swan-Tail it of general, a occurrence In the associate shells. to six possible is and knots disconnection 166 26 (DEs), tails, events Swan-like secondary 13 the solitons, along 41 164 tails, A and struc- tail II. wavy main the 1910 304 along Halley tures revealed Comet analysis of visual im- Atlas These systematic the 1P/Halley. from of are tail ages plasma struc- the morphological along of tures the purpose the measuring for and analysed Septem- are identifying from 1911 May images to 1909 six ber eighty and hundred Eight oices ihicesn oeoeti distance. to cometocentric equal increasing with is increase images to different the 36 of (128 Vkc in velocities measured corrected knots the of value average aeeghl esrdi 0dffrn aystruc- (1.7 wavy to different equal 70 is tures in measured lc wavelength rziod u nvriy apsLbrae Galv˜ao Liberdade, Campus University, Sul do Cruzeiro EST TAIIAINEFCSON EFFECTS STRATIFICATION DENSITY 5 H DMDLN FTEBIPOLAR THE OF MODELING 3D THE ± m h envleo h orce cometo- corrected the of value mean The km. .M Carneiro M. C. ± 2 ms hr satnec o n lc and A for tendency a is There km/s. 12) 5 ms h envleo h corrected the of value mean The km/s. 15) NESELRMEDIUM INTERSTELLAR EUANC2346 NGC NEBULA ± 1 n .R Gon¸calves R. D. and .)x10 x 0.1) 6 ± madtemean the and km 8 ms The km/s. 28) 1 ± 0.1) XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes n oe.W osdrdtedniycntn nthe in constant torus (n density torus the components: considered we two We has distribution lobes. and 2346 density NGC The 2003, for assumed al. 1136). et 340, modeling B. the MNRAS, (Ercolano, for 3D MOCASSIN used a was for code process candidate The excellent an modeling. star, be detailed central to as be- seems system also PN binary and this a 6302; 370) has (NGC 2346 418, NGC PN MNRAS, cause bipolar 2011, a al. is of et there Wright modeling that 3D Considering one responsi- shapes. only bipolar partially the be that for could is ble stars suggestion central accepted binary well well the not A is yet. types understood morphological different so present i n (i) oiainsae bevdi hsnbl.S a,the far, So higher nebula. n the this in reproduce observed to stages strati- order ionization density in that essential observed is have fication we models our In ewe h bevdadmdldspectrum. modeled and observed the between eJnio aer er nˆno 3 08-9,Rode Rio 20080-090, 43, Antˆonio, ([email protected]). Pedro Brazil Janeiro, Ladeira Janeiro, de 1 ntefraino e eeaino stars. of role generation its new as a well of formation as the the 126.1–0.8–14 G discuss in we of data, origin available the the onto possible all out on spread Based cat- found shell. are source candidates cYSOs point Several object molecular infrared alogs. using stellar this made young of was for part (cYSOs) search densest A the Sh2-187 shell. region onto HII located young is The spectral accurate distances. their and get pro- types to in shell, located cat- with the stars inside of observed OB jection four we lack of area, the spectra the the given GEMINI in and stars shell, O-type the pos- alogued the of disentangle To origin origin. sible thermal 126.1– G a with has an- associated 0.8–14 we emission data the infrared whether the an- alyze and continuum we properties. to radio physical data related the main CO From gas its and estimate molecular HI and and structure on atomic Based the kpc. 126.1–0.8–14 alyze G 1 of about distance The is region observed. 126.1– a G is named of shell, 0.8–14, molecular study defined well multi-wavelength a where a present We .Cichowolski S. L bevtoi oVlno-Uiesdd eea oRio do Federal Universidade - Valongo Observat´orio do ∝ L 2.–.–4 OEUA SHELL MOLECULAR A 126.1–0.8–14: G Ortega r osat i)n (ii) constant; = − T 1 n he ieetcssi h oe (n lobes the in cases different three and ) itiuinhsgvntebs agreement best the given has distribution 1 .M Arnal M. E. , EAE OSH2-187 TO RELATED 1 .Pineault S. , L ∝ 4,5 r 2 n .A Suad A. L. and , − .Gamen R. , 1 n ii n (iii) and ; 3,4 L .E. M. , ∝ 5 ABSTRACTS r − L 2 ): . 4 3 Canada. Universit´e Laval, 2 1 G 32FR IHDSESO SPECTRA DISPERSION HIGH FORM 6302 NGC China. 2 Brasil. 1 ieai rfie rmfridnlnsfrdifferent for lines forbidden the from derived profiles we kinematic Dias Brazil, dos in Pico dispersion, (MCT/LNA) at Observatory tele- high Coud´e spectrograph 1.60m the Using the and with scope obtained km/s. spectroscopy slit 40 long and velocities 20 expansion between typical have nebulae Planetary 5 . n 8.0 between and out carried 3.6 survey a GLIMPSE, by detected l.W netgtdJ10tastoso molecules of bub- transitions this of J=1-0 center 12 investigated the emis- We at region infrared ble. HII in- and an is molecular There the in sion. surrounding N10 environment bubble frared the studied We 24 tr.Bsds h otiuina 8 at contribution the nearby Besides, by heated stars. grains O small of contribution a with itiuin tcnla st nesadtetrig- region. the this in understand scenario to formation us their star lead and gered clumps can the dis- It of to distribution. stage intended evolutionary also the We cuss through features parameters. clumps, physical observed derive presents the m can N10 13.7 we bubble PMO which The from the at object telescope. observations This radio of target formation. the star was massive 4.5 of at excess stages the early that In proposed is bubbles. it of N10, PDRs of case the the from radiation hydrocarbons) by aromatic excited (polycyclic PAHs by nated RCbn niaea uflw intr of signature a outflow, an indicate band IRAC m autdd inisAto´mcsyGeof´ısicas, Astron´omicas Argenti y Ciencias de Facultad nttt eAto´sc eL lt,Argentina. Plata, La Astrof´ısica de de Instituto Argentina. Espacio, F´ısica del Astronom´ıa y de Instituto nttt retn eRadioastronom´ıa, Argentina. de Argentino Instituto ´ preetd hsqe egei hsqee d’optique, et g´enie physique de physique, D´epartement de CO, IEAI RFLSO G 98AND 3918 NGC OF PROFILES KINEMATIC eatmnod srnmad A/S,S˜ao Paulo, IAG/USP, do Astronomia de Departamento eateto srnm,Pkn nvriy Beijing, University, Peking Astronomy, of Department .Gama D. ,crepnigt h msino o dust, hot of emission the to corresponding m, 13 .J .Lago A. J. P. OadC and CO 1 .Lepine J. , .W loaaye h msinat emission the analyzed also We m. H UBEN10 BUBBLE THE 18 oad 1.Ti betwas object This N10. towards O 1 n .D .Costa D. D. R. and 1 .Wu Y. , 2 n .Yuan J. and , sdomi- is m 1 2 135 na. XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ag ubro otenpaeaynebulae. planetary for southern technique of this number apply large the and a use code, nebulae SHAPE to planetary the these intend with model we to Hereafter profiles for years kinematic shell. 3111 was external expansion result the assuming the velocity; age, uniform used kinematic with were its profiles litera- estimate velocity the the to from NGC3918, For results other ture. with agreement good eMxc.([email protected]). Mexico. de 1 1 pa- For them, 805 of age. of distance kinematic a some estimate and for we distance NGC6302 and, as pro- such nebulae, velocity rameters derive the to for us allowed files south- Results of sample PNe. a for ern slit the along positions angular 136 iiyo h rdadteptnilsd applications visi- side the potential increase the it. to and of 3MdB, grid in the grid of stored a bility and for run ask the can be of Anybody to some description 3MdB. and use a managed that is here projects database present the We way the data. of extraction to desired the references facilitate the different to of aimed and with is project models database each of identify The grids 2013). host to al, et photoionization (Ferland Cloudy code used widely the by and using known accessed obtained well are is models It The tools. requests. attempt IDL MySQL previous and a Cloudy3D of on version based modern models. large more a a photoionization is construct This of to effort database original multipurpose an is 3MdB The nvriaed ˜oPuo u oMta,12 Cidade - 05508-090. 1226 Mat˜ao, CEP do - Rua Brasil Universit´aria - S˜ao S˜ao Paulo, Paulo-SP de Universidade .A Oddone A. M. nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto nttt eAtooi,UiesddNcoa Autonoma Nacional Universidad Astronomia, de Instituto MB H EIA ILO MODELS MILLION MEXICAN THE 3MDB: OT-ATRGO FTELARGE THE OF REGION SOUTH-EAST TUTR FBBLSI THE IN BUBBLES OF STRUCTURE .Morisset C. AELNCCLOUD MAGELLANIC 1 .Ambrocio-Cruz P. , n .V Goldes V. G. and 1 DATABASE n .Delgado-Inglada G. and 4 2 .LeCoarer E. , ± 4p,in 143pc, 1 ABSTRACTS icas, 3 , h iuegnrlbcgon owihte belong. they over which to objects background isolated general en- relatively diffuse studied an are the the they as if if identity discern or some semble, to kinematically try Supershell we have way the objects this compose In that of 9. (stellar LMC mechanism) bubbles origin other different the or the is explosion which supernova distinguish wind, to would us that allow age), density, ambient luminosity, measure, (superfi- mass, emission density, structures electronic brightness, char- these cial the of determine we parameters balance acteristics energy of means By ooiu E 0,DML most DEM the 202, being regions L DEM HII 208, several notorious L DEM and 165, 221, four L L DEM of DEM and composed 164 L is DEM scanning 9 shells LMC giant counting a Supershell photon The reducer, a camera. focal and a interferometer tele- Fabry-Perot with diameter 36cm equipped a with scope, ESO at out carried Way, Argentina. 4 Francia. Grenoble, inlnswr esrdo h pcr,allowing spectra, the on was measured coverage were lines spectral sion The m 4.1 3500-8000 the about Chile. with Research in decli- obtained Astrophysical Telescope), spaced (Southern were equally telescope data and different SOAR position- The different of by on grid nations. nebula slit a whole the from ing the spectroscopy data covering slit collect positions Long to of used mapping was properties. spectroscopic the physical on their based rem- N49 Cloud, supernova N11L, Magellanic two and Large of the to study belonging a nants presents work This bevtoshv encridoti h rm fa of frame the in H out carried The been of 9. have LMC observations results Supershell the the of kinematical Cloud, region Magellanic South-East the Large the in report located we structure the work this In u´ nm e saod iag,M´exico. Hidalgo, 3 de Estado Aut´onoma del 2 (mao @oac.uncor.edu). C´ordoba, Argentina X500BGR, 854, C´ordoba, Laprida 1 α bevtroAto´mc el nvria ainlde Nacional Universidad la Astron´omico de Observatorio autdd ae´tc,Atoo´ayFıia C´ordoba, F´ısica, Astronom´ıa y Matem´atica, de Facultad aoaor ’srpyiu,UiesteJsp Fourier Joseph Universit’e d’Astrophysique, Laboratoire nttt eCeca ´scseIgne´a Universidad Ingenier´ıa, e B´asicas Ciencias de Instituto UENV ENNSI H LARGE THE IN REMNANTS SUPERNOVA uvyo h aelncCod n h Milky the and Clouds Magellanic the of survey PCRSOI TDE FTWO OF STUDIES SPECTROSCOPIC .Pauletti D. AELNCCLOUD MAGELLANIC .Frec bet bu 0emis- 50 about object, each For A. ˚ 1 n .V .Copetti F. V. M. and 0 n E 207. L DEM and 206 ˙ 1 , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes OII ( III] [O on ttecnr.I 1Lteeeto density electron cm the 100 N11L than In less values from centre. higher varies the the at with symmetry found shows spherical distribution rough temperature a electron The gradi- cm East. 600 density from strong varying density a the presents with ent N49 spectively. is h aso lcrndniyadtempera- and II] density [S the electron using of obtained ra- were maps intensity ture line The interesting many tios. of maps build to ot-ett oeta 00cm 3000 than more to North-West ueo hs w uenv remnants. struc- supernova the two of these picture of a build ture to filaments. used bright were the maps on These found values higher the with eMeio praoPsa 024 ´xc,DF 04510, D.F. M´exico, 70–264, Postal M´exico, ([email protected]). Apartado M´exico, de 1 ([paulettid;mvfc]@gmail.com). Brazil RS, P´os-Gradu¸c˜ao Sa Maria, 97119-900 de Maria, Santa em Programa de Federal F´ısica, e Matem´atica, Universidade de tamento 1 ersosbefrtelreaudnediscrepancy abundance large and the factor shocks, for in responsible might energy be regions, shadowed turbulent and of reconnection, magnetic dissipation as photoionization, that direct such suggest to addition and in RLs processes from other abun- derived proper those derived the are those that dances imply than results These larger times RLs. from two about excited are collisionally lines lines. from or derived forbidden similar pressures from are Electron derived II densities O than of RLs smaller while from lines, derived forbidden densities from the are continua derived Balmer those II, with than together O lower I H of of temperatures (RLs) RLs (2) lines The and recombination regions. (1) II from derived H extragalactic one Galactic is sample: eight temperature our and of low objects and oxygen- all density in for absent high signature the of that clumps find of rich We sample II, a regions. of O II temperature of H and computations density atomic the NLTE study the we V1 and multiplet II O of of observations high-quality on Based ESTE,TMEAUE,PRESSURES, TEMPERATURES, DENSITIES, nttt eAtoo´a nvria ainlAut´onoma Nacional Astronom´ıa, Universidad de Instituto EOBNTO IE NHI REGIONS II H IN LINES RECOMBINATION aoa´rod naieNmeiaeAto´sc,Depar- Astrof´ısica, e Num´erica An´alise de Laborat´orio N BNACSDRVDFO II O FROM DERIVED ABUNDANCES AND λ 5007+ .Peimbert M. N HI IMPLICATIONS THEIR AND t 2 ausosre nHI regions. II H in observed values λ 4959)/ 1 λ 33ln ai esr,re- sensors, ratio line 4363 n .Peimbert A. and − 3 oaot40cm 400 about to λ − 6717 3 tteSouth- the at /λ 1 − 71and 6731 3 tthe at ABSTRACTS − nta 3 , eaiet H to relative ie ie,adrltv bnacso He of abundances relative and lines, cited toso h ln ftesywr band Abun- obtained. were sky N the of fluctu- of dances temperature plane Small the on sensors. ations the III] [O from and temperatures II] electron [N and and constructed. II] sensors, [S IV] the were [Ar from profiles calculated were spatial densities From Electron and direction. East-West declina- maps the different on them, the slit several the to in with tions attached telescope SOAR obtained spectrograph m were 4.1 Goodman data the spectrophotometric with spectroscopy. slit resolved and spatially Long 6302 through NGC 2440 nebulae chemical NGC planetary and the physical of the conditions of analysis an present We rmrcmiainlines. recombination from 1 et nteHbn (1.65 band H the in ments clouds. interstellar of to evolution key is the forces, understanding gravitational knowl- and with turbulence together on MF, edge the of description A cloud. tla eim-teMsaDr lu MC,a (MDC), (0.25 inter- Cloud large the Dark (MF) pc), Musca (200-250 of field the nearby magnetic structure - the pre-collapse medium of stellar a study of the structure is goal Our Ribeiro L. N. ui 91 24-0,Sa o´ o aps P Brazil SP, Campos, dos Jos´e S˜ao 12244-000, ([email protected]). 2911, RS, fumi, Maria, Santa 97119-900, 2 Maria, ([alinerauber;mvfc]@gmail.com). Santa Brazil Matem´atica, Universi- de de Federal Departamento dade F´ısica, e de mento bet rb ein esrta htwspossible was what optical. than the denser in were regions we probe 2004), to optical able Magalhaes earlier & our (Pereyra with obser- observations these OPD the combining at By located vatory. telescopes cm 160 and cm aoa´rod naieNmeiaeAto´sc,Depart Astrof´ısica, An´alise Num´erica e de Laborat´orio PTA AITOSO HSCLAND PHYSICAL OF VARIATIONS SPATIAL nvriaed aed aaıa v hsiaHi- Shishima Av. Para´ıba, do Vale do Universidade H ANTCFEDSRCUEOF STRUCTURE FIELD MAGNETIC THE .B Rauber B. A. ehv bandlna oaiainmeasure- polarization linear obtained have We LNTR EUA G 32AND 6302 NGC NEBULAE PLANETARY HMCLPOETE FTHE OF PROPERTIES CHEMICAL + + O , 1 UC AKCLOUD DARK MUSCA .M Magalh˜aes M. A. , eedtrie rmcliinlyex- collisionally from determined were + 1 S , .V .Copetti F. V. M. , .Cambresy L. + G 2440 NGC Krabbe S , 2 ,O +, )wt h rzla’ 60 Brazilian’s the with m) 2 2+ 3 ◦ 1 Ne , .Pereyra A. , 3 x 1 2+ n .C. A. and , ◦ filamentary ) Ar , + n He and 3+ Ar , 2 and , 137 4+ 2+ a- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes h n ad lo st ocueta the Av that to up conclude through- least light at to the cloud us polarizing the out are allow grains between bands of comparison type H same The and MDC. V the the H- in the Our tendency of same parts cloud. the general inner aligned the in well of show axis is data small which band MF projected a the by with surrounded is cloud 3 2 condensations. optical cloud, 1 the the the of for in size MF pc the the 0.21-0.29 to of obtain comparable lengths we correlation band, polariza- of H range the of the subcritical function at a structure tion is the From Musca that cloud. concluded gravitational the and and across magnetic energies the mG) esti- compared We (0.02-0.16 we intensity cloud. vectors, Utilizing MF polarization ISM. the general the mated the of in dispersion those the as same the are 138 aa h 2 deg 520 The Way 2MASS Milky and data. the GLIMPSE with in complemented Variables (VVV), VISTA ESO survey the of public observations (NIR) combina- Near-Infrared the of on map tion based disk extinction Galactic an Southern of the development for the on report We nrrdbns( bands infrared siaino xicinb rvoswr ae on based alone. data work NIR previous under- 2MASS by systematic recently. extinction a of developed show estimation maps results other our Furthermore, with consistent is netnto a ihapxlsz f1’ of size pixel obtain a to with us map allowed extinction have an (RJCE), Color method Rayleigh-Jeans the Excess using results, wave- Our mid-infrared to lengths. pho- near the multiband from have thus ranging to and tometry surveyed surveys, sources VVV overlaps GLIMPSE the 152 and allows disk, 2MASS the Galactic the Southern work, with the this Way. of by Milky tiles/fields surveyed the region of history The im- formation are the and about which questions structure information fundamental address of to wealth portant a are epochs, UVY ALIHJASEXTINCTION RAYLEIGH-JEANS A SURVEY: AATCDS SSE RMTEVVV THE FROM SEEN AS DISK GALACTIC bevtied tabug-France. - Strasbourg de Observatoire Brazil. - INPE Brazil. - IAG/USP u tde nteotclbn hwdta the that showed band optical the in studies Our H XICINO H SOUTHERN THE ON EXTINCTION THE .Soto M. 1,2 .Barb´a R. , J Roman-Lopes , 2 H bevdb V n5near 5 in VVV by observed , MAP K 2 .Firpo V. , s , Y ∼ , 2 -,adta these that and 8-9, Z ,admultiple and ), 2,3 n A. and , × ’ which 1’, ABSTRACTS hc hyaie pr rm[ II] [N from Apart from component arise. plasma they the for which only of Thus, correct type are either 7009. line from NGC derived within abundances emis- chemical ions forbidden the parent the the to from rise differentsion giving a that from from volume the arises to that component emission plasma recombination additional an indicating of is emission, kinematics forbidden there the III] that [Ne with and and II, coincide III] O not [O II, the does N lines II, II C the Ne of consistent kinematics hydrogen The are of distribution IV] emission. the [Ar den- and and imaging electron direct II] The with [O agree velocity. from III] and derived [Ne sities position and given III], a [O at II], [N from temperatures ens10 ot,L eea Chile. Serena, La 3 Norte, 1200 ternas ([email protected]). USA 2 21218, MD Baltimore, 1 ieteiec o eobnto otiuinto contribution recombination II] [N found a We for similar. evidence very direct unexpectedly lines of are all recombination lines from derived these II kinematics the incom- all and Ne from evidence are derived other and structure they ionization the II, with discrepant: patible O are the II, kinematics in whose N emitting II, component plasma C excited a collisionally find and lines.We transfer, charge flu- orescence, recombination, for con- maps them.We well-known position–velocity struct from the derived elucidating discrepancy in abundance useful be differ- with or could similarities collisions ences whether and determine to recombination electrons comparing by in VLT excited interested spec- are the lines we slit at particular In long spectrograph ESO. UVES of from the 7009 from the troscopy NGC of emission nebula of kinematics planetary the analyzed have We ibefrtemdu rmwihte arise. they re- which from be medium should the them for from liable derived nebulae, abundances ionized the to so in used abundances usually lines chemical forbidden determine the with anomaly no .Torres-Peimbert S. eatmnod ´sc,Uiesddd aSrn,A.Cis- Av. Serena, La F´ısica, de de Universidad Departamento APCNCT aPaa Argentina. Plata, La IALP-CONICET, pc eecp cec nttt,30 a atnDrive, Martin San 3700 Institute, Science Telescope Space UCINO OIAINSTRUCTURE IONIZATION OF FUNCTION EOBNTO N COLLISIONALLY AND RECOMBINATION H ICEATKNMTC OF KINEMATICS DISCREPANT THE λ XIE IE NNC70 SA AS 7009 NGC IN LINES EXCITED 75 netknit con,teelectron the account, into taken Once 5755. n .Arrieta A. and 1 .G Richer G. M. , 3 2 .Georgiev L. , λ 75 efind we 5755, 1 , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes oa eSnaF,Meio 11,D .,M´exico, , F. D. 01219, M´exico, 880, Fe, Reforma Santa la ([email protected]). de de Lomas Paseo Prolongaci´on 22800, Iberoamericana, C., B. Ensenada, 3 877, M´exico Postal ([email protected]). Apartado M´exico, de 04510, D.F. M´exico, 2 70–264, Postal M´exico, ([email protected]). Apartado M´exico, de 1 V n ettegs rudteesas large a stars, these Around (10 gas. hot 13.6 the and than heat greater hy- and energies atomic eV) the radiation, able ionize (EUV to radiation, drogen eV), UV 6-13 of radiation, between (FUV deal energies molecule great O hydrogen the Massive a dissociate emit to jets. stars asso- and B frequently disks time or are protostellar long and with a re- phase, ciated spend protostellar HII which the and stars, in winds low-mass stars, to ionizing massive gions, strong from for masses, different nebula, responsible Orion of the stars like have regions, formation star Some ayt dutcrflysm aaeeso h jet the of neces- parameters is some but carefully proplyd, adjust the perturbation to of a sary front causes ionization jet the the in that conditions. show Beehive results the Our for adapted al., properly et 2000), (Raga Yguaz´u-A code the using an over mak- grid, hypothesis adaptive simulations this numerical test hydrodynamic we 3D work, ing this front In ionization per- the jet. are of the rings by crossing the the that to due suggested turbations (2005) axis. jet’s al. its HH540 et to the Bally to due coaxial attention rings of attracted system exotic has proplyd of Nebula, giant source a Orion Beehive, the in The and radiation. star ionizing low-mass the the dis- between jet. the protostellar tance on a depends characteristics and morphological shock Its bow some- external and, an region times, ion- photodissociation an a a disk, distinguish front, accretion can ization an exhibit with we Proplyds star which low-mass from central with (1993). shape described al. cometary proplyd, et a O’Dell a in object, accuracy stellar type a young produce regions of HII inside stars T-Tauri gion. nttt eAtoo´a nvria ainlAut´onoma Nacional Astronom´ıa, Universidad de Instituto Aut´onoma Nacional Astronom´ıa, Universidad de Instituto eatmnod ´sc ae´tcs Universidad Matem´aticas, y F´ısica de Departamento .A Feitosa A. J. DSMLTOSO H BEEHIVE THE OF SIMULATIONS 3D 4 K TRFORMATION STAR eini omd nw sHIre- HII as known formed, is region ) 1 .J Vasconcelos J. M. , PROPLYD Cerqueira 1 1 n .H. A. and , ABSTRACTS ieisvlct n jcinfeunyi re to order observations. in the frequency matching results ejection the and have velocity its like on rjc seSno-iv ta. eiae to dedicated properties. X-ray al.) the et of on- Santos-Silva studying another (see as well project as obser- going rep- performed, GMOS more been additional have a vations spectra, Aiming of set detected. resentative have we sources ray 1 1 4 fte r lsie sCT n 6 are to 76% ( correspond and fraction results CTTs small present as a the classified However are WTTs. them 51 stars: young of Among are 24% 38 (WTTs). TTs candidates, Classical counterparts TTs separate optical weak-line to used from was (CTTs) flux total the of 2 @iag.usp.br). pcrsoyo u -a ore eryZCawas optical CMa pre- with Z Multi-object nearby performed the sources star X-ray active. than our where of very Myr spectroscopy CMa, still few Z is a cluster around formation least stellar cluster, at a known by CMa, viously older GU is X- to that our near data, on discovered, near-IR and we Based optical by complemented Sh2-296. data ray nebula ionized the in studied shaped have activity we ( formation (CMaR1), young R1 star Major the Canis the unravel to Aiming pcr hwteL ie n fteidctr of indicators the of one of line, width equivalent I The their Li youth. since is the (TTs), that show stars sample Tauri spectra the T as of classified nature in- mainly were the stars confirm young to and of spected continuum features the Typical fitting bands. TiO and stan- library with spectra comparison type dard on Spectral based sources. was X-ray determination 45 counter- of optical candidates for the results parts In the and show Sh2-296. older we of work edge both present the from around population clusters mixed younger a of istence md m1,Ihes rsl(afioagalcm mjvasc [email protected]). ([email protected]; Jorge @uesc.com; Ilh´eus, Brasil Rodovia 16, 45662-900, km Cruz, Amado Santa de Estadual versidade nvriaed ˜oPuo A,Bai (jane.gregorio.het Brazil S˜ao IAG, de Paulo, Universidade ntttdAtohsqed ai,France. Paris, de d’Astrophysique Institut aoa´rod srfıiaTerc bevcoa,Un Observacional, Astrof´ısica T´eorica e de Laborat´orio .Gregorio-Hetem J. SOITDT ON CLUSTERS YOUNG TO ASSOCIATED H AUEO -A SOURCES X-RAY OF NATURE THE < y)cutr soitdt h arc- the to associated clusters Myr) 5 Gemini RUDSH2-296 AROUND ∼ 5)o h niesml fX- of sample entire the of 15%) Montmerle 1 .Fernandes B. , eecpst ofimteex- the confirm to telescopes 2 Hα esrda 10% at measured 1,2 n T. and , 139 em i- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ftecodpoetdi the in projected distribution cloud density the the from in of centrally differs found a that substructures has stars the cluster of this distribution that concentrated that shows sample frac- our analysis The of tal clus- behaviour. object the statistical only ), anomalous the presents A95 is 541, 6530 A&A, NGC 2012, ter work previous al. a 2011, in et presented (Fernandes al. As an et 627). (Lomax on 412, MNRAS, points based works of other distribution corre- artificial to cloud-cluster compared good when a sam- is lation, the there of that most indicate dimension of ple fractal parameters The statistical other clusters. distri- and young superficial the stellar the of the evaluated bution of that profile A107) density 547, radial Gregorio- A&A, se- and (2012, Santos-Silva was by Hetem sample study The the from members. lected cluster the distri- of spatial the bution com- with to structure geometric designed their analysis, means pare fractal by statistical evaluated Q was the aim- clouds of the clouds. clusters dense of star to structure young association The their 21 characterize of to ing study a present We 2 @ufabc.edu.br). 1 140 htteoiia lu emtywscagdb the by changed formation. was cluster geometry cloud original the that a nteds ssffiinl oie ob coupled be to ionized sufficiently is disk the the in if exists gas only mechanism disk this to However, leads accretion. that magneto- turbulence a is (MHD) for hydrodynamic (MRI) responsible instability mechanism ob- the central magneto-rotational probably the The into accreted accre- be ject. mo- to an of angular order of their process in lose mentum formation the must material in the whose disk is general, tion In there formation dust. star mag- pro- and turbulence, the field to of: netic rise formationconsisted gives star that of cloud cess the of ambient The UT RT-TLA CRTO DISKS ACCRETION PROTO-STELLAR DUSTY LSESADTERPRNA CLOUDS: PARENTAL THEIR AND CLUSTERS nvriaeFdrld B,CC,Bai (annibal.hetem Brazil CECS, ABC, do Federal Universidade nvriaed ˜oPuo A,Brazil. IAG, S˜ao Paulo, de Universidade NRAEO OIAINFATO OF FRACTION IONIZATION OF INCREASE .Hetem A. NTEASCAINO ON STAR YOUNG OF ASSOCIATION THE ON TTSIA RCA ANALYSIS FRACTAL STATISTICAL A YDMIGO ALFV OF DAMPING BY 1 .Gregorio-Hetem J. , n .Santos-Silva T. and .Jatenco-Pereira V. A 2 V NWAVES EN ´ .Fernandes B. , 1 2 a,suggesting map, ABSTRACTS 2 , usp.br). 05508-090 - Mat˜ao, 1226 (vera.jatenc Universit´aria, do Brazil Cidade S˜ao SP, Rua Paulo, S˜ao Paulo, de Universidade 1 R nalrepr ftedisk. the of part the large of a ion- presence in the the MRI increase possible and can making disk fraction, mechanism the ization this to waves that en- the show of of we damping transfer to the the due from study waves ergy We the to resonances. coupled mag- cyclotron highly a dust- are in the disk grains near netized charged damping since a frequency, heating suffer cyclotron waves additional The an the as source. study Alfv´en we waves work means of this by damping in heating models alpha-prescription, viscous the the the in of Besides included often field. mechanism magnetic the to e ftetruetrcneto iuincoefficient diffusion reconnection val- turbulent obser- effective the of the with ues evaluated consistent have we also Finally, is vations. magnetic which helical geometry predominantly field sim- a our in develop up have built ulations we cores supercritical Besides, the that nearly observations. found become the them with is of which consistent sub-Alfv´enic cores, few supercritical, a or only critical but collaps- from clumps, flux magnetic ing remove to able is RD nearly that confirming and trans-Alfv´enic turbulence, strength and gravity, transonic field is between magnetic interplay core the supercritical complex self-gravity, a a of by formation in- regulated results the Our that collapse. clump dicate its cloud induce subcritical and initially supercritical strong an becomes make RD to which enough identi- under also conditions have We the that efficient. fied is demonstrate RD We setup self-gravity. our within gas the the for of account effects also and spher- cylindrical potentials with gravitational clouds in ical realistic more diffusion consider recon- reconnection we numeri- clouds, of of earlier process studies Extending a cal (RD). induce diffusion can nection turbulence the pres- of the of Fast in ence place regions the collapse. takes which the outer from reconnection prevent magnetic the can required this some to otherwise is stars cloud, regions form flux inner to magnetic denser, clump of cloud transport molecular a For H OEO EONCINDIFFUSION RECONNECTION OF ROLE THE .R .Le˜ao M. R. M. nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto NTEGAIAINLCLAS OF COLLAPSE GRAVITATIONAL THE IN UBLN LU CORES CLOUD TURBULENT Santos-Lima 1 .M eGueaDlPino Dal Gouveia de M. E. , 2 n .Lazarian A. and , 3 2 o@iag. R. , icas, XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes oa sdet oteato fteR ahrthan rather RD the of action diffusivity. the numerical to to re- to flux due magnetic is detected moval trans-Alfv´enic the initially that ensuring for clouds, especially numer- the than diffusion, larger much ical are they that found and a eCie atao-Chile. - Santiago Chile, de dad 3 France. - Grenoble (styx@fisica.ufmg.br). Brazil Hori- 2 - Belo MG 31970-201 zonte, - 6627 Antˆonio Carlos, Avenida Gerais, 1 2 Cient´ıfica, UNICAMP. 1 3 USP. rfie ncasclTTuisas n dpigi to it adapting H and the stars, Tauri model T classical in profiles ehns htaersosbefrtefrainof formation the H for the accretion responsible and are ejection that the mechanism of us understanding give the better from will a work data with This being it observations. is compare interferometric line we this then where and region formed, the showing map sity a xli rntti iei hs objects. these in line this not mechanism or wind explain disk can a whether and stars, Ae/Be big rfiewihi omnidcto fwn.Its wind. of indication common a H re- is circumstellar which H profile its the in Moreover the processes gion. in ejection accre- of star and evidence Herbig shows tion Ae it and brightest hemisphere the northern is Aurigae AB oeta led a enue omdlteH the model transfer to radiative used been a had Using already that where this ejected. code region being With the is AU. observe wind AB the 1 to of possible than case it’s the smaller in resolution, sizes size: represent in arc Aur of milliseconds de- of spec- resolve tails can VEGA which the CHARA-array, the by in region, inter- trometer optical spectral stars. the using Tauri in disk observed T ferometry a been classical is has the variation Aurigae of AB this those explain to processes to similar the used wind of be One can side. that blue-shifted its in occurs NIOMN FA U SN H H THE USING AUR AB OF ENVIRONMENT .H .A Lima A. R. H. G. M C NS-Dpraet eAtooi,Universi- Astronomia, de Departamento - CNRS FCA UMI nvriyo Wisconsin. of University α ntttd lneooi tdAtohsqed Grenoble, de d’Astrophysique Plan´etologie et de Institut eatmnod ´sc,Uiesdd eea eMinas de Federal Universidade F´ısica, de Departamento nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto nttt eMtmaia sa´siaeComputa¸c˜ao e Estat´ıstica Matem´atica, de Instituto iei eyvral,adms fti variation this of most and variable, very is line α OEIGTECIRCUMSTELLAR THE MODELING ieaon BAradi oeo h Her- the of some in and Aur AB around line α iei BAr ecluaea inten- an calculate we Aur, AB in line n .Benisty M. and 1 .Perraut K. , α LINE iesosaPCgitype P-Cygni a shows line 2 2 .Dougados C. , α 2,3 ABSTRACTS icas, line α , oeeu betsmlsrqie osuydisks, study to ho- required and samples large stars provide object of they side, mogeneous origin one back- the On the on planets: are and studies regions observational of forming star bone of surveys Deep auld at rz apsSaeNzred An- Salobrinho, de Nazar´e Bairro (pockerrohan@gmail. [email protected]). 16, Soane Ilh´eus-Bahia-Brasil [email protected]; Km com; Campus 45662-900, Amado, Cruz, Jorge CEP Rodovia Santa drade, de tadual 1 ceitc fteds+trsystem. disk+star char- specific the the of of acteristics independent be stars to the appear the rates, results As accretion to and older. overall masses different become thinner have objects studied age become the the disks as maps extent the the scale objects: height accretion the the the that of of show part We central Disk the the disks. Emitting predict for (Jet also behavior which models same Disk), SAD Accretion Standard + + JED obtained the solutions the with of analysis qualitative a make r ihe,coe n hne nisinrregions, inner with its disks the in with thinner compared expected) and when (as cooler disks the lighter, that are show results Our stant. slae l 20) ecmaeorrslswt the with for results disks our same the compare of We solutions (2009). al. et Isella fteaglrmmnu r otoldb h vis- the by controlled parameter, are cosity distribution Sun- momentum and angular accretion & the the (Shakura of disks, disks these In accretion yaev). standard struc- of vertical and ture radial the for solutions present We rto ik rdc that predict disks cretion ik ftevsoiycnb ecie yapwrlaw power a by described be ν can viscosity the if disk, hwdta o apeo 4yugselrobjects, stellar young 14 of − sample a for that showed o 1o hs bet,using objects, these structure of the computed 11 have for we evidences, these on OPEECNU FBONDAF IN DWARFS BROWN OF CENSUS COMPLETE .R .O Magalh˜aes O. S. R. E. TAYSAEACEINDS MODELS DISK ACCRETION STEADY-STATE 0 rgaad P´os-gradua¸c˜ao Es- Universidade de F´ısica, Programa em ∝ . .Muzic K. 8 R ≤ .Geers C. H OY UVY OAD A TOWARDS SURVEY: SONYC THE γ γ with ≤ TRFRIGREGIONS FORMING STAR 1 0 .Scholz A. , γ . 4 ,idctn that indicating 8, IHVARIABLE WITH .Dawson P. , .Rcnl,Iel ta.(2009) al. et Isella Recently, 1. = α .Vasconcelos J. efsmlrt ouin o ac- for solutions Self-similarity . .Tamura M. 1 .H Cerqueira H. A. , 2 .Jayawardhana R. , α 4 utb osato the on constant be must .P Ray P. T. , α α 5 ( 10 = R 1 α specie by prescribed as ) α = − α 3 osat We constant. α o10 to 4 ( and , R 1 n M. and , .Based ). 3 − V. , 1 con- , 141 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes Japan. 5 Ireland. Studies, 4 Canada. Toronto, 3 Kingdom. United 2 1 candi- of spectra NGC1333, 700 in than objects more date obtained spectroscopic which have in VLT, we extensive and Subaru by with campaigns followed follow-up optical and deep motions, proper conducted with combined have star photometry, near-infrared nearby We and in provide population regions. to substellar forming the project of ongoing census an a is Clusters”, Young fun- theory. are formation which star (IMF), on Function constraints Mass damental limit Initial low-mass the the such and of side, shape other the the determine surveys On multiplicity. and accretion, 142 h uselrIFi o elcaatrzddw to down groups, characterized other well ∼ now of is efforts IMF substellar the the and to Thanks survey close SONYC limit. masses burning the with Deuterium the objects below or of objects, to, handful substellar a and new them identified 60 among have We than more Lupus-3. characterized and Sco, Upper I, d6 nte motn ic fifrainfor to down information that, of is piece theories formation important 2 star between Another the lies dwarfs 6. brown to ad respect with stars of u ntelts nig nNC33 uu- and Lupus-3 NGC1333, in fo- findings Upper-Sco. and latest results, the main on cus its discuss survey, SONYC the clusters the neglected. their of be budget that can mass so the stars, to contribution are than total numerous masses less planetary times with 20–50 objects free-floating the .Navarete F. bevtoa vdne.Totere rdc the of predict star: lacks theories massive of objects Two formation such moreover, of evidences. and formation observational Way of Milky processes the the in were identified stages formation clearly early in stars massive few Very colo hsc srnm,S.AdesUniversity, Andrews St. Astronomy, & Physics of School eateto srnm srpyis nvriyof University Astrophysics, & Astronomy of Department uoenSuhr bevtr EO,Chile. (ESO), Observatory Southern European 5 colo omcPyis ulnIsiuefrAdvanced for Institute Dublin Physics, Cosmic of School OAD APEO ASV YSOS MASSIVE OF SAMPLE A TOWARDS UVYO XEDDH EXTENDED OF SURVEY A OY,sotfr“uselrOjcsi Nearby in Objects “Substellar for short SONYC, nti otiuinw ilpeettesau of status the present will we contribution this In ainlAtooia bevtr fJpn Tokyo, Japan, of Observatory Astronomical National − 10M J n efidta h ai ftenumber the of ratio the that find we and , 1 .Damineli A. , .Blum D. 1 i ρ .L Barbosa L. C. , ymrigo o mass low of merging by ) pici Chamaeleon- Ophiuchi, 3 2 EMISSION 2 n R. and , ∼ 5M ABSTRACTS J , 3 2 ([email protected]). Brazil S˜ao Paulo/SP, E-302, 05580-090 Office Mat˜ao, 1226, do S˜ao Rua de Paulo, Universidade 1 B)Cua nvriai,Pbl´nIF,Ciudad IAFE, ([email protected]. Pabell´on Argentina ar). Aires, Universitaria, Buenos de Aut´onoma Ciudad UBA) 1 tr or stars lrhdoe rniina 2.12 at molec- transition the hydrogen through formation ular star massive on earliest the of investigate Based stages to designed was MYSOs. survey no a with that, are associations both there for on but evidences found YSOs, were low-mass cen- and structures the intermediate Those to associated sources. outflows tral bipolar the is of scenario presence accretion the for evidences prominent ol aebe ntae yteRImechanism. RDI the BRC by the initiated the in the been embedded that have On objects could suggests stellar BRC. young balance the of pressure being birth of the are layers hand shocks external other that the show and in clump we driven the gas, of molecular the border gas the illuminated ionized of the the evalua- at between periphery the balance located the pressure From the in of G52.85-0.55. tion located region BRC HII evolved a of multi-wavelength a study out radiation-driven carried We as (RDI). known responsible implosion mechanism be formation the star might subsequent through and stars collapse the OB triggered dark for of these nearby of by periphery illumination clumps The the regions. in HII dense evolved located and clouds small are molecular (BRCs) clouds Bright-rimmed ihteI aea pra SA,Cie and H Chile) Extended (SOAR, Spartan Hawaii). (CFHT, cameras WIRCam IR observed were the sources with the and program Source MSX ∼ n flwms tr ol o rdc jet-like produce not would stars mass structures. low merg- the of since scenario, ing re- accretion These the mor- support outflows. sults bipolar collimated have the suggesting sources) of phology, 30% (50 and sample detections the positive of 55% toward found was TD FTIGRDSA FORMATION STAR TRIGGERED OF STUDY nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto OO usn rzn,USA. Arizona, Tucson, NOAO, Brazil. Campos/SP, S˜aoUNIVAP, Jos´e dos nttt eAtoo´ayFıiadlEpco(CONICET- Espacio F´ısica del Astronom´ıa y de Instituto 0 YO addtswsslce rmteRed the from selected was candidates MYSOs 300 .E Ortega E. M. NABIH-IMDCLOUD BRIGHT-RIMMED A IN ii ya crto ik n ftemost the of One disk. accretion an by ) 1 .Paron S. , Petriella 1 .Giacani E. , 1 .Asml of sample A m. 1 n A. and , 2 emission icas, XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes asi 01 iutnoswt h 01CoRoT 2011 40 during the second with the Simultaneous and 2011. 2008 in in first days days the 23 satellite, for CoRoT the time by twice observed was G 24i on ( young a is 2264 NGC 5 4 3 ([email protected]). Chile Serena, 2 La 1200, ternas 1 nune yteeegtcato fnab and O nearby of stars. action massive B energetic the are by which clus- influenced globules, those bright-rimmed with to compared populous associated be ters and will regions in- they and the star-forming clusters, of large free relatively of formation fluence star laboratories the simple clusters study are These to globules dusty contamination. subtrac- to field for associated star methods the and of analyzed tion be are to sample we full clusters the Now, of establish to fields. procedures the star in candi- working surrounding the cluster the of the and comparison for dates the function from morphology luminosity also observed the and images from the determined on are clus- The positions areas photometry. ter PSF surrounding through and comparison are candidates for we cluster Firstly, both, for diagrams 2014). color-magnitude and Serena color-color al. producing La (Barb´a et of Group members VVV by clus- stellar developed VVV dusty candidates new to ter the associated from selected clusters are dark of globules to sample associated This candidates set clouds. clusters a small of four properties of near-infrared the analyse we tion, L´actea V´ıa (VVV) of the sample survey infrared a public under and observed ESO/Chile globules of been have dusty that study to clouds bright-rimmed associated a clusters from star small results present We NRRDSUYO E TRCLUSTER STAR NEW OF STUDY INFRARED .P Sousa P. A. Jaque H NE IK FCASCLTTAURI T CLASSICAL OF DISKS INNER THE eatmnod ´sc,Uiesddd aSrn,A.Cis- Av. Serena, La F´ısica, de de Universidad Departamento .St King Soto P. .UiesddCat´olica (Chile). Universidad (USA). P. Institute Science Telescope Space (Argentina). IALP-CONICET (Argentina). ICATE-CONICET ADDTSASCAE ODUSTY TO ASSOCIATED CANDIDATES .Bouvier J. 1,2 .Firpo V. , 1 .T McGinnis T. P. , 1 TR NNC2264 NGC IN STARS .Barb´a R. , 2 .Teixeira P. , 1,3 GLOBULES .Minniti D. .L Nilo L. J. , ∼ nti hr communica- short this In . y)selrcutrthat cluster stellar Myr) 3 1 .Roman-Lopes A. , 3 n .Stauffer J. and , 1 5 .H .Alencar P. H. S. , 1 .Soto M. , it aibe in Variables Vista 1,4 1 and , 4 M. , ABSTRACTS 1 , uti h ne ikaesbtnilydffrn from different substantially ISM. the are the disk of inner properties the in the dust alone, is variability extinction the to if lo- attributed that, explain warp and indeed variability disk can observed radius the inner curve co-rotation an the light near that Initial cated indicate 2264. results NGC model in Tau-like observed AA photo- the the CTTSs of present analysis We spectroscopic ra- and system. co-rotation metric star-disk the inho- the to is of close dius material located occulting and the mogeneous and interac- dynamic The star-disk is axis. the tion rotation indicates stellar variability in- the observed field to star-disk magnetic respect the stellar with by clined a created by inclination. be mediated high to interaction thought at AA is seen in warp observed CTTS This like studied rotates, well eclipses system that a warp Tau, the disk as in- inner star are an the curves to light due These as depth terpreted timescale. and deep rotational width with a in in curves substantially vary light accret- that optical the minima of exhibit fraction systems in a shown ing campaign, As about CoRoT stars. Tauri members, first T cluster the classical 500 are and which than of optical more 200 the for in IR curves simulta- near light obtained precision We high data, (CFHT). neous Chandra photome- Megacam band of from U days try and 3.5 spectroscopy microns, FLAMES 4.5 VLT and observations 3.6 Spitzer of at days 30 or- included was that ganized campaign multi-wavelength a observations, intrso trfrain omnyosre at observed commonly formation, star of infrared without signatures earli- phase the core represent (starless) quiescent cores protostellar Quiescent est a from one. active phases, an different to in be may IRDCs 0p n aso 10 of mass a and pc 10 – )addne( dense and K) nrrdDr lus(RC)aetecl T cold the are (IRDCs) Clouds Dark Infrared 4 (alana Brasil 3 - IPAG. MG Horizonte, Belo 2 31270-901 @fisica.ufmg.br). - 6627 los, 1 nvriaed eea eMnsGri v Antˆonio Car- Av. Gerais Minas de Federal de Universidade pte cec etr-Caltech. - Center Science Spitzer Universit¨at f¨ur Wien. Astrophysik Institut .Vasquez J. ILMTRADFRI OBSERVATIONS FAR-IR AND MILLIMETER ntttd lneooi tdAtohsqed rnbe- Grenoble de d’Astrophysique Plan´etologie et de Institut FTEID G341.24-0.27 IRDC THE OF 1,2 > .Cappa C. , 10 5 cm Rubio − × 3 1,2 ein,wt cl f1 of scale a with regions, ) 2 − .Romero G. , 3 5 M ⊙ oe ihnthe within Cores . 2 n M. and , < 143 25 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes u rlmnr iayfato of birth. fraction at binary not) preliminary (or Our starts scale sub-AU that at piece namely, multiplicity important puzzle, an star-formation (binary) bring the will been into it have confirmed, the If might that found. hints binaries us proto-spectroscopic give analyzed nature. first targets stellar the of of are that Three uncovered indicating velocities pre- radial profiles with the well photospheric reasonably stellar agree dicted sample proto- the our of in spectra earth’s stars the the that target by found We the established atmosphere. zero-point of velocity the to radial relative function the cross-correlation deliver to 2-D region designed a forming using star derived the were in objects ρ stellar resolution young high 7 near-IR a (R present spectroscopic we young such companions, finding for- at their Aiming in involved mation. scales time the the understanding and for mechanisms clue invaluable would forma- an binary therefore star spectroscopic be in young a question uncover open To an tion. mul- still pristine is systems within resul- tiple evolution or dynamical the clouds, of from molecular by-product tant a of are fragmentation they initial If companions spectroscopic formed. how actually unclear are it- still process is formation explained star it easily the self, of be outcome normal can a distances as visual com- stellar at in of panions found existence the mostly While are systems. neighborhood multiple solar the in Stars 2 gentina. 1 4.5 extended have enhanced cores and active while wavelengths, IR far 144 312-.7adG4.202() rjce onto G341.24-0.27. projected IRDC far-infrared the G341.22-0.26(a), Objects) and Green and mid- (Extended G341.23-0.27 and EGOS the lines, towards data CO(2-1) and 1), 3 Argentina. iewt h ointa utpiiyi eyhg at high very is multiplicity that notion the with line .VaaAlmeida Viana P. IAIS RCS UT-PC RADIAL MULTI-EPOCH PRECISE BINARIES: autdd inisAto´mcsyGo´scsd aPlat La Geof´ısicas Astron´omicas de y Ciencias de Facultad eatmnod srn´ma nvria eChile. de Astrono´ımia, Universidad de Departamento nttt retn eRdosrnmı,CNCT Ar- CONICET, Radioastronom´ıa, de Argentino Instituto picu.Terda eoiiso ahsource each of velocities radial The Ophiuchus. nti ok eaayeC(-) 13CO(2- CO(2-1), analyze we work, this In ∼ Figueira EOIISO RTSASIN PROTOSTARS 7 OF VELOCITIES IDN PROTO-SPECTROSCOPIC FINDING 00)mlieohrda eoiysre of survey velocity radial multi-epoch 60000) 1 .Sterzik M. , 1,2,3 emission. m OPHIUCHUS .Melo C. , 2 n .F Gameiro F. J. and , 2 .C Santos C. N. , ∼ 1 sas in also is 71% ρ 1 1 P. , ABSTRACTS a, on u,adteeoeti aito environment. radiation this the therefore of could and Sun, characteristics analogs young the stellar about Solar ori- at- information the life. provide planetary of in evolution of and and evolution conditions gin the surface in their role mospheres, a play emit- radiation could for 1700 particular below in ted that Sun, than present stronger ac- much the magnetic was of the Sun young Earth the the of of tivity ages early the During iloe e eu o h nesadn nthe system. on solar understanding own the our for of This venue origin new formation. of a process open the close- will in around just an- stars planets high young reveal by and might sensivity resolution its gular finished, place. taken is are ALMA formation When star disks and circumstellar planet the the where of the parts study innermost to allowing obscured regimen those optical to the similar in obtained resolutions angular provide Millime- now of Large ries observato- Atacama These era (ALMA). the Submillime- Array in and ter/Submillimeter the (SMA) studies on Array formation observatories: ter challenges planet submillimeter and and the advances star recent the the present I nˆ noCro,62 ets,Bl oiot G 31270- MG, palmeida@fisica.ufmg.br. - Brasil, Horizonte 901, Belo Ventosa, - 6627 Antˆonio Carlos, 3 Chile. tiago, Portugal. 2 Porto, 4150-762 trelas, 1 1 on gsadteeoei ih eapoutof product a be might it therefore star-formation. and ages young .Odert P. SRBOOIA PRAHT STUDY TO APPROACH ASTROBIOLOGICAL .C Abrevaya C. X. S,Aos eCroa30,Csla101 iaua San- Vitacura, 19001, Casilla 3107, Cordova de Alonso ESO, nvriaeFdrld ia eas vnd Presidente Avenida Gerais, Minas de Federal Universidade etod srfıia nvriaed ot,RadsEs- das Rua Porto, do Astrof´ısica, Universidade de Centro etod aiatoo´ayAtosc Cy) UNAM. (CRyA), Astrofisica Radioastronom´ıa y de Centro TRADPAE OMTO NTHE IN FORMATION PLANET AND STAR TR TLA SYSTEMS STELLAR & STARS R FTESUBMILLIMETER THE OF ERA BEVTRE SMA/ALMA OBSERVATORIES 2 H ISNPOET AN PROJECT: BIOSUN THE .E Horvath E. J. , n .F ot eMello de Porto F. G. and H RGNO LIFE OF ORIGIN THE 1 .Sc nacdrdainfluxes radiation enhanced Such A. ˚ .Hanslmeier A. , .Zapata L. 1 .Ribas I. , 1 2 .Leitzinger M. , 3 .Galante D. , 5 2 4 , , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes h aaotie previously. obtained to data according the conditions, simulated environments laboratory under this to expos- out microorganisms/molecules carried ing be Finally, will approach conditions. experimental planetary the prebiotic early some the of in outflow c) molecules halites; and and inflow meteorite formation, Nakhla con- The the we model studies a Mars as For sider time. that of at possibility Mars or Venus-Earth The Mars-Earth Early between b) microorganisms tested; of also “transfer” record. be fossil will Europa microbial and at the confronting Earth survive with early could the that on cells radiation of Whether level that explore: radi- con- this to simulated could 2)Reproduce ditions laboratory or under are life. environment that for ation System suitable Solar been plan- the have radia- other of and the bodies Earth Characterize early etary the 1) ra- of environment to the through tion Sun analogs on young focus stellar the to solar of is features project emission this diation of objective The oMto12,Cdd nvri´ra 50-9 a Paulo, Sao 2 Universit´aria, 05508-090 ([email protected]). Cidade Brazil 1226, Matao do 1 5 4 3 Austria. epeet9Lbn pcr fteB star Be the of spectra L-band 9 present We aeb eozre l 20) ept h atthat fact the one Despite the (2002). as al. diagram et widths Lenorzer ratio by line flux made line strengths, a line constructed ejection and measured matter Be We the including of time episodes. evolution along the envelope study star to documented order well in relatively outbursts of time chose recurrence We short envelope. star the opti- of the conditions in changes depth to cal sensitive are Hy- that diagnostic lines important from drogen contains region microns L-band 4.1 The to 2.9 presented. also are years 13 the for mates erdrn neoho eaiepooercquies- ∆ photometric a relative to 1 prior of cence along epoch distributed an during ISAAC VLT year the with obtained .Aguayo G. UT-PC NRRDSPECTROSCOPY INFRARED MULTI-EPOCH nttt fPyis alFazn-nvria rz Gr Graz, Karl-Franzens-Universitat Physics, of Institute bevtrod aog/FJ i eJnio Brazil. Janeiro, de Rio Valongo/UFRJ, do Brazil. Observatorio Paulo, Spain. Sao Barcelona, Campinas, l’Espai/CSIC, CNPEM/LNLS, de Ciencies de Institut ulod eqiae srbooi/A S,Rua USP, - Astrobiologia/IAG em Pesquisa de Nucleo etuia u agtdet t rgtesand brightness its to due target our as Centauri OF ETUIPIRT OUTBURST TO PRIOR CENTAURI 1 .E Mennickent E. R. , V antd banddrn h last the during obtained magnitude V . a ubrt iulesti- Visual outburst. mag 0.4 = Granada 3 1 .Otero S. , 2 n A. and , ABSTRACTS Cen az, odto utpirt ao outburst. thick major optically a an to to prior just thin condition optically envelope, an circumstellar from the moving of opacity as the variability in this changes interpret We series. Humphreys to trOsres(AS) abrg,M,USA. MA, Cambdrige, 3 (AAVSO), Observers Star (gusaguayo@astro-ude 2 Concepci´on, Chile. 160-C, Casilla 1 2 Bogot´a, ([email protected]). Bogot´a, Campus Colombia Colombia, de Nacional Universidad 1 qiaetwdh fafis u-apeo 3stars. 33 of sub-sample the first report a We Obser- of Haro Mexico. widths equivalent Guillermo Sonora, Cananea, the in on of vatory spectrograph telescope echelle 2.11m CanHiS the the were with (R=65000) obtained data brightness. G intermediate spectroscopic type resolution of ex- (spectral High V) an class stars in luminosity solar-like project and abundance of a Li sample of the tended results determining preliminary at present aimed compan- We sub-stellar of be ions. presence to the appears with en- abundance convective correlated Li with Additionally, stars for Li indicator velopes. of age hand, result an other a be the can as On element this nucleo-synthesis. of primordial abundance the on restric- tion strong global a with provides stars abundances in metal present sub-solar in lithium the hand, On importance one astrophysics. the fundamental contemporary of of contexts multiple is stel- in atmospheres abundance lithium lar the of determination The NO,Tnnznl,Pel,M´exico. Puebla, Tonantzintla, INAOE, LN UBRT DIINLEVIDENCE ADDITIONAL OUTBURST: ALONG efudtesa noaqisec eid eob- we Bracket- emission of in period, strength changes line quiescence monotonic a and into significant serve star the found we .M Amazo-G´omez M. E. eeaOsraoyUiest fGnv,Switzerland. Geneva, of Observatory,University Geneva nvria eCnec´n eatmnod Astronom´ıa, de Concepci´on, Departamento de Universidad unsArsAgniaAeia soito fVariable of Association Aires,Argentina;American Buenos bevtroAto´mc ainld ooba OAN, Colombia, de Nacional Astron´omico Observatorio nttt ainld Astrof´ısica, de Nacional Instituto .Dagostino C. EEMNTO FL BNAC IN ABUNDANCE LI OF DETERMINATION OA YESASO INTERMEDIATE OF STARS TYPE SOLAR CRTO ICMP FV01OPH V2051 OF MAPS DISC ACCRETION NFVRO H MASS-TRANSFER THE OF FAVOR IN NTBLT MODEL INSTABILITY 2 .Bertone E. , BRIGHTNESS 1 .Hernandez- B. , α n Pfund- and 2 n .d aLuz la de V. and , piayElectr´onica, y Optica ´ γ Aguila ´ ie relative lines 2 M. , c.cl) 2 145 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes S49S0.I rvoswr,temto of method the work, na- candidate previous (OCR) physical a remnant the In cluster assess open ESO429-SC02. to the intend of we ture study this In ray- ([email protected], Brazil [email protected]). Catarina, 1 146 o fteMI(atsae l 07.Hr we Here 2007). velocity-resolved of al. fa- et ( analysis in (Baptista mapping the evidence eclipse MTI DN stronger report the yielding of of DNs group the vor a Oph of V2051 is MTI. one by there is powered are has that which decade idea of outbursts last sup- the the in of model, evidence port DI compelling set- the provided be of progressively to mass-transfer favor seemed enhanced issue in the of tled While burst model). MTI a mass-donor or (the to the model) in leading instability DI an star (the of disc consequence accretion a as the in insta- cycle thermal-viscous to a bility fac- of by weeks because brighten either discs 20-100 from tors accretion timescales their to which on days in years, recurring from and lasting binaries weeks outbursts, mass-exchanging repeated are showing (DNs) novae Dwarf n uwrswt eoiisof velocities with inwards spreads outwards which and radius, emission circularization enhanced of the ring at a with on starts telescope. outburst ESO based The m outburst, 1.5 the consec- July with 4 2002 collected spectroscopy on its Oph along nights V2051 utive of curves light continuum ict us fdne nacdmass-accretion enhanced regions. dense, outer of sparse viscous good its burst a through in a of are to response but expected disc model, the DI with odds the agreement at are of results The predictions below nights. with remain other and all on model, limit in that DI while to be according should tempera- gas outburst disc the critical which the the above reach barely temperature pc, maximum 108 outburst novae. at of dwarf tures distance outbursting other a the in Assuming of seen reminiscent arms arcs maximum spiral outburst asymmetric The two day. shows a map than less in disc +0 | .S Angelo S. M. v PCRSOYO H PNCLUSTER OPEN THE OF SPECTROSCOPY rp eAto´sc,Uiesdd eea eSanta de Federal Universidade Astrof´ısica, de Grupo | . 2 400 = ENN ADDT ESO429-SC02 CANDIDATE REMNANT km/s .L Andrade L. E. − epciey ofr netne bright extended an form to respectively, , 1000 Jr. 1 .J .Corradi B. J. W. , 1 km/s n .F .Maia S. F. F. and , ) 1 Hβ n .Baptista R. and , e λ HeI 1 − ≥ .F .Santos C. F. J. , 92adnearby and 4922 1 0 . 9 1 km/s ABSTRACTS and Hβ tr ln h ieo sight. field of line of overdensity the suggest along random results stars a Our is system. ESO429-SC02 coeval that a for what expected with pa- is inconsistent the are in them for dispersion derived high rameters along the spectral and stars sequence Besides, member main the candidate km/s. 64 of to distribution types 9 from velocities dial 0 u ut-betsetocp f3 tr nisin- its in stars 31 (r area of ner spectroscopy an carried We as multi-object OCR. or possible out OCR a as an it (2007) as classifying object asterism, Bica the & characterize to Pavani failed by devised characterization rm1 from R inr ouin(rmorcd)o a or sta- code) the our use trial we (from this initial solution for tionary integrate, an to needs start to ZEUS-3D solution hy- we code. numerical our results drodynamic from stability their solutions stationary compare their the we with then confirm and ZEUS-3D, to code called hydrodynamic order numerical time–dependent a In use lutions. ( tigslto a on,idvda itne of distances the individual to close found, stars was solution fitting te yaPdv scrn in well isochrone Padova stars a those by selected fitted and outliers inter- reject to data actively kinematical an sigma-clipping positional 5-dimensional using routine a member performed candidate identify we our to stars, for order derived In were stars. values science reddening and spectroscopic via parallax distances Individual UCAC4. motions from proper and em- data photometric also radial We 2MASS from ployed obtain parameters. templates to atmospheric and all libraries velocities PHOENIX with and spectra ELODIE science our task) 1 h eoiyaddniypolso h stellar the Ω– of fast, profiles for the density solutions namely: known and winds, three velocity of possess the winds stars radiation–driven of massive theory the Currently, ut.Fs n ohso ttoaysltosare solutions stationary re- slow same both the and obtain we Fast cases both sults. In field. velocity ATADSO AITO-RVNWIND RADIATION-DRIVEN SLOW AND FAST J . hsc eatet-IE/FG(Brazil). ICEx/UFMG - Department Physics o0 to 0 − ≈ .Araya I. H 00.W rs-orltd(RFsFXCOR (IRAF’s cross-correlated We 2000). . ) p o4 to kpc 5 . × 6 [ 46; OUIN SN ZEUS-3D USING SOLUTIONS ( ∼ < H 4 1 e/H F − .Cur´e M. , ′ sn MSGMN- (resolution GMOS/GEMINI-S using ) K . kpc; 4 s unffpoint turnoff igas lhuhaisochrone a Although diagrams. ) from ] Santill´an 1 E .ud-Doula A. , ( − B 0 − . 5t 0 to 95 3 slow V rt h G range RGB the to or K ausrnefrom range values ) s × and . 1dxadra- and dex 61 2 ( β J n A. and , lwfrthe for –law δ − – slow K s and ) so- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ubto ttebs ftewn nodrt study to between order oscillations in or wind the transitions per- of possible small base of the effects at the turbation exploring wind are better. the we nature is Currently, its of investigation understand result further to rotation. but needed the high overloaded, likely with mass most stars being are for kinks (2007) by Such obtained al. ones et the to Madura similar profiles, velocity the eoiypol) nsm ae eobtain we and cases density some (base in sensi- conditions very profile), boundary is velocity the ZEUS-3D that to found tive we addition, velocities In terminal 3%. the than code, lower between our and velo- differences ZEUS-3D the from having Further- with fields agreement density good stable. and very city all a is are there and more, ZEUS-3D in attained ioCt,Mexico. City, xico 3 2 ([email protected]). Chile n atsolutions. fast and ut,aatd otl320 unjao ´xc (santi- M´exico Guanajuato, 36240, postal [email protected]). apartado juato, 1 1 ySliae l 20) efidtelmtvalue limit the find we (2004), al. et Sollima by pcr n h htmti aabs of base data synthetic photometric the the with and models comparing spectra By evolutionary stellar band. on our photometric brightness NIR in selected depen- increase the the non-standard study the also we of Baron (1997), dence code al. PHOENIX et Hauschildt the & with synthetic With generated phases. spectra post-RGB cali- the in and the driven mechanism changes on mass-loss Reimers impact the the increase of bration and non-standard luminosity the tip-RGB degenerated stars, in the low-mass of in evolution cores late inter- and the on structure emission nal neutrino conse- enhanced the analyze of we quences prescrip- (2005), mass-loss al. Schr¨oder the et by Reimers with tion neutrino along the 2007), for of al. reinterpretation tables et STARS (Kantor numerical the decay of plasmon updated version (1995) with al. code et Pools the Using .Arceo-D´ıazS. ν nttt eFıiayAtoo´a nvria eValpara F´ısica Astronom´ıa, de de y Universidad Instituto enSaeWrhntnSrno,Dnoe USA. Dunmore, Scranton, Worthington State Penn GI,UiesddNcoa u´nm eM´exico, Me- Aut´onoma de Nacional Universidad DGTIC, FET FNNSADR NEUTRINO NON-STANDARD OF EFFECTS eatmnod srnmı,UT,Cmu Guana- Campus UGTO, Astronom´ıa, de Departamento ≤ 2 MSINO H VLTO OF EVOLUTION THE ON EMISSION . 2 × 10 − 1 12 O-ASSTARS LOW-MASS -.Schr¨oder K-P. , B . Zuber 2 1 .Jack D. , 1 n K. and , kinks ω δ − –slow ABSTRACTS Cen ´ıso, in on yCree l 21)for (2011) al. Cur´e et by found sthe as eaiesoe o h ratio the a For has relation slope. the negative hydrodynamics with found values a rse,Zlece e 9 -16 rse,Germany. Dresden, D-01069 19, Weg Zellescher Dresden, tat 2 rdnmcoe i atrbten23.The profiles velocity the 2-3). for et (1999) between Kudritzki al. hy- with factor agrees than a Relation FASTWIND Wind-Luminosity (in using obtained ones values We drodynamic loss code. mass HDUST less and FASTWIND ing al,w opr hs eut ihthe with results these compare we nally, eL lt,L lt,Argentina. Plata, La Plata, La de n oodlmgei edcmoet.Anew A components. field magnetic poloidal toroidal both for and de- allowing general summarized, these is A governing equilibria equations MHD eventually criterion. ideal a the stability can of a scription construct which using we tested equilibria, work be barotropic unstable this of dynamically In set be would 2009). barotropic (Reisenegger state a with of stars equation magnetized conjecture that recent states a confirm that timescales, to short interesting on be would stars it magnetic for re- a model constitute alistic not does matter barotropic Although 2 ([email protected]).para´ıso, Valpara´ıso, Chile. 1 eoiypol n sn h oie eso of version modified the the reproduce using to FASTWIND and the profile calculate to velocity hydrodynamics the of using types HD75149, HD53138) two HD52382, HD42087, HD80077, the (HD41117, HD52382, stars study one HD79186, SGs we B solution: Here eight of for solutions slow. types one two rota- have and slow can fast (or stars non-rotating SGs type previous tor) A from the known un- that is to studies It information important evolution. parameters us their wind give derstand stars, and SG stellar B the of of estimation The .Armaza C. ntttfrKr-udTicepyi,Tcnsh Univers Technische Teilchenphysik, und Kern- fur Institut eatmnod ´sc srnmı,Uiesddd Val- de Astronom´ıa, F´ısica Universidad y de Departamento nttt eGo´sc srnmı,UiesddNacion Astronom´ıa, Universidad Geof´ısica y de Instituto .Arcos C. NMGEI ILSI BAROTROPIC IN FIELDS MAGNETIC ON v IDSUYO G STARS SGS B OF STUDY WIND esc 1 1,* .Cur´e M. , nrae the increases .Reisenegger A. , n .Haucke M. and .Marchant P. 1 STARS .Kanaan S. , v ∞ 1 v erae,lk twas it like decreases, .A Valdivia A. J. , 1,3 ∞ H δ so solutions. -slow 2 /v α β 1 .S Cidale S. L. , esc ye u o the for but type, iepol.Fi- profile. line eobtained we , β a us- Law 2 and , 2 147 , al i- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes a 20N aSrn,Cie([email protected]). Chile Serena, La N, 1200 nas 1 1 briefly are obtained discussed. equilibria the and of configurations, properties de- these some of equation equilibrium Grad-Shafranov the so-called scribing the order solve in to developed is code numerical finite-difference 148 46Mcl atao Chile. 2 Santiago, 782 Macul, 4860, Vicu˜na0436 Mackenna Av. Chile, Cat´olica de versidad ln h ubro aatcOtp trsystems star dou- O-type almost Galactic orbits. are known of we with number since the stars, bling context binary the in massive unprecedented of is result This butions. distri- mass-ratio and eccentricity, spectral-type, the period, luminosty, of analysis the spectroscopic we and O-type systems, work, fifty binary over this for deter- orbits In the of Survey”: mination “OWN days. of result 2200 periods main the to orbital present 1.5 new from The spanning binaries. and multiple-lined binaries, 9 spectroscopic double-lined spectroscopic 43 single-lined 56 binaries, being including systems, km/s, new 10 108 than of show- greater sample variations stars 146 that radial discovered From ing have we stars. stars, WN O-type der and 190 O (van spectra 240 5000 stars about almost WR of collected have Galactic We of 2001). Hucht Galac- Catalogue and the VII 2004) in the al. (Ma´ız multiplicity Apell´aniz et Catalog of O-star indication tic which no for is stars those there The to corresponds Argentina. sample and selected Chile using in campaign, facilities sustained observational of years seven completed eCie ail 5,Snig,Chile. Santiago, 653, 3 Casilla Chile, de r aatcO n Ntp tr.Tehigh- The ( and stars stars. O of WN WN-type survey monitoring high- and spectroscopic the resolution O- of Galactic south- results of ern survey main monitoring the spectroscopic resolution briefly describe We e ¨gl7,D511 on Germany. Bonn, * D-53121, H¨ugel 71, dem .R Walborn R. N. .Barb´aR. eatmnod ´sc,Fcla eCeca,Universida Ciencias, de F´ısica, Facultad de Departamento [email protected] eatmnod ´sc,Uiesddd aSrn,Cister- Serena, La de F´ısica, Universidad de Departamento readrIsiu ¨rAtooi,Uiesta on Au Universit¨at Bonn, f¨ur Astronomie, Institut Argelander nttt eAto´sc,Fcla eF´ısica, Pontificia de Astrof´ısica, Facultad de Instituto W UVY EUT FE SEVEN AFTER RESULTS SURVEY: OWN PCRSOI OIOIGOF MONITORING SPECTROSCOPIC ER FHIGH-RESOLUTION OF YEARS OTENOADW STARS WN AND O SOUTHERN 1 .Gamen R. , W Survey OWN 4 .Ma´ız Apell´aniz J. , .Alfaro E. 2 .I Arias I. J. , abae l 00 has 2010) al. Barb´a et , 5 5 1 .Sota A. , .Morrell N. , 5 and , ABSTRACTS Uni- 3 , d - f 5 4 3 2 oh oeadtasesmte oawiedwarf white a to matter transfers its and overfills secondary) lobe (the Roche star late-type the systems where binary close are (CVs) variables Cataclysmic aer,LdiaPdoAtno4,20000Rod Janeiro de Rio ([email protected]). 20080-090 Brazil 43, Antonio Pedro Ladeira Janeiro, 1 ocutraon h ik a center. Way Milky the around associated motion cluster the mean to around same rotates the with streams) center sys- (or cluster tails coordinate tidal this the In tems, energy. since around orbit, minimum likely orbit requires most it the circular is ex- a potential can dominant that We the of considering stream. center this a the thus plain direc- towards forming Way, normal direction Milky a the the in to stars related results of Our tion agglomeration orbit. cluster’s an parent show the stars to that orbits such similar to are cases, due orbits chaotic may most cluster escape In their the cases alter quickly to potential. some orbit) Galactic in chaotic the and to a stars in orbit, These (again chaotic return a Problem. with in Body understood escape be Three cap- can Restricted or cluster escape the we globular stellar work The this from of ture collision. stage that next study the center In the will Way. around disk) Milky the the (on of orbit clus- circular globular we a a in from code, ter form this streams understand tidal to how analyse order (Aarseth, in collision NBODY6 Firstly, a with 2003). by GC formed different interested two cluster are between globular of We a theories studying evolution. for in and laboratories dynamics true since stellar Universe are the systems of understanding these impor- our an in plays role (GC) clusters tant globular of study The .W Borges W. B. nttt eAto´sc eAndaluc´ıa-CSIC, Spain. Astrof´ısica de de USA. Instituto Institute, Science Telescope Space Chile. Observatory, Argentina. Campanas Plata, Las La Astrof´ısica de de Instituto bevtoi oVlno nvria eea oRode Rio do Federal Universidae Valongo, Observat´orio do AITOSI AALSI VARIABLE CATACLYSMIC IN VARIATIONS ERHN O YLCLPERIOD CYCLICAL FOR SEARCHING OLSOSBTENGLOBULAR BETWEEN COLLISIONS .T Belloni T. D. 1 .Baptista R. , 1 CLUSTERS n .J Rocha-Pinto J. H. and STARS 2 n .S Oliveira S. A. and , 1 3 , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes tradtepeec fatidbd ntesystem. the in body third a of presence the secondary and the star in activity for magnetic explanations current phenomenon: two the the is of modu- context variation observed in the the lations discuss We that periodic. indicating strictly s), not semi- 17 a of with amplitude modulation yr plus show (22 linear timings ephemeris published sinusoidal new the the from cover deviations and data significant observations Oph of V2051 years The 35 s. with 47 years modulation of 24 yr semi-amplitude covers 26 a diagram presents O-C and observations Aqr of UU The di- agrams. (O-C) observed-minus-calculated We updated OPD. con- struct to at measurements and published telescopes with timings them m combined mid-eclipse 1.6 white-dwarf obtained and new were se- m measured photometry Times 0.6 CCD the speed using Brazil). high (OPD/LNA, of Dias ries dos Observat´orio at Pico 2013 to obser- to do The 2008 project from CVs. long-term done in were of vations poster variations this results period cyclical In first study the disc. report accretion an we via primary) (the ug.Teoe lse addtsVVCL124, VVV candidates cluster galactic open the The in clusters promising are bulge. globular these new Thus, for be Galaxy. Galac- candidates should inner the they the from because in kpc unusual, rare quite few are inner center the tic However, in poor, clusters. objects metal open these old intermediate respec- as classified old, kpc be 6.98 could Gyr and and 5-10 stars. 9.2 are sequence 6.8; tively, at main projected and are clump giant They red red VVV defined some well CL119, show branch, CL150 VVV VVV The and of CL143 follow: as diagrams are color-magnitude candidates L´actea (VVV). public interesting Via ESO most the the The in by Variables covered in- VISTA the area in survey bulge projected and clusters disk open parame- ner infrared fundamental 20 and of discovery ters the report We aed aaıa ˜oJsedsCmo,Brasil. Para´ıba, S˜ao Campos, do Jos´e dos Vale Florian´opolis,3 Brasil. Trindade, Campus Catarina, CEP88905-120, 2 150, Pereira, ([email protected]). Jo˜ao Ararangu´a, Brasil Pedro Rua Ararangu´a, 1 EL ICVRDODOE CLUSTERS OPEN OLD DISCOVERED NEWLY .Borissova J. nttt ePsus eevliet,Uiesdd do Universidade Desenvolvimento, & Pesquisa de Instituto eatmnod ´sc,Uiesdd eea eSanta de Federal Universidade F´ısica, de Departamento nvriaeFdrld at aaia Campus Catarina, Santa de Federal Universidade .Kurtev R. 1 NTEVVSURVEY VVV THE IN .Ram´ırez Alegr´ıa S. , 1 n V trcutrteam cluster star VVV and , 1 .N Chen´e N. A. , ABSTRACTS 2 , ya xlso nryof energy explosion an by tr rmami eunems f1–5M 12–15 of mass sequence main a from star, 0 r le hn1Gr l lsesaevr red- very are clusters and All Gyr A Gyr. reaching 1 1 dened, and than Myr older are 100 50% between our ages from have candidates cluster sample nature. new their of confirm 15% summary, to In necessary are data more typical clusters, but supergiant show red CL130 of VVV diagrams color-magnitude and sample, CL117 our VVV from candidate. namely candidates pair cluster cluster while two new finally, Myr, And good relatively are 80 are The and clusters rich, around Both metal Gyr). estimated kpc. (1.3 older is 3.8 is CL140 CL139 of radial of modulus similar age show distance cluster other, and pro- The to are velocities each CL140, close respectively. VVV very kpc and jected projected 8.7 CL139 are VVV and They candidates 5.5 are clusters. 5.0; and open at stars old sequence as se- main classified defined and well evolved show of CL161 quence VVV and CL160 VVV n a ing ossetwt h xlso fa34M 3–4 is a SN of explosion the the that with estimated hydrody- consistent of we with curve evolution calculations, light velocity namical its the and high Modeling 2011hs SN indicating but profiles velocities. dominate, I line H features expansion by absorption I He dominated broad where spectra with spectra from SN, to of lines class this Its of typical metamorphosis shape. the curve showed evolution light spectral narrow a a by was characterized SN, 2011hs SN (Bufano (M submitted). 2011hs faint of relatively MNRAS SN sample of 2013, a particular, al., present of in et We study SNe, the IIb issues. from Type obtained open such results still of the nature are the stars made and progenitor that possible mass-loss structure of final such mechanism The explosion. fmsiesasta eeal orti nyathin a only retain to able were ( that stage stars evolutionary massive final of the are Supernovae IIb Type ’oouPaeHl,H 62,USA. 96720, HI Hilo, Place ohoku A’ 5030, 2 Casilla ([email protected].) Ancha, Chile Playa Breta˜na 1111, Gran para´ıso, Av. 1 ∼ < eatmnod ´sc srnmı,Uiesddd Val- de Astronom´ıa, F´ısica Universidad y de Departamento eiiOsraoy otenOeain etr 7 N. 670 Center, Operations Northern Observatory, Gemini M 1 56 RGNTR:S 01SFO A FROM 2011HS SN PROGENITORS: NELN YEIBSUPERNOVA IIB TYPE UNVEILING ⊙ ims qa o00 M 0.04 to equal mass Ni /eetra neoea h ieo the of time the at envelope external H/He ) UEGATSTAR SUPERGIANT V B 2 a nsm ftecases. the of some in mag =28 .Bufano F. 1. a)adrdTp IIb Type red and mag) -15.6 = E ≈ 1 ⊙ 8 . n characterized and 5 × 10 50 ⊙ ⊙ r s erg He-core eject- , 149 − 1 . XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes oeswt ecr mass core He with models R ol ne rmi rgntrrdu of radius we progenitor size, a progenitor it from cooling the infer the on could of mainly rate depends decreasing branch the Since 1993J. and SN duration to similarly the days, 8 lasting phase ing ahr,Petn R H,UK. 2HE, 3 PR1 Preston, cashire, (gcandlish@astro-udec. 2 Concepci´on, Chile 160-C, Casila 1 CLUSTERS STAR POPPED OF MIXING PHASE (milena.bufano@gmai com). Santiago Rep´ublica 252, Avda. Bello, 1 discovery the before days 6 (2,455,872 that occurred assumed we explosion evolution, the curve light the on Based 150 ainlsgaue n h esblt fdetection. of feasibility the obser- and possible signatures the vational our investigate is Using we which model, simulations. theoretical body components, N- disk with compared and com- then halo potential type bulge, Milky-Way phase prising full the disk a Miyamoto-Nagai of and a potential in evolution stars time of distribution the space describe theoretical a to construct Considering we model motions, potential. vertical the analytical only evolves background it a as mixing system in phase stellar the out-of-equilibrium to the due of arises of which source numerical structure, the Using investigate this we methods, tree. analytical Christmas and a in passing to a both with resemblance velocity, popping, vertical density and after number position stars vertical stepped cluster a of of distribution demon- existence stellar have unbound the simulations an strated N-body to the Previous leads development: This ex- system. their is pops. in cluster cluster early star the star and in low quickly with gas pelled form the to efficiencies, expected formation are clusters star As e ¨gl7,D511Bn,Germany. Bonn, D-53121 H¨ugel 71, dem unemse bv 20 above masses quence rsneo opno star. companion a does the of of curve presence signature light typically deviations, radio strong the show not although of possibility origin, the binary indicate a could mass progenitor the .N Candlish N. G. eatmnod srnmı,Uiesddd Concepci´on, de Astronom´ıa, Universidad de Departamento readrIsiu ¨rAtooi,Uiesta on Au Universit¨at Bonn, f¨ur Astronomie, Institut Argelander ⊙ eeihHrok nttt,Uiest fCnrlLan- Central of University Institute, Horrocks Jeremiah eatmnod inisFscs nvria Andr´es Universidad Fisicas, Ciencias de Departamento ieasprin tr u oeigrlsout rules modeling Our star. supergiant a like , Gibson ± 2 D,rsligi naibtccool- adiabatic an in resulting JD), 4 .Kroupa P. , 1 .Smith R. , M 3 ⊙ n .Assmann P. and , 1 uhalwrlmtfor limit lower a Such . > .Fellhauer M. , 5 M ⊙ ..mi se- main i.e. , ≈ 1 .K. B. , 500–600 1 cl). ABSTRACTS l. f aii,IP,Sa o´ o aps PBrazil. 2 SP S˜ao Campos, Jos´e INPE, dos paciaia, 1 s00()dxfrcro,01(4 o irgnand nitrogen for 0.12(14) oxygen. for carbon, 0.08(7) for dex 0.04(7) is cly h rlmnr bnac difference abundance preliminary directly Specif- the obtained ically, widths. equivalent those of measurements with through synthesis spectral measured abundances by have the we of elements, comparisons performed some For differential abundances. and elemental velocity microturbulence metallic- [Fe/H], gravity, parame- ity surface the present temperature, thus effective We ters oxygen. and carbon, re- as nitrogen to such spectral elements lines volatile the atomic of abundances and cover method bands have differential molecular We of the synthesis chemi- to star. of added and study planets also the between for connection essential cal is about which errors dex, with particularly 0.01 precision, with high elements a volatile such and chemical refractory and of parameters abundances derived photospheric have classical we Ob- results, the the Campanas main Las at the the Among spectrograph servatory. in MIKE telescope Magellan the 6.5m with spec- their collected had solar-type and second tra These metal-poor the moderately super-Earths. are around stars three and are there planet one Jupiter-type holds HD111232 first hot the star that a such the HD020794, compared with (ef- (standard) have star target we the metallicity).Therefore, of and gravity those surface to temperature, fective similar are parame- that photospheric stan- ters a predetermined to with compared star are star dard target equiva- the of chemical of widths measurements derive lent method, to this In differential order the technique. in using precision 000), high with 65 abundances = resolution high (R the spectra inspecting by be- planets the of connection and presence composition a chemical in- of the of in to not) anomalies study tween (or planets, existence without the the and on vestigate with emphasizes stars, metal-poor project present The nvriaed ˜oPuo S Brazil. USP S˜ao Paulo, de Universidade ii˜od srfıia nttt ainld Pesquisas de Nacional Astrof´ısica, Instituto Divis˜ao de VDNE BU LNTFORMATION PLANET NEW ABOUT STAR: EVIDENCES POOR METAL A OF ANALYSIS EALDDFEETA CHEMICAL DIFFERENTIAL DETAILED .G .C Carlos C. C. G. M. .Mel´endezJ. 1 .d .Milone C. de A. , 2 1 and , δ [E/H] Es- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes rtto fteei ne rprto n ilbe will and preparation else. under somewhere Inter- is published these 2006-2007. interval of the pretation It component in again. days persistent 16-64 up the became show that emphasized when dis- be 2012 practically to has and it 2011 Then, till corresponds appears 2000-2007. which interval cycle the solar to 23rd the the to of up minimum in- maximum from is no mainly component days nature in Identified 64 termittent Beyond observed. is series. days component occurrence 16-64 of CMEs range the the known in within all component new iden- of a to removal tify us permitted After com- investigation 27-day 11- this known. components, a well Also, are: is 1-year. studies ponent compo- 2.8-year, other periodic 6-year, and Known this year, series. in the identified when in nents as present well as is long identifica- how it and the component, any possible of level. becomes tion confidence WS compo- 95% of Spectral the Application within series. searched residual are the nents of (WS) spec- trum wavelet and pe- removal, by decomposition, components made known spectral riodic been series has of: analysis combination The a interval. a covering cycle from of 2000-2012, full years a obtained selection the for series the catalog CDAW continuous in the techniques consists time of It onset combination CMEs applied. Ejections new occurrence been of a has Mass pattern periodicities its Coronal either or of investigate terms in to (CMEs) order In aii,CP 1,12700 ˜oJsedsCmo-P Bras S˜ao([email protected]). Campos-SP, Jos´e 12227-010, dos 515, C.P. paciais, 1 oee yeprcllbais nti ak new a talk, this In libraries. empirical well by not patterns) covered abundance and tempera- metalicities (in tures, space libraries, parameter explore empirical to of particular in limitations overcome recent in to used years increasingly Theo- been have models. libraries synthesis ingre- retical main population the stellar of of one dients are spectra stellar of Libraries ii˜od srfıia nttt ainld Pesquisas de Nacional Astrof´ısica, Instituto Divis˜ao de .R Cecatto R. J. E IRR FTHEORETICAL OF LIBRARY NEW A PCRLAAYI FTECME THE OF ANALYSIS SPECTRAL TLA PCR O STELLAR FOR SPECTRA STELLAR OUAINAPPLICATIONS POPULATION CURNESERIES OCCURRENCE 1 .R .Guedes G. R. M. , .Coelho P. Pereira 1 1 1 n .S. E. and , ABSTRACTS Es- il omtebsso h V uoae classification automated VVV the algorithms of will basis which the types, different form of stars large light variable a for near-IR curves build high-quality, to well-defined, thus of is database different Project of the Templates purpose VVV of main the The representative study. be sample under classes to significant variability taken a stars for curves of tem- light (i.e., statisti- near-IR high-quality proper plate) of a face database of to significant construction had cally the we been problem in thus variability first has stellar the to first near-infrared, the dedicated the is survey VVV Since large entirely are ever classes. curves such light some good for that lacking way so extensive near-IR, sufficiently the have a in in classes observed variability been lim- many yet very not worse, is even curves and, light ited high-quality particular, of In number field. the research been has ill-explored near-IR relatively the a in variability stellar now, Until 1 1 is nvria eVlaaıo rnBean 11 Playa Breta˜na 1111, Valpara´ıso, Valpara´ıso, Gran Chile. Ancha, de Universidad cias, ([email protected]). Chile 2 Santiago, 782 Macul, 4860, Vicu˜na0436 Mackenna Av. Chile, Cat´olica de versidad ewe .07ad004,a ohsolar-scaled both at 0.0048, and and 0.0017 metalicities between Gyr, 14 Z stellar and of Myr 30 the modelling between cover the populations to which consists required spectra It space low-resolution parameter and presented. high is of library stellar theoretical ftelbaya ela oprsn oobservations to presented. comparisons be as well will as library the of D´ek´any .CnrrsRamos Contreras R. nvriaeCuer oSul. do Cruzeiro Universidade nttt eAto´sc,Fcla eF´ısica, Pontificia de Astrof´ısica, Facultad de Instituto eatmnod ´sc srnmı,Fcla eCien- de Astronom´ıa, Facultad F´ısica y de Departamento Navarrete Townsend α Pichara XESV MULTICONFIGURATION EXTENSIVE ehne opstos h characteristics The compositions. -enhanced ACLTOSO OSCILLATOR OF CALCULATIONS H V EPAE PROJECT TEMPLATES VVV THE 1 .Hajdu G. , 1 1 .Angeloni R. , .Eyheramendy S. , 1 .Borissova J. , epae Team. Templates 1 .Hempel M. , 1 .Catelan M. , 1 .Alonso-Garc´ıa J. , 2 .Navarro C. , 1 n h VVV the and , 1 .Jord´an A. , 1 .Gran F. , 2 K. , 1 1 1 I. , C. , B. , Uni- 151 - XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes u´ nm eBeo ie,Argentina. Aires, Tandil, Buenos 7000 Aut´onoma de 399, Pinto Argentina. Aires, Aires, Buenos 4 Buenos de de Pcia. Pcia. la de Centro oainlvlct itiuino apeof the sample obtain a of to distribution order velocity In rotational quantity. observable mental 1 152 h rjce oainlvelocity rotational projected The ae e oqesn 90L lt,Pi.d unsAires, Buenos de Pcia. Plata, 3 La 1900 Argentina. s/n, Bosque UNLP, del Paseo (CONICET), T´ecnicas Cient´ıficas y Investigaciones (acruzado@fcaglp. Argentina Aires, 2 La Buenos 1900 de unlp.edu.ar). s/n, Bosque del Pcia. Paseo (UNLP), Plata, Plata La de Nacional iee steeprclg ausi h rsn work. present the in xenon- values gf con- of empirical are the spectra as spectra, sidered observed synthetic with fitting Yuce stars by overabundant by (2011), obtained al lines et XeII for strengths astrophysical The with oscillator approach, obtained. empirically (LSF) values gf Fitting ob- the Square method theoretically Least (HF) the values Hartree-Fock and the gf adopting the by XeII compare tained, for We obtained have present lines. we we work results this He- preliminary In He-weak, some stars. of Ap spec- and spectrum HgMn, analyze the strong, to in intend observed we lines the mind, tral with in variations this possible With their time. as el- well chemical as some ements, of accurate abundance the the critical of atmospheres is determination it the stars, In peculiar chemically abundances. of uncer- stellar the cal- of of the in culation effects values gf the obtaining with estimate associated ad- tainties to In aim interest. we astrophysical of dition, strengths lines oscillator spectral obtain of to is (gf) work this of goal The s ooti hsdsrbto ne h assumption the under distribution this obtain to ism formal- a developed M¨unch (1950) & Chandrasekhar PLCTO OMI–EUNEFIELD MAIN–SEQUENCE TO APPLICATION nttt eFıiad rooSc,UiesddNcoa d Nacional Universidad Seco, Arroyo F´ısica de de Instituto autdd inisAtnoia Geof´ısicas, Aston´omicas Universi y Ciencias de Facultad TEGH SFLFRASTROPHYSICS FOR USEFUL STRENGTHS nttt eAto´sc eL lt,CneoNcoa de Nacional Consejo Plata, La Astrof´ısica de de Instituto OIE,A.Rvdva11 C03A) Ciudad (C1033AAJ), 1917 Rivadavia Av. CONICET, E EHDT IETNL THE DISENTANGLE TO METHOD NEW A .Cruzado A. OAINLVLCTE FSTARS: OF VELOCITIES ROTATIONAL .Cur´eM. 1 .F Rial F. D. , 1,2 APPLICATIONS .H iRocco Di H. O. , Marchiano Christen STARS 2 .Cassetti J. , 4 1 v 3,4 sin n .E. P. and , 3 i n A. and , safunda- a is v sin ABSTRACTS dad i el , Valpara´ıso, Chile. a auae,Uiesddd unsArs Argentina. Aires, 4 Buenos de Universidad 3 Naturales, y tas 2 ([email protected]). Chile 1 rKnaai itiuinfunctions. distribution Kaniadakis or is stars field non–Maxwellian main–sequence velocity of the that function proving distribution (2009) al. et Carvalho from n aao fproi n rnin aibe in variables transient and periodic of catalog computa- database a massive variability general and a a talk, of produce details to my effort the In tional on expound is products. will data data I homo- these high-level south- requires and of exploration the geneous global potential and its scientific bulge and The the manifold, in disk. objects ern hundreds of for millions near-infrared of the in time- long-baseline photometry deep, series providing ESO is (VVV) Survey Lactea Via Public the in Variables VISTA The fterttoa eoiisfo rjce velocities projected from ( velocities (CDF) rotational We function the distribution of on cumulative formalism. the based (1950) obtain M¨unch velocities, & rotational Chandrasekhar of distribution the criteria. but convergence problem, no inverse has of method kind distri- this this the of disentangle function to bution (1974) Lucy was by method iterative developed alternative an An of integral. derivative Abel’s intrinsic the an to to associated due problem but applied numerical usually distributed, not is uniformly method are this axes rotational that hnapidto applied confidence. high When very with recovers CDF it the distributions theoretical to applied When the gives veloc- step rotational ities. one of just function in distribution and cumulative robust is method The main- 12.500 about of stars. sample field a sequence with distri- b) velocity and rotational bution the for dis- Maxwellian functions theoretical tribution a) using tested is the method simulations Through axes. rotational distributed v .Dekany I. nttt eFıiayAtoo´a nvria eValpara F´ısica Astronom´ıa, de de y Universidad Instituto eatmnod ae´tcs autdd inisExac- Ciencias de Matem´aticas, Facultad de Departamento nvria ainld eea amet,Argentina. Sarmiento, General de Nacional Universidad nttt eEtdıtc,PnicaUiesddCat´oli Universidad Estad´ıstica, Pontificia de Instituto sin eew rsn e ehdt disentangle to method new a present we Here u anrslsare: results main Our H EEA AAO FVISTA OF CATALOG GENERAL THE i ne h tnadasmto funiform of assumption standard the under ) AIBE NTEVALACTEA VIA THE IN VARIABLES 1 .Ple,D int,adM Catelan M. and Minniti, D. Pullen, J. , n r etrdsrbdb Tsallis by described better are and real aa ercvrteresults the recover we data, ade ca ´ıso, XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes urn ttso h rjc,adwl ocueby conclude will and results. project, selected the the highlighting procedure, of the the database, status the of current of steps uses possible main and the characteristics discuss community. will VVV pulsation the I by stellar conducted from ba- microlensing, studies the to specific as various serve for may sis a which of database form on-line the duly simple in to products is project data this science-ready of provide goal The VISTA the System. Flow by Data provided photometry using bulge, the a ,adLnsy3aelctdi einta we that region a in located Parisi are Lind- 3 by 1, Lindsay HW and described particular 2, In say as (2011). Piatti spread and some (2009) with Tautvaisiene & Pagel (1998), by relation age-metallicity the to)aeitreit-g lses ihae be- ages with fluctu- field clusters, tween a intermediate-age these as are that identified ation) confirm 34, HW results (except The clusters tests. star and performing artificial Completeness obtained were CMDs. uncertainties photometric field control and the cluster comparing Mem- determined were ones. probabilities observed bership the reproduce synthetic best the that identify which CMDs to fitting, statistics likelihood isochrone the self- of uses a means in by derived profile way were consistent King parameters other applying The out fitting. telescope, carried SOAR were parameters 4.1m from the V built reaching with were obtained profiles density B-V images radial (V, and diagrams where first the CMDs) colour-magnitude 3, for studied Optical Lindsay are 2 and Lindsay time. 1, and 2, HW 34, Lindsay HW 3, Cloud 1, 40, HW AM Small HW the are: 34, clusters of HW studied context cluster, The the each in evolution. for them profile place density and central derivation and the core radius are reddening, modulus, work distance this metallicity, age, of of goals main The Gyr. 1 nbigiseto falrepro covering period large a of dy- galaxy, inspection and dwarf enabling neighbouring chemical are this the of Cloud evolution study namical Magellanic to Small pieces the fundamental in clusters Stellar Chile. .Dias B. AAEESFRSCCUTR FROM CLUSTERS SMC FOR PARAMETERS nttt eAtosc,PnicaUiesddCtlc d Catolica Universidad Pontificia Astrofisica, de Instituto ∼ 1,2 and 1 .Kerber L. , .Ortolani S. ∼ 3 h eemnto fstructural of determination The 23. ∼ M MODELING CMD y.Termtliiisfollow metallicities Their Gyr. 5 1,3 5 n .Balbinot E. and , .Barbuy B. , 1 .Santiago B. , 4 ∼ ABSTRACTS 10 4 , e tti setea auaa oVVV. sub- do para saturadas VVV estrelas e as stituir 2MASS combinar podemos Al´emdisso, importˆancia. pr´e- a maior onde ´e de jovens, sequˆencia o principal abertos tra- ser aglomerados queremos com provou que balhar este vez uma brilhantes, adequado, precisos mais m´etodo mais menos estrelas resultados as Emb- obtenha para t´ecnicas. fracas algoritmo outras mais o detect´aveis com magnitude ora as uma que de do mais estrelas para aldWs ao Bsdo ae yDa tal. et Dias by 1311.4579). paper arXiv: on accepted; (Based A&A, 2013, Halo. West called o aspeio aaa srlsmnsbrilhantes menos estrelas as (J para da- precisos gerar de mais capaz dos foi algoritmo o fato tom´etrica, fo- de profundidade precis˜ao usu´ario e mantendo o com intera¸c˜ao a ´e evitar algoritmo caracter´ıstica do ex- cipal L´actea” Via a the in para Variables cat´alogo algoritmo fotom´etricos do um dados tra¸c˜ao apresenta de trabalho Este 5 4 3 2 1 RPRMTOSO R-ANSEQUENCE PRE-MAIN OF MOTIONS PROPER 1 ansqec tr n enn h srmtyfor astrometry the refining pre- and more stars including sequence by improve- database main an existing represents an star- of work nearby ment This proper in determine stars regions. to sequence forming is pre-main work The of this motions strategy. of point objective convergent velo- main radial the and using motion data proper city from inferred members be group moving can be- to they distances which Individual to stars long. mov- young detect of In to structures group us formation. ing allow star motions of proper stages context, important early this an the is discuss stars to young tool of study kinematic The .B Galli B. A. .C .Ferreira S. C. A. nvriaeFdrld i rned u,Brazil. Sul, do Italy. Padova, Grande Universit´a di Rio do Federal Universidade Brazil. LATO-DCET-UESC, Chile. ESO, Brazil. S˜ao Paulo, de Universidade IAG, UFRGS. S-ITN IEIEFRVVV-ESO: FOR PIPELINE PSF-FITTING A ∼ > 6 H 16, H TRCUTRPSI 24 PISMIS CLUSTER STAR THE .A .Dias G. A. R. 1 ∼ > .F eCampion Le F. J. , 55eH e 15,5 1 .Teixeira R. , STARS ∼ > 1 n .Bonatto C. and 5 confi´avel fotometria e 15) VV oEO prin- A ESO. do (VVV) 1 2 .Ducourant C. , n .Fidˆencio M. and , 1 “VISTA 2 P. , 153 1 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ain r oae o ls oteCped( com- Cepheid the the to of close too most located However, are panions models. evolution constrain pulsation and and distance, and mass sys- esti- evolution, the binary and mate age in their investigate are can we Cepheids tems, when Baade-Wesselink Finally, bias the also method. through can estimate presence distance Their the Cepheid. atmo- pulsating the the of in sphere waves possi- shock loss, by mass generated ongoing proba- bly or were past present CSEs through These the formed bly Cepheids. to of access rate give loss mass they partic- as is CSEs important com- the ularly study of the characterization so and The and (CSEs) panions. stars, envelopes these circumstellar of their environment close the Group. Local the in indicator pri- distance as used mary are Cepheids classical because important star. particularly the are to measurements distance distance and Independent the angular provide its can mode, variation pulsation linear the probe to us lows circum- close a environment. the in stellar probe distances a and measure opti- is way, to pseudo-geometric this tool at unique Cepheids, and resolution For powerful giv- milli-arcsecond wavelengths. technique to cal/infrared only access the ing is interferometry Optical s ogbsln nefrmtyo pruemask- aperture to is or ing. systems interferometry such long-baseline resolve spatially use telescope. to class way 10-meter only a The with observed be to mas) ofe ia,Uiesdd eSa al,Bai (and- Brasil Paulo, S˜ao 2 de [email protected]). [email protected], Universidade mosf´ericas, them 1 compare dis- and catalogs. we results astrometric Here our published with of literature. accuracy the the from cuss data Observatory, use Bordeaux also the and Observa- and Moraes SP) Abrah˜ao (Valinhos, de the tory at located motions meridian circles CCD the proper the with stellar in performed observations the information from calculate motion We proper literature. poor with stars 154 IMTR,DSACS CIRCUMSTELLAR DISTANCES, DIAMETERS, bevtied odax France. Bordeaux, de Observatoire nttt eAtooi,Go´sc ieca At- Ciˆencias e Geof´ısica Astronomia, de Instituto nefrmtyas ffr h osblt oprobe to possibility the offers also Interferometry al- diameter angular mean measured the While .Gallenne A. OGBSLN INTERFEROMETRY: LONG-BASELINE LSIA EHISFROM CEPHEIDS CLASSICAL NEOE N BINARITY AND ENVELOPES 1 .Kervella P. , .Breitfelder J. 2 .M´erand A. , 2,3 3 and , ∼ 1-40 ABSTRACTS ail 90,Snig 9 Chile. 19, Santiago F-92195 19001, Casilla Janssen, Jules 3 Place France. 5 Meudon, Diderot, Paris Universit´e (agallenne@astro-udec 2 Concepci´on, Chile 160-C, Casilla 1 S˜ao Lu´ıs, Brasil. 2 Maranh˜ao, ([email protected] S˜ao Lu´ıs, Brasil 1 Ps r yia fteobtlmto time-scale 10 motion within orbital orbiting the matter of for typical are (HF oscilla- QPOs) QPOs high-frequency quasi-periodic Twin-peak spectra as (QPOs). power such tions frequencies, show power given star of at fractions a neutron enhanced several either a by characterized or with hole (LMXBs) black binaries X-ray Low-mass edo h opc bet wnpa FQO are frequency central QPOs HF their by gravitational Twin-peak characterized strong object. compact the clumps the of with accreting field interacting by released matter energy of could the modulations from such Thus, arise object). compact the bet( object qaeapiue( amplitude square o atraon 10 a around matter for h bevdbhvo fteeeg ( energy the of for behavior account chang- may observed the the shape (ISCO) potential orbit Schwarzschild the circular ing to stable approaching orbits most or- for inner given that on the highlight depends We for matter bit. shape of potential clump Schwarzschild the the on tides by loaded yteti-ekH QPOs. HF twin-peak the by hr ∆ where otdsi h ne ato h crto ik It disk. 2 accretion a the around of disk be part inner to survive the turns can in that matter tides of to clumps maximum of the radius the estimate allowed of we source potential root Schwarzschild as force ( tidal work energy strong the the highlight by We done the LMXBs. of several behavior in observed characteristic the on vestigate RMTERAPIUEADCOHERENCE AND AMPLITUDE THEIR FROM .German`aC. SILTOSI -A IAIS CLUES BINARIES: X-RAY IN OSCILLATIONS nvria eCnec´n eatmnod Astronom´ıa, de Concepci´on, Departamento de Universidad uoenSuhr bevtr,Aos eC´ordova 3107, de Alonso Observatory, Southern European EI,Osraor ePrs NSUR80,UPMC, 8109, UMR CNRS Paris, de Observatoire LESIA, eatmnod ´sc,IsiuoFdrld Maranh˜ao, do Federal Instituto F´ısica, de Departamento eatmnod ´sc,Uiesdd eea do Federal Universidade F´ısica, de Departamento r rms WNPA QUASI-PERIODIC TWIN-PEAK ν g = stewdho h ek eew in- we Here peak. the of width the is eesdb P.B en fthe of means By QPO. a by released ) 1 R .Casana R. , GM/c ∼ M 0mfrmte na accretion an in matter for m 40 .R Gomes R. A. rms ⊙ 2 eto trand star neutron stegaiainlrdu of radius gravitational the is n coherence and ) M 1 .M eriaJr Ferreira M. M. , ⊙ lc oe h work The hole. black r g 2 rmtecompact the from rms ν R Q otmean root , ∼ = carried ) 1 5 m 150 ν/ and , .cl). rms ∆ ). ν , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes NTEOII FTEWN VARIABILITY WIND THE OF ORIGIN THE ON 1 tde fGlci tutr sn hs variables. only these provides using VVV the Via structure II for As the Galactic crucial and is in of Survey Variables studies I Public Vista ESO Type (VVV) the Lactea in between found distinction Cepheids the Making 2 ([email protected]). Santiago Macul, Chile 782-0436 Vicu˜na 4860, Mackenna Av. Chile, one ih-ongtvrain nisH pro- its exhibits in Cygni variations night-to-night 55 nounced supergiant B-type early The sesti rbe,w aecmae h VVV the compared Templates have VVV we To and problem, made. unambiguously this be whether assess can obvious distinction immediately a not such is it however, IR, light-curve near-IR on based be properties. to has distinction ehisfudi h V aawl rvd ac- bump provide the stars. will these data of for VVV parameters curves stellar the De- curate light in curves. the found light Cepheids of near-IR fea- modeling the bump in tailed the appears as also data, ture VVV using identified easily accu- of degree high a able racy. with be variables will such Survey classify VVV to the for schemes development classification under alone, automatic I feature the simple Type that this with suggesting by confused out sorted be half are per- could limit, Cepheids that 50 this variables above As lie the limit variables of Cepheids. II upper Type I the an Type of is cent of amplitudes there the range, for period of most Cepheid over example, the the For for enough classification. different using of be purposes of Cepheids to found parameters II were Fourier Type types these 215 The and I decomposition. Fourier Type 213 of ties RPRISO USTN AIBE IN VARIABLES PULSATING OF PROPERTIES .Hajdu G. h ik a ilnimNces atao Chile. Santiago, Nucleus, Millennium Way Milky The PIA/ERIFAE LIGHT-CURVE OPTICAL/NEAR-INFRARED nttt eAto´sc,PnicaUiesddCat´oli Universidad Astrof´ısica, Pontificia de Instituto Tomi´c .Haucke M. eas fterrdcdapiue ntenear- the in amplitudes reduced their of Because ehv lofudta upCped a be can Cepheids bump that found also have We H EHI NTBLT STRIP INSTABILITY CEPHEID THE 2 .S Cidale S. L. , 1,2 .D´ek´any I. , 1 .Kraus M. , Calder´on Espinoza F5 CYG 55 OF K 1 Cur´e .H Nickeler H. D. , K S 1,2 bn ih-uv proper- light-curve -band 2 S .Catelan M. , .O .Venero J. O. R. , bn ih uvs this curves, light -band 3 1 1,2 2 n M. and , α n D. and , P-Cygni 1 S. , ade ca ABSTRACTS , h erCmcmr,i -adYbns This the Y-bands. to and complementary and H- is program (Chile) in monitoring Observatory camera, tele- RetroCam Campanas Swope the the Las using at 2009–2011, scope and years clusters the as star tween known photometric young regions, galactic near-infrared star-forming 39 a of performed monitoring have We .Soto M. oa Lopes Roman is nvria eValpara´ıso, Chile. de Universidad cias, 3 Republic. Ondˇrejov, Czech 2 ([email protected]). Argentina, Plata La CONICET-UNLP, Astrof´ısica Plata, de La Instituto 1 .JqeArancibia Jaque M. 04 on htteHeI (Precision the that vari- al. found of 2014) et 301, cycle Kraus Symposium IAU a hand, Proceedings, during other Asteroseismology three the of On mass factor ability. the a by of rate changes wind the loss suggest for parameters values The stellar cyclic and days. a 17 have about to of seems behaviour intensity) and (shape pattern 1) lhuhw eental ofida exact an find to able H not the from were period we Although 488- 323, 512). A&A 1997, code Herrero The FASTWIND & Puls (Santolaya-Rey, using parameters. modeled wind were and observations stellar the the analyze in to spec- variations of order of Observatory in sample the Republic), a Ondˇrejov at (Czech studied taken we observations, work this troscopic In stel- variable wind. strong lar a to related probably profile, line fteoclainmodes. oscillation coupling the the to of attributed be could The loss post- mass a modes. variable in pulsation multiperiodic be with could phase Cygni RSG 55 that 433, conclude MNRAS, we 2013, 1246), Meynet, & Georgy supergiant blue (Saio, the region to back prop- evolving those pulsation su- than different erties red have the (RSG) to stage sequence pergiant main the the from As evolving variations. stars observed a the only that for the responsible be found agent not could we pulsation parameters of anal- mode theoretical the gravitational From our be of could period. which ysis longer period, a day over 1.09 superimposed a presents line tion I FSAS AL EUT N NEW AND RESULTS EARLY STARS: OF NIP autdd inisAto´mcsyGo´cs NP and Geof´ıcas, UNLP, Astron´omicas y Ciencias de Facultad eatmnod ´sc eerlgı,Fcla eCien- de Meteorolog´ıa, Facultad F´ısica y de Departamento srnmc´ utv kdmevˇed Akademie ´ustav, Astronomick´y 5 .Ferrero G. , CISN BINARIES ECLIPSING 2 .Tre Robledo Torres S. , .Frae Lajus Fernadez E. α 1 iepol aitos h same the variations, profile line 6 .H Barba H. R. , .I Arias I. J. , λ 68poopei absorp- photospheric 6678 2 I fStars of NIP 2 .Gamen R. , 2 7 .Gunthardt G. , .Morrell N. , ekeRepubliky, Cesk´e ˇ 7 Vista and , be- , 3 A. , 155 4 , , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ht wrsaeteedsaeo l ansequence main 8 all than of massive state less end stars the are dwarfs White 7 6 5 4 3 2 1 L´actea Via the in Variables 156 s ore bevdin observed sources est gsotie nteK ihteVSAtlsoein im- telescope VISTA of of the set framework with the small Ks the a variability, in obtained of included ages analysis We can- the them to binaries. also among eclipsing massive tens stars, for of variable didates discovery for the candidates with photomet- of work, program this of this monitoring analysis In ric preliminary a stars. discov- present binary of we goal eclipsing main massive the ering with and regions, clusters star-forming such of variability photometric of census in rlmnr nlsso h ih-uvso hs bi- a these present of We light-curves O2 naries. the of components. of type its analysis spectral of a preliminary with one star as them, rare If*/WN6, classified of a one been has and 58, have MTT stars, stars O-type The as spectroscopically young 3603. massive NGC of the discovering in cluster binaries infrared eclipsing the massive announce four we special, In DSadteeoetettlvlm ilb (2 be will than volume farther total times the 2.5 therefore dwarfs and white SDSS see com- should be we will J-PAS while (5 20.5, plete of below most magnitude SDSS; have a dwarfs than white and deeper confirmed First go spectroscopically new will SDSS many dwarfs. It discover white dwarfs. to as us white allow up will end J-PAS will foremost, stars all of 46tmslre.B ento vr object every in definition while By observed, spectroscopically larger. be will times J-PAS in 14.6 = 1 - .Kanaan A. HT WR TR NTEJA SURVEY JPAS THE IN STARS DWARF WHITE .B Pereira B. C. V´azquez Rami´o CGP nvria ainld aPaa Argentina. Plata, Argentina. la IALP-CONICET, de Nacional Universidad FCAGLP, USA. STScI, Argentina. Cordoba, de Observatorio Chile. Observatory, Campanas Chile. Las Serena, La de Universidad Argentina. ICATE-CONICET, Villegas .Marcolino W. VVV EETO ASDTRIAIN- DETERMINATION MASS - DETECTION EPRTR DETERMINATION TEMPERATURE σ h i fti apini oproma perform to is campaign this of aim The . 3 eetos ont 25i ahfitr So filter. each in 22.5 to down detections) .R Gon¸calves R. D. , 1 .Schmitz T. , 3 .Bre Fernandes Borges M. , PSCollaboration JPAS 4 6 .Ribeiro T. , VVV .Mart´ınez-Delgado D. , uvy(int ta.2010). al. et (Minniti survey M 1 I fStars of NIP .J Alfaro J. E. , ⊙ hc en ht98% that means which , 4 5 .Lorenz-Martins S. , ( .Ederoclite A. , VVV ,a h bright- the as ), 3 .Aparicio T. , r saturated are 2 .Daflon S. , 6 n the and , 6 H. , ABSTRACTS 4 . , 5 3 3 , 401 siaeta h hnrska ii in- 86, limit D, 2 Chandrasekhar to Rev. the creases that Phys. estimate (2012, 042001) B. Mukhopadhyay & U. 6 5 Brazil. Janeiro. 4 Brazil. Brazil. - SC 3 Florian´opolis - - 88040900 2 - CP476 Catarina. 1 AJ,24 )etmt ny12 ht wrshave dwarfs 1 white 2013 above 1-2% masses al. only estimate et et 5) Kleinman 204, Kepler 1315), (ApJS, 375, luminous). (MNRAS, 2007 (less common) al. radius (less smaller stars have massive of and be- product rare, final are the They ing merger. or progen- accretion progeni- SNIa through probably the the itors are of dwarfs but white metallicity Massive 63), the tor. 47, on ARA&A, depend 2009 does S. limit (Smartt explode SNII will as masses 676, higher 355). ApJ, with 693, stars 2008, ApJ, sequences 2009, Main al. Koester & et Bolte Kalirai Williams, 594; Weidemann 647; (e.g. 363, end A&A, mass final 2000 high vs. the initial at the relation of mass determination pro- the in tand Massive gap objects, a duce rare overshoot. intrinsically are core dwarfs and white loss mass progenitor, assas .. ansqec tr ihmse be- masses intermediate fi- with (8 and stars the low sequence low- Galaxy, main all our i.e., of for stars, in mass evolution born endpoint of stars stages evolutionary all nal of the 95% are nearly dwarfs White etpoeiosi h ag 2 sug- range 2003fg type the SN Peculiar in 2009dc, progenitors SN gigagauss. gest 2007if, SN a 2006gz, to SN kilogauss Ia ranging few in, a As freezes field from dwarf. magnetic white wind. the down, a rapidly stellar cool leaving star they ceases, a the burning exposed, in and is envelope cools shell H-rich growth burning the core the When between of race loss a and are burning helium ter o3000 mn u ol r h td fthe of study distri- the mass the are bution. and goals function luminosity our dwarf white Among 20,000 approximately 300,000. from more to dwarfs much total white the be of increase also to number expect will We taken, SDSS. sample than spectra dwarf complete their white had our objects so chosen only SDSS etod suisd iiadlCso eArag´on. Spain. de Cosmos del Fisica de Estudios de Centro nvriaeFdrld egp.Brazil. Sergipe. de Federal Universidade Andaluc´ıa. Spain. Astrof´ısica de de Instituto bevtoi ainl iitei eCˆni Tecnolo Ciˆencia e Minist´erio de Observat´orio Nacional, bevtoi oVlno nvriaeFdrld i de Rio do Federal Universidade Valongo, Observat´orio do eatmnod ´sc,Uiesdd eea eSanta de Federal Universidade F´ısica, de Departamento . 5 ± 1 . . 3 5) HT WR STARS DWARF WHITE − M M 2 . ⊙ 6 ⊙ eedn nmtliiyo the of metallicity on depending , .O Kepler O. S. h nlsae feouinaf- evolution of stages final The . M ⊙ o xrml ihmagnetic high extremely for . 4 1 − 2 . 8 M ⊙ n Das and , gia. XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes hsc,adtehsoyo tla formation. density stellar high of of history study the the the around and for physics, and tools clusters valuable in are stars func- Sun dwarf luminosity white the of through tion with properties together mea- envelope and to and seismology, determina- used interior mass are their stars the dwarf sure in white magnetic yet Pulsating of included effects tions. not the are but problem (A&A, solved, fields the 2013 been 1309.0886) and finally arXiv L19) the 7; has 557, 531, with A&A, (A&A, 13; Only 2011 552, al. 2013). et Trem-blay of al. ApJ, calculations convection 2011, et (3D) tridimensional al. et Kleinman et Bergeron Tremblay 128; 253; 730, 367, (e.g. ApJ, DAs ap- 1991, for increases al. 000K gravity) 13 surface below the parently by measured mass average (as with the unidimensinal shows spectra (MLT) lenght-theory using the mixing calculated fitting MNRAS, atmospheres from 2013, model hydrogen- measured the of (DA) al. distributions rich et mass The Kepler 2934). 5, 439, al. 204, et (Kleinman ApJS, ones 2013, massive white the corre- of including varieties a dwarfs, rare with relatively (SDSS), in increase Survey sponding with Sky dwarfs Digital discov- white Sloan inher- We spectroscopic the 000 or 20 progenitors. around zone, Ap/Bp ered convection massive from surface ited own through developed star’s likely are the fields magnetic determine these over- ultimately if an and causing gravity, WDs, surface en- in estimated fields broadening magnetic line propose the We mag- hance high-field dwarfs. degen- of white progenitors double netic the 2012, proposes are example, mergers al. for Garc´ıa-Berroerate et 25, 69). 749, 744, et ApJ, I. (ApJ, Hachisu 2012 to according al. it, increase accre- also by could induced tion rotation differential but stars, field 1 huhteelsscnanmlino ie,vr few very lines, of Al- million spectrum. contain each lists in these appear though absorp- should the that of lines parameters tion atomic these lists, the generate line contain that molecular which galaxies. and codes atomic of the are for populations spectra synthetic inputs stellar the the of of One stars study observed the new to of de- for parameters from used astronomy, atomic termining in extensively applications are different many spectra stellar Synthetic nvriaeFdrld i rned u,Brazil. Sul, do Grande Rio do Federal Universidade IEIETFCTO NTESUN’S THE IN IDENTIFICATION LINE .R Kitamura R. J. SPECTRUM 1 n .P Martins P. L. and 1 ABSTRACTS apsLbrae u ava un,88 iedd,S˜ao ([email protected]). Liberdade, Brasil 868, Galv˜aoPaulo, Bueno, Rua Liberdade, Campus 1 nteaoi aaees sfreape ie in lines errors example, wrong. is large for wavelength central with as the lines parameters, models. which identify atomic the to the in try in missing also still identify will to lines We try the to Sun quantify the synthetic and will of the we spectrum compare observed to project the and strategy this reproduce careful In cannot a develop stars. still observed we of one reasons spectrum is main This the star, lines. many studied of misses most and spectra stars. closest synthetic the our in the that, appear Sun, Besides that the lines for the 200%. Even all as know the not large in do errors as we the be lines can The many parameters for laboratory. that in is measured consequence actually were them of l,20,AA 5,29 o h asitra of interval mass the for 269) 456, M 0.15-3.8 et A&A, (Landin 2006, code ATON2.4 al., by generated obser- were Theoretical and tracks theoretical diagrams. in Hertzsprung-Russel isochrones vational and tracks ary evolution- sequence pre-main non-gray presented We o agrmse,btfrM for way but same masses, larger the for roughly behave transformations with both obtained tracks The metallicity. increasing with eune osalrtmeaue o ihrV higher (or main temperatures in smaller shift, to known well sequence, the show diagrams Russel Hertzsprung- observational (CMD). and theoretical diagrams in Tracks their color-magnitude to in isochrones we counterparts and systems, tracks photometric & theoretical (VadenBerg 778) converted BVRI 126, and AJ, 231) 2003, et 333, Clem, (Bessel A&A, 1998, UBVRIJHKL al. in corrections and relations bolometric color-temperature using By +0.37. and sa2 y l ytm ossigo w aeB- late two of consisting M system, 2.9 of old stars Myr type 22 a is omtosrtr B return formations u famlil ytmadayugcluster. young a and system sta- multiple evolutionary in a the isochrones of the investigate tus and to in tracks used incompleteness were our opacity Finally, CMD the UV. to and due blue and be stars can cool it for especially theory and observations .R Landin R. N. ´ ce eAstrof´ısicaN´ucleo d Te´orica, de Cruzeiro Universidade R-ANSQEC EVOLUTIONARY SEQUENCE PRE-MAIN OO-ANTD DIAGRAMS COLOR-MAGNITUDE RCSADIOHOE IN ISOCHRONES AND TRACKS ⊙ n ealcte f[Fe/H]= of metallicities and 1,3 .T .Mendes S. T. L. , ⊙ − ahada07 M 0.79 a and each oosi iareetwith disagreement in colors V Vaz 3 < . M 0.8 2,3 ⊙ n .P R. P. L. and , eslstrans- Bessel’s ⊙ − pre-main .4 0.0 0.24, η Sul, o Mus − 157 I) XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes enaeo tr’cutri . y,wa si agree- in works. is other what Myr, with 3.5 ment is cluster stars’ of age mean al,Rad a˜o12,Cdd Universit´aria, 05508-09 Brazil. Cidade SP, S˜ Mat˜aoS˜ao 1226, Paulo, do de Rua Universidade Paulo, da Atmosf´ericas Ciˆencias e Geof´ısica 3 USA. 85719, S˜ao Crist´ov˜ao, SE, 49100-000, 2 s/n, ([email protected]). Rondon Brazil Marechal Av. 1 (lpv Brasil Gerais, Minas Horizonte, @fisica.ufmg.br). Belo 31270-901, CEP Gerais, 3 Minas Horizonte, ([email protected]). Belo Brasil 31270-901, CEP Gerais, Minas 2 (nlandin@uf Brasil br). Gerais, Minas Florestal, 30690-000, CEP 1 stars 0.1-0.6M 2264 range NGC the in that mainly, estimated masses, have We star. sequence 158 observations. pei ie ln ihsrn msinlnsfrom lines emission strong Photo- H with the Technology Telescope. along SOAR lines New 4.1-m spheric 3.6-m the the and Telescope with its of acquired medium-resolution characterization spectra optical binary. the from Be/X-ray present counterpart a we optical be work to this assumed In pho- X-ray was near-infrared its it and on tometry, optical Based from and Cloud. properties, Magellanic Large located the source in X-ray an is J054134.7-682550 XMMU oipoetecaatrzto ftesse from system the of XMM- characterization aims the which improve Addi- program to binary. ongoing Be/X-ray an present a conclusive we indeed now tionally, or is is dense system it a the Thus, with that star disk. Be circumstellar a large is counterpart optical the NSAC FPEIEIOHOA AGES: ISOCHRONAL PRECISE OF SEARCH IN OT AL N AEINAPPROACH BAYESIAN AND CARLO MONTE et.d nehraEeroia nvriaeFdrlde Federal Eletrˆonica, Universidade Engenharia de Depto. eatmnod ´sc,Uiesdd eea eSergipe, de Federal F´ısica, Universidade de Departamento et.d ´sc,Uiesdd eea eMnsGerais, Minas de Federal F´ısica, Universidade de Depto. nvriaeFdrld ics,Cmu F Florestal, UFV Campus Vi¸cosa, de Federal Universidade .Lorenzo-Oliveira D. eatmnod srnma nttt eAstronomia, de Instituto Astronomia, de Departamento ainlOtclAtooyOsraoy usn AZ Tucson, Observatory, Astronomy Optical National RPRISO H IHMS X-RAY MASS HIGH THE OF PROPERTIES .Lpsd Oliveira de Lopes R. α NELN PIA N X-RAY AND OPTICAL UNVEILING Newton H , IAYXM J054134.7-682550 XMMU BINARY β n eea rniin fio hwthat show iron of transitions several and wf/A n S/XEX-ray ASM/RXTE and Swift/BAT , 1 n .F ot eMello de Porto F. G. and 1 n .M Placco M. V. and ⊙ n the and 2,3 ABSTRACTS 1 ao v. 0 aer,Ldiad er noi,4,CP 08-9,Rio 20080-090, ([email protected]). CEP: Brazil 43, Janeiro, Antonio, de Pedro do Ladeira Janeiro, 1 loe st n htulk nteotcl where optical, the in unlike that find spec- data to X-ray Swift/UVOT us soft Simultaneous allowed and of hard components. consists both tral group with a third sources where The those i.e. region emission, region. a spectral X-ray colliding-wind in X-ray produce soft arises shocks low-velocity single, likely a which with component, composed sources is accretion- group those second an of The from which layer. coming boundary component, probably disk hard as absorbed identify with we highly sources distinct those single, contains three group a into first naturally The fall ther- groups. and with three consistent emission during symbi- are mal spectra 50 programs X-ray than fill-in Their more Swift years. detections of using X-ray survey stars new a otic 14 of result The known the de- previously sources. were will X-ray not I be were to white that 14 population. of symbiotics Swift/XRT X-ray the dwarf with soft detection thought a the were scribe mainly giant red be a a to from which accretes in dwarf systems white binary symbiotic recently, Until in oenn h vlto faglrmomentum stars. angular solar-type of in might evolution rela- activity the firmer governing and of tions establishment age the of towards calibrations contribute Such solar-type for stars. calibrations age robust the of enable construction ob- will future applied relationships for age-activity-rotation when to useful moreover, very metallic- and, be follow-ups and will servational masses sample covering ages, This ages subgiant of ities. isochronal and domain MS extensive accurate of an very sample a with derive stars to we able determinations, be these will From inference. and and Bayesian simulations ZAMS) Carlo (at Monte radius through gravity mass, surface as fundamen- such and parameters age tal isochronal proba- their of based calculate distributions ages we bility this, stellar For reliable statistics. most solid on evolutionary the are and sur- which spectroscopic isochrones veys, several in of identify, to grid aimed tracks We dense systems. a exoplanetary of build evolution evolution the and as structure well as Galactic important the is stars understand FGK to for ages accurate Obtaining bevtoi oVlno nvriaeFdrld i de Rio do Federal Universidade Valongo, Observat´orio do .J .Luna M. J. G. YBOI TR NXRY N UV AND X-RAYS IN STARS SYMBIOTIC Nelson 1 .L Sokoloski L. J. , 4 n .E Nu˜nez E. N. and , 2 .Mukai K. , 5 3 T. , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ercppln Muoe l 2013). al. et (Mauro pipeline metric as- disk. a usually through is accretion which with flickering, sociated UV stronger tend have emission X-ray to harder with shows stars photometry symbiotic UV that the X- components, two stars. spectral the ray symbiotic of UV interpretation of physical detectable property our Supporting common seen, a not is are flickering ac- typically the disk from variations cretion brightness stochastic rapid, 3 2 1 ob- VVV-SkZ and automatic extracted 2010) new are the data al. with The GeMS/GSAOI. et with (Minniti tained the Survey in Variables Lactea VISTA the Globular Via from Galactic data several using to clusters and using applied 1 method magnitude Triplet Liller Ks Calcium of the Branch from the results of Horizontal some study the the of of results structure preliminary the show We pacio. 5 4 3 2 1 amrlnssmlaeul.Bcueo chemical of several presence of of the Because matching and stratification the simultaneously. and equilibria lines ionization FeII/III Balmer via and way OI/II iterative of (He- an deter- in were Centauri parameters mined a Atmospheric star synthesis. spec- non-LTE tral Bp state-of-the-art of the means high-S/N by variable) of and high-resolution spectrum a UVES analyzed have We r o ace ihasadr oe atmosphere. model standard a with matched not are O-T OF NON-LTE .L Maza L. N. TOPEI TAIIAINSGSIN SIGNS STRATIFICATION ATMOSPHERIC eiiOsraoy aai USA. Hawaii, Chile. Observatory, Antofagasta, Gemini Norte, del Catolica Universidad Chile. Concepcion, de Universidad nvriyo Minnesota. of University USRA. & NASA/GSFC CONICET. Espacio, University. F´ısica del Columbia y Astronomia de Instituto HTMTI NLSSO GALACTIC OF ANALYSIS PHOTOMETRIC .Mauro F. nttt eCeca srnoia,d aTer e Es- del y Tierra la Astron´omicas, de Ciencias de Instituto TLA LSESI V SURVEY VVV IN CLUSTERS STELLAR Geisler 1 1 1 .Mn Bidin Moni C. , .F Nieva F. M. , .Villanova S. , 3 HE AND Levato CEN A 2,3 1 4 n .N Chen´e N. A. and , HE 1,2 .Przybilla N. , 1 .E Cohen E. R. , NTEB STAR BP THE IN 3 He ieiephoto- pipeline h elines He the , 3 n H. and , 1 3 D. , ABSTRACTS etraineetdmntsoe hto rotation M 1.0 of and that 0.8 over for dominates magnetic the effect (2) perturbation and envelope; con- convective convection the we inhibits reduces field (1) so magnetic findings: the main that firm our Summarizing G. 50 hw eesldrn h aah rcsa lower M at 0.6 tracks and Hayashi (0.4 the masses during reversal a shows oiin iiglnt ovcintetetwith treatment α convection M 1.0 mixing-length and of position, phase, 0.8 sequence 0.6, pre-main 0.4, the at starting models, antcfil otiue ohge ufc lithium the surface (3) higher and abundances. to contributes cooler; field tracks magnetic the makes perturbation s[ as hloe eraei eprlyr,o (c) or layers, deeper in decrease shallower hrceieti tri oeraitcmne than models. manner classical realistic more to do a us in allow star stratifi- this calculations He characterize line-formation the the for in solution cation empirically an and tope h he olwn as a h ai ewe the between ratio densities, the energy of (a) gas one and magnetic laws: to following according para- three interior scales the imposed, stellar strength an the surface of whose throughout effects field includes, magnetic the now metric 953) method, 334, this A&A via 1998, al. et (Ventura rc,Austria. bruck, eea eMnsGri,Bl oiot M) Brazil (MG), Horizonte Belo Gerais, Minas ([email protected]). de Federal 3 Germany. Nuremberg, (nmaza@icate- Argentina Juan, 2 San conicet.gob.ar). (ICATE), Espacio del 1 1 ufc au costeselritro,(b) interior, stellar the across value surface ei eda etraino h tla struc- stellar the on perturbation mag- The the & a equations. treats ture Lydon as which by field 357) proposed 101, netic first ApJS low-mass (1995, of method Sofia evolution a and using field structure stars, magnetic the the of on studies effects ongoing our report We e emdlao conigfrthe for accounting atom model He new A =Λ nttt fAtoadPril hsc,Uiest fInn of University Physics, Particle Astro-and of Institute .T .Mendes S. T. L. eatmnod nehraEeroia Universidade Eletrˆonica, Engenharia de Departamento eesSenat CP nvriyo Erlangen- of University ECAP, & Remeis-Sternwarte nttt eCeca srnmcs el iray Tierra la de Astronomicas, Ciencias de Instituto m TLA OESO OAIG PMS ROTATING, OF MODELS STELLAR / ( H r TR IHMGEI FIELDS MAGNETIC WITH STARS ) P /M 15adsraemgei edsrnt of strength field magnetic surface and =1.5 ⋆ ] 2 / 3 ete optdrttn stellar rotating computed then We . ⊙ 1,3 ass u hi eaieimpact relative their but masses, .R Landin R. N. , TN2.3 ATON ⊙ Vaz ⊙ ;i n ae h magnetic the case, any in ); ihslrceia com- chemical solar with 3 tla vlto code evolution stellar 2,3 β mg n .P R. P. L. and , skp tits at kept is , β mg β 3 mg He decays a a has iso- 159 s- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 2 1 (lpv@fisica.ufmg.br). Brazil (MG), Horizonte Belo Gerais, ([email protected]). 3 Brazil (MG), Florestal 2 160 nalrevlm fteGlx,b en fthe of means by Galaxy, the enclosed of density volume formulation mass large hereafter new a dynamical 30, in a the 751, proposed calculate ApJ, (2012, to recently has al. MB12) et Bidin Moni rnfre otenwrsas h qaoilrota- equatorial The is stars. cloud tion newer formation, parent the the stellar to of transferred in momentum angular origin the its when has rotation Stellar rmtefitn rcdrsaeue oetmt the estimate to used are mean procedures fitting the from inprosby periods tion odrsl hncmae oma ausfo the from values mean data. to observational compared when result good ino hs tr.Fnlythe Finally stars. those distribu- velocity of rotational tion projected the fitting by awlinfnto.As edtriethe determine we Also function. Maxwellian rertto fasml fPeae tr with named stars Pleiades function, of distribution sample generalized a the of rotation cluster. true Pleiades inclination in mean stars real of set the a out for present find angle The to intends data. work observed and pro- models between divergences a theoretical to Such leads study. infrequently under not sample cedure pop- data stellar the the or of ulation particularities of value the a of adopts independent always angle inclination mean h qaoilrotation equatorial the aai siae rmtertobtentemean the velocity between projected ratio the the observational of from of sample estimated a is of sight, data rotation of stellar line the the between and axe angle inclination the is i .Miranda D. SIAIGTEMA NLNTO OF INCLINATION MEAN THE ESTIMATING UERN. IFMA. .Mn Bidin Moni C. nvriaeFdrld ics,Cmu F Florestal, UFV Campus Vi¸cosa, de Federal Universidade eatmnod ´sc,Uiesdd eea eMinas de Federal Universidade F´ısica, de Departamento NTELCLDR ATRDENSITY MATTER DARK LOCAL THE ON hswr t h itiuinfnto fthe of function distribution the fits work This OAINLAE FTEPLEIADES THE OF AXES ROTATIONAL V sin a ecluae rmterdu n rota- and radius the from calculated be can i 1,2 M´endez o uhPeae apepouiga producing sample Pleiades such for .B Soares B. B. , V 1 .Smith R. , 2 = 5 n .Moyano M. and , πR/P Silva V V 2 h mean The . 2 nteltrtr,the literature, the In . 2 .Carraro G. , sin n .R eer da Pereira R. J. and , i q n h enof mean the and ausobtained values 1 sin 3,4 .A. R. , i q since , value ABSTRACTS π/ q 4 - 6D atao Chile. Santiago, 36-D, ffcsi oeua lusdet oal accelerated rays. locally cosmic to low-energy due clouds molecular in ionizing effects enhanced submm of related implications on chal- I and work measurements recent the them. our from and describe drawn then W51) be will gamma- can and such that few conclusions W44, a lenging (W28, on focus sources will ray gamma-rays I gen- rays, high-energy brief cosmic and linking a After introduction regions. eral star-forming massive clouds molecular in with interacting AG- remnants and su- Fermi pernova intermediate-age with the associated by is range satellites, GeV the ILE the tele- in gamma- Cerenkov in other and especially of and scopes, HESS plane, class by seen galactic a as range the TeV that in established sources well ray now is It 4 Chile. Santiago, Vitacura, 3 Concepci´on, Chile. 160-C, Casilla ([email protected]). Chile Antofagasta, 2 0610, Angamos Av. ut,hneterciiim sntteslto othe MB12. to by re- solution found the the results not on puzzling is effects criticisms their negligible hence has sults, assumption BT12 den- MB12 by the mass that criticized the show of we evidence, overestimate Moreover, observational strong sity. as- all a an causes by on that based out is ruled formulation sumption BT12 contribution, this that cor- In show a matter. we dark that of ex- amount and the pected assumption, recovers formulation wrong 756, one-dimensional calculation a rected ApJ, MB12 by (2012, that flawed Tremaine argued is So- BT12) & the hereafter Bovy at 89, they matter dark literature, position. of the lar lack kine- a in three found available to surprisingly sets formulation data pop- this matical stellar Applying test a ulation. of kinematics three-dimensional iooOsraoi ,I312 aoa Italia. Padova, I-35122, 5 3, Osservatorio Vicolo 1 1 UENV ENNSCLIIGWITH COLLIDING REMNANTS SUPERNOVA eatmnod srnmı,Uiesddd hl,Casill Chile, de Astronom´ıa, Universidad de Departamento nvri´ iPdv,Dpriet iFsc Astronomia e Fisica di Dipartimento Padova, Universit´a di eatmnod srnmı,Uiesddd Concepci´on, de Astronom´ıa, Universidad de Departamento uoenSuhr bevtr,Aos eCroa3107, Cordova de Alonso Observatory, Southern European nttt eAtoo´a nvria a´lc e Norte Cat´olica del Astronom´ıa, Universidad de Instituto ntttdAtohsqed ai,France. Paris, de d’Astrophysique Institut OEUA LUS RMHG-TO HIGH- FROM CLOUDS: MOLECULAR O-NRYINTERACTIONS LOW-ENERGY .Montmerle T. 1 a , , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 1 46Mcl atao hl ([email protected]). Chile 2 Santiago, 782 Macul, 4860, Vicu˜na0436 Mackenna Av. Chile, Cat´olica de versidad .Jablonski J. lse fvrals u oli hswr a the was work many this of in goal samples Our the a improve variables. represents of to classes 870), also variable and 696, new of objects discovery ApJ, the photomet- for 2009, opportunity – unique the al., (CRTS et like Survey Transient Drake telescopes, Real-Time made Catalina surveys robotic ric synoptic small of by number increasing The eemn itnemdlso ( of modulus distance a determine erpr na xesv iesre td fthe of study time-series extensive cluster globular an on report We 21,AJ 7,1L nteVISTA the in 19L) D´ek´any the 776, by al. Using derived ApJ, et stars (2013, stars. RRab Phe for SX relation PL for used weighted-average were while magnitudes Cepheids, II RR Type for and magnitudes Lyrae fitted Fourier bands using both near- derived in were the relations Phoenicis) in (PL) SX coverage Period-Luminosity IR. phase and unprecedented Cepheids an II stars with pulsating type 270 RRc, for curves (RRab, per- the light derive was of to photometry epochs formed 100 PSF and and 42 VIRCAM@VISTA, cluster variable of This large in total its cluster A to 1310.1996). due content. project arXiv: star this 2013, for chosen was al. (Cate- et project Templates lan VVV the of framework the l 20,AJ 5,32.Fo yeI Cepheids II Type ( From of value 362). a derived 652, we ApJ, (2006, al. ± r udmna-oeplaos(lc ta.2005, them 40). al. of 363, et 12 MNRAS, (Olech least pulsators at that fundamental-mode confirm are the pulsa- we their use and infer we modes, to tion stars, magnitudes Phe and SX periods For derived (2006, 1979). al. 370, et Matsunaga MNRAS, by found was what to similar .S Oliveira S. A. IHINZTO CRTO SIGNATURES ACCRETION HIGH-IONIZATION ERI EIDLMNST RELATIONS PERIOD-LUMINOSITY NEAR-IR Ramos NCMATBNR ADDTSFROM CANDIDATES BINARY COMPACT IN h ik a ilnimNucleus. Millennium Way Milky The nttt eAto´sc,Fcla eF´ısica, Pontificia de Astrof´ısica, Facultad de Instituto .4mg ngo gemn ihDlPicp et Principe Del with agreement good in mag, 0.04 .Navarrete C. O AIBESASIN STARS VARIABLE FOR ORTLSOEOBSERVATIONS TELESCOPE SOAR 1,2 J .Gran F. , 2 and .M .Silva G. M. K. , 1 .V Rodrigues V. C. , ω 1,2 K etui(G 19,otie in obtained 5139), (NGC Centauri .Catelan M. , S 1,2 epciey eetknusing taken were respectively, , D´ek´any m .Alonso-Garc´ıa J. , − M 1,2 1,2 ) 0 n .A Almeida A. L. and , 1,2 13.67 = 2 .Cieslinski D. , ω .Contreras R. , m CENTAURI − K S M ± 1,2 ytm we system, ) .7mag, 0.07 0 n I. and , 13.78 = 2 ABSTRACTS Uni- F. , 2 - a etdi eino 4 method of region The a spa- in overdensities. to tested motion pa- was belongingness proper a and star provided tial codes the these indicating star, rameter each contam- For stars field ination. eliminating and after position em- motion, in the binary proper functions of Two density analysis using probability the sky pirical from motions. the established were proper of codes areas and large position in identi- stellar clusters for open method fying non-parametric a developed We o aps Brazil. Campos, dos 2 ([email protected]). Brazil Campos, 1 ofimdta n fte sClidr10 for We 140, Collinder clusters. is open them be of could one that them revealed confirmed of analysis three proper detailed and A that spatial having overdensities. de- groups motion to We stellar up catalogue. UCAC2 six BSS stars from tected UCAC2 1300 obtained supplement its were and R=11 located. magnitude are the 132 Collinder and oercosrain naflo-pproject. follow-up a in using pho- observations studied and tometric be polarimetric, will mCVs spectroscopic, work The time-resolved this in ratio. found S/N candidates low 1 with and features object 3 spectral Nova, unidentified absorption Hole 1 pure Black with (AGN), a objects as sources candidates identified extragalactic 14 previously 5 eruption, object 1 Novae, of mCVs, Dwarf stages to to final candidates the strong in 14 Nova this found In CRTS. we from sample 39 mostly nm on selected 468,6 decrement, objects Balmer variable II of inverted He and signatures line as for emission search accretion, to mass Telescope on high-ionization Spectrograph m Goodman 4.1 the SOAR used observational We (spe- detailed for classes follow-up. allowing these and of CBSS) expand- samples cially small candidates, hitherto the the for ing nature CV to CBSS magnetic the associated or constrains features accretion mass spectral high-ionization Finding accretion interesting probe scenarios. and objects rare progenitors. are Supernova Both (CBSS), Ia Type Sources to X-ray candidates disk, strong Supersoft accretion Binary no Close Cat- and with magnetic (mCVs) of Variables subclass a aclysmic polars, new of discovery PNCUTRDTCINI EXTENSIVE IN DETECTION CLUSTER OPEN .G Pa´ız G. L. PDUIA,A.Sihm iui 91 S˜ao Jos´e dos 2911, Hifumi, Shishima Av. IP&D-UNIVAP, A-NEMT,A.dsAtoats 78 S˜ao Jos´e 1758, Astronautas, dos Av. DAS-INPE/MCTI, K EIN SN ASTROMETRIC USING REGIONS SKY 1 .S eBiasi De S. M. , PARAMETERS ◦ × 1 5 n .B Orellana B. R. and , ◦ hr olne 140 Collinder where 161 1 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes sdi h raddntalwt eetit. detect to allow not did data literature. the area the of the density in in low found used the 132, not Collinder are to they Related magni- and than two 10.0 fainter other tude members The have clusters literature. possible the with agreement good iso bu 2 n enpoe oincompo- motion proper mean and (¯ 12’ nents about of dius srnm fteBlainAaeyo cecs Smolyan, Sciences, 3 of Academy Bulgarian Bulgaria. the of Astronomy Republic. Czech 2 Brno, University, Masaryk 1 Argentina. Plata, La 1900, s/n, Bosque del Paseo 1 (¯ coordinates mean which 162 gentina. u ftedlmasnei svr ffiin.Up efficient. very is Johnson the it in observations since only dilemma now, way to one the be of could are, out Photometry stars target faint. the very and normally, dense fields. very cluster are globular regions for Most spectroscopic important detailed very a is analysis for stars of preselection peculiar The apparent wide elemental peculiarities. a chemical suggest local of results variety their new Thought in members, of homogeneous distribution models. rather evolutionary be modify to and test to laboratories astrophysical main are clusters Globular nldn htmti swl ssetocpcstud- observations spectroscopic follow-up as ies. well for as which basis photometric solid results, including a promising as very serve give 6205 will NGC 7099, 104, NGC NGC and clusters: globular 3 for vations ∆ Str¨omgrenand ntergo rm40 o5600 5200 to around 4900 peculiarities from any distribution region flux filter the the three in measures This system band stars. narrow II Population peculiar ically ∆ a autdd inisAto´mcsyGo´scs UNLP, Geof´ısicas, y Astron´omicas Ciencias de Facultad nttt ueird Correlaci´on Geol´ogica, de Tucum´an, Superior Instituto LSES G 0,NC60,ADNGC AND 6205, NGC 104, NGC CLUSTERS: .Paunzen E. ohnNtoa srnmclOsraoy nttt of Institute Observatory, Astronomical National Rozhen A eateto hoeia hsc n Astrophysics, and Physics Theoretical of Department htmtyi mlydi re odtc chem- detect to order in employed is photometry BEVTOSO HE GLOBULAR THREE OF OBSERVATIONS α cosδ 1,2 ,¯ uvbyβ δ .K Illiev K. I. , =94 a/rwr band in obtained, were mas/yr )=(9,4) ytm r beTeto of tool The able are systems 7099 α , δ ¯ 2 )=(110.8 n .I Pintado I. O. and , .Tefis ∆ first The A. ˚ nodrt find to order in A ˚ ◦ ,-32.0 UBV a ◦ ,ara- a ), obser- ( ABSTRACTS RI 3 Ar- ) rbtost srpyia eeomn ftegalac- con- the main of and development astrophysical history to the tributions through travel a present I Brazil. 1 ods msin seilyi h 12 the in especially sensitivity emission, its to dust candi- owing to cluster fundamental for is embedded WISE Galactic analyze, dates. 10 to time, images first (NASA) the to- WISE database wave- with photometric infrared gether 2MASS work evolu- the at this In employed early visible dust. we by only and obscured heavily often being formation lengths, are their they Because during tion general in this, clouds. molecular born of giant are within associations embedded and clusters Star sfil fluctuation. resulted 55 field photo- Dolidze as and the 47 Dolidze only while considering data, Sequence metric appear systems, 25 Main physical Dolidze be Pre and 5 to and Dolidze MS present. are a (PMS) 25 (MS), Dolidze Sequence for Main clear while a show fit- and 5 Dolidze isochrone objects for The tings the areas. for decontamination important regions field their were extraction the RDPs central define The and to cases, significant. distribution certain profile are concen- In the density central 25, a Dolidze RDPs. ef- present in e.g. how objects extensions shown All and have tration systematically is. and been it publications has fective our method CMDs. in (Bressan This clean used models 2012). obtain PARSEC al. to from et isochrones 2010) Bon- fit (2007, by We Bica method & decontamination atto field em- We the (RDPs). ployed profiles density candi- radial diagrams and 4 colour-magnitude pa- (CMDs) astrophysical for produced B.). their We results determining (E. rameters. show of us view we in of study dates list present one We the this by In from 2002). inspections additional objects al. with Dolidze et (Dias interesting database selected DAML02 communicated the was to which Kronberger M. by clusters .B Pavani B. D. ad.W olwdtervsdls fDolidze of list revised the followed We bands. m AATCDNMC:OII,HISTORY, ORIGIN, DYNAMICS: GALACTIC eateto srnm,PyisIsiue UFRGS, Institute, Physics Astronomy, of Department AATCEBDE LSESWITH CLUSTERS EMBEDDED GALACTIC MS NRRDPHOTOMETRY INFRARED 2MASS RSN N PROSPECT AND PRESENT 1 .P eAraujo De P. P. , .Pichardo B. Bonatto 1 1 1 .Bica E. , n 22 and m 1 n C. and , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes e ag cl uvy oudrtn ti h next the the in with it understand prospects to decades. the surveys struc- scale and Way large dynamics Milky new the it from from known ture is what integral an of with vision finishing models, success- and most predictions the ful by passing discipline, dynamics tic 17 ail 90,Snig,Chile. Santiago, 4 19001, Casilla 3107, Breta˜na 1111, Gran 3 Valpara´ıso, Chile. Valpara´ıso, Ancha, Ave. Playa de Universidad cias, (bogdan.popescu USA 2 45221-0011, [email protected]). @uc.edu, OH Cincinnati, 210011, 1 M´exico (UNAM). de 1 LSESFUDI H IT VARIABLES VISTA THE IN FOUND CLUSTERS imgn OBx91,60 LNjee,TeNether- The Nijmegen, GL 6500 9010, lands. Box PO Nijmegen, Chil 22, Santiago 306, Casilla 5 Chile, Cat´olica de versidad Kurtev ihsfrselrcutr nbodbn surveys. algo- broad-band search in optimize clusters and stellar are for design rithms to templates used Lactea MASSCLEAN being Via Our also the in Survey. Variables (VVV) Vista the from can- didates clusters/cluster stellar ana- discovered to newly fitting the re- lyze isochrone mass. to traditional and templates sharpen age and CMD fine of MASSCLEAN function these a use We as nu- planes in color n- (templates) of merous maps thousands density of tens stellar of and dimensional creation errors. ages the photometric in and results observational masses This the cluster mimic tem- of CMD variety which generate a to for order plates in sam- clusters mil- stochastically stellar of 5 pled simulations perform We Carlo to Monte package lion bands. MASSCLEAN near-infrared the to used when limited ob- result are when particularly servations parameters fitting, all isochrone simple in using errors iden- the large clearly or available tifiable, when not is However, turnoff sequence main (CMD). dis- clus- color- diagrams using stellar by and magnitude determined resolved accurately mass partially better are or ters age, resolved of parameters: tance important The SN ASLA ODSRB STELLAR DESCRIBE TO MASSCLEAN USING eateto srpyis MP,RdodUniversity Radboud IMAPP, Astrophysics/ of Department nttt eAto´sc,Fcla eF´ısica, Pontificia de Astrof´ısica, Facultad de Instituto uoenSuhr bevtr,Ae lnod Cordoba de Alonso Ave. Observatory, Southern European eateto hsc,Uiest fCnint,P Box PO Cincinnati, of University Physics, of Department eatmnod ´sc srnmı,Fcla eCien- de Astronom´ıa, Facultad F´ısica y de Departamento nttt eAtoo´a nvria ainlAut´onoma Nacional Astronom´ıa, Universidad de Instituto .Popescu B. NTEVALCE VV SURVEY (VVV) LACTEA VIA THE IN 2 .D Ivanov D. V. , .Minniti D. 1 .M Hanson M. M. , 3 4 .Catelan M. , n .Lucas P. and , 1 .Borissova J. , 4 .S Larsen S. S. , 6 2 R. , ABSTRACTS Uni- e. 5 , eerhIs. nvriyo etodhr,Hted AL1 Hatfield, Hertfordshire, UK. of 9AB, University Inst., Research 6 Janeiro. 1 xicin fteErhsbopeefo h Late the from Cretaceous-Tertiary. the biosphere to Earth’s Ordovician mass the great five of the with extinctions arms pas- of spiral Sun’s the habitability the through of long-term sage correlations impli- the possible possible and to Earth, than the fact the more discuss this We of arms, cations spiral stars. the nearby 30% crossing most spends lifetime therefore verti- its low and of a component, de- and velocity eccentricity Sun, cal low The radius, co-rotation exceptionally a galactic time. has the from the to vary proximity half its can nearly time spite to arms the percent and spiral few inside neighborhood, solar spent stel- of the accu- fraction diversity in large good a orbits with is lar there traced that the be found when We Myr, can racy. 500 position last arm the in spiral arms spiral spent time the total inside the stars including solar-type parsecs, 212 20 than all nearer for passages his- ex- arm the spiral supernova of of tory by calculations detailed posed present We layer ozone plosions. destruc- Earth’s the and of ages; tion ice and cloudiness atmosphere increased Earth’s in triggering regions near forming rays heavy cosmic star provoking to exposure and higher cloud a bombardment; comet dis- Oort clouds the molecular turbing giant danger- include extinctions. is mass threats arms to Possible conducive spiral and biospheres around to or ous inside whether through spent surrounds passages time still Controversy few for arms. spiral makes the status this consid- that generally ers wisdom the Conventional of arms. perturbations wave spiral density the the in as co-rotation Galaxy period the the same around near revolve very stars mass where lies on radius, Sun bearing The possible planetary a extinctions. long-term with for evolution, stability important climate biosphere Galaxy, be of the might factor of which mentioned disk arms, rarely spiral the a Galactic are the in through stars passages their the and of orbits The H OA EGBRODADTESUN: THE AND NEIGHBORHOOD SOLAR THE .F ot eMello de Porto F. G. ASETNTOS AATCOBT IN ORBITS GALACTIC EXTINCTIONS, MASS etefrAtohsc eerh cec n Technology and Science Research, Astrophysics for Centre bevtoi oVlno nvriaeFdrld i de Rio do Federal Universidade Valongo, Observat´orio do Lorenzo-Oliveira CONNECTION? A 1 .S Dias S. W. , 1 n .K Siqueira K. R. and , 2 .L´epine J. , 4 3 D. , 163 0 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 1 Reggiani M. H. 2 164 ag vrbnacso abn([ carbon of overabundances large ea-or(EP tr.Teeaemetal-poor are These carbon-enhanced as known ([ stars. stars (CEMP) of halo class metal-poor Galactic a the is of there populations stellar the Among eea oRod Janeiro. de Rio do Federal 4 S˜ao Paulo. de mosf´ericas, Universidade 3 jub´a. 3 University. National 2 S˜ao Paulo. de Universidade vlto iuain fCM stars. will, CEMP and of stellar simulations prep) new evolution in against al., abundances their stars et. test eventually, theses (Kennedy confirmed that stars We stars CEMP stars. as CEMP Lyr newly-identified RR of known set are tele- a Observatory WiFeS of Spring with scope Siding obtained 2.3m results showed observations over- In we large elements. work, has s-process this that the and Lyrae carbon RR of abundances VMP recent the a is of interest particular discovery system Of halo Way. the Milky the in of studied metal-poor dwarfs extremely and giants and that (EMP) (VMP) revealed with metal-poor have consistent very are stars patterns abundance Lyrae typical el- observations their RR s-process spectroscopic metal-poor Recent and of carbon companion occurs. of a ements production from the transfer star, where (AGB) branch mass giant asymptotic of low-metallicity to evidence believed resultant widely exhibit be enrichment, which element class, s-process CEMP-s of the of of is one number Christlieb them characteristics; a & abundance specific (Beers the exist with stars of 2005) There CEMP details of classes elements. uncover different the to of begin origins abundance can their one studying by patterns, decreas- so with and increases metallicity, stars ing these of frequency The e/H F nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto ainlOtclAtooyObservatory. Astronomy Optical National eerhSho fAtooy&Atohsc,Australian Astrophysics, & Astronomy of School Research nttt eCˆnisEaa,Uiesdd eea eIta de Federal Universidade Ciˆencias Exatas, de Instituto nttt alsCaa ih eBiof´ısica, Universidade de Filho Chagas Carlos Instituto OTNE ERHFRCM RR CEMP FOR SEARCH CONTINUED A nttt srnoio efıioed ieca At- Ciˆencias de e Geof´ısico Astronˆomico, Instituto ] < 1 . )saswoeamshrsexhibit atmospheres whose stars 0) 1 .R Kennedy R. C. , YA STARS LYRAE .Beers C. 3 2 .Rossi S. , / e C/F ] ≥ 1 n T. and , +0 ABSTRACTS icas, . 7). - h aedniy h retto angle orientation the density, base the crto o:avr togwiedafmagnetic white-dwarf the strong at bands), very conditions I a extreme and flow: to R accretion related be in may polarization X-ray which no soft very and J1007.5- a spectrum, RX harmonics, (conspic- cyclotron peculiarities optical disk. observational uous accretion some has an without 2017 main- dwarf of low-mass white formation magnetized a the a from sys- to flows binary star matter compact sequence a which in polar: tem a is J1007.5-2017 RX Chile. - 3 France. Meudon, - 2 Universit´aria, 05508-090. S˜ao Paulo-SP - Cidade Brazil - Mat˜ao, 1226 do Rua 1 rcs ffitn,frec estar. the Be in each obtained for also fitting, is of process and parameter, scaling time The of observed curves. grid the light to a computed, we from that derived models dynamical curves, curves theoretical light con- two-color fitting from of of by extracted state be process the can whole that disk dynamical show the the We the during dissipation. on and disk struction depends the bump of the state of a cover form that excesses. The magnitude stars “bump-like” Be show and of years curves analy- few light the two-color through of only rate, sis injection mass the and a ikmdl ope ihterdaietransfer radiative the dynami- with that coupled code show models we disk VDD, cal the for approach disk ikprmtr,sc sthe as such parameters, disk ad ymaso icu ocs olwn the Following forces. viscous out- diffuses of and means dynamically star by the is wards of equator material the cir- near stars, for ejected Be model disks (VDD) Disk” cumstellar Decretion “Viscous In .G Silva G. M. IHMGEIE OA XJ1007.5-2017 RX POLAR HIGH-MAGNETIZED .R R´ımulo R. L. S,Aos eCroa 17-Vtcr,Snig eChile de Santiago Vitacura, - 3107 Cordova, de Alonso ESO, .V Rodrigues V. C. bevtied ai LSA lc ue ase,92190 Janssen, Jules place 5 /LESIA, Paris de Observatoire eatmnod srnma nvriaed S˜ao Paulo, de Universidade Astronomia, de Departamento AAEE FDSSO ESASBY STARS BE OF DISKS OF PARAMETER OAD H EEOMN FA OF DEVELOPMENT THE TOWARDS HDUST H NLSSO IH CURVES LIGHT OF ANALYSIS THE NETGTN H VISCOSITY THE INVESTIGATING EIUOAI IEIEFOR PIPELINE SEMIAUTOMATIC RBN CRTO NTHE ON ACCRETION PROBING 3 a eue o osriigfundamental constraining for used be can .Baptista R. , Costa 1 .C Carciofi C. A. , 1 α 1 .Cieslinski D. , n .Campbell R. and , .Rivinius T. icst aaee ok sa as works parameter viscosity 4 .S Oliveira S. A. , α 1 3 icst parameter, viscosity .Haubois X. , 1 .Ribeiro T. , 5 i ftedisk the of 3 .E R. E. J. , 2 and , 2 K. , α - XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes n h ylp oe hc dpsa3 represen- 3D column. a accretion adopts the which of tation code, us- Cyclops modeled de- was the orbital emission The ing cyclotron dwarf. the white of the pendence mainly near arises region emission a line of from that tomography reveals Doppler state dis- low are the phases. state, components some two low in are and tinguished in narrower lines are components; the lines three state the have bright are and lines in HeII broader Gaussians: and Balmer single and The not HeI, lines. Balmer, emission The strong HeII show star. spectra mass-donor low-state bright-state the The from on features superimposed phases. absorption lines emission orbital contin- humps Balmer The show some cyclotron spectra the at nm). and visible 700 states to are both region (435 in nm varies spectral 760 uum the to cover 360 from data resolution spectral 29k/ n 7 ms.I rgtrsae the state, brighter a In was resolution km/s). spectral 170 and low resolutions km/s the spectral two In (219 with data states. gathered brightness we state, different found We in 2012. object dis- of runs the semester observing first the in time- around telescope tributed SOAR spectro- obtained the Goodman we at mass- the dwarf, graph the using white from spectroscopy the accretion, resolved accre- to the low star a study To donor and surface) rate. on tion MG 100 (around field qa to equal o e i r a g i i a l a ,Z,La, Zr, Y, Ba, Al, Na, Ti, Si, Mg, Ca, Cr, Ni, Fe, composition for chemical the at- and the parameters spectroscopy mospheric resolution high using 2360 NGC aatcnrcdsac qa o9 to equal distance galactocentric 5 4 3 2 ([email protected]). Brazil paciais, G 30i noe lse ih0 with cluster open an Galaxy. is the of 2360 un- stars the NGC field reducing with stars distance associated and the certainties disk), age since thin same evolution, the the and and present (thick of structure disk stellar evolution the and and of formation our components test two the to of laboratories excellent knowledge are clusters Open 1 ubltSaeUiest,USA. University, Brazil. State Catarina, Humboldt Santa de Federal Para´ıba,Universidade Brazil. do Vale do Brazil. Universidade Sergipe, de Federal Universidade ii˜ od srfıia nttt ainld Pesquisas de Nacional Astrof´ısica, Instituto Divis˜ao de IHRSLTO PCRSOI OF SPECTROSCOPIC HIGH-RESOLUTION E INSSASI G 2360 NGC IN STARS GIANTS RED .V ae Silva Sales V. J. − 0p.W eemn o1 tr nthe in stars 15 to determine We pc. 30 1 ≈ n .B Pereira B. C. and 7k/.Telw(high) low The 170km/s. . 8Kcadheight and Kpc 28 . 5Gr with Gyr, 85 1 ABSTRACTS Es- hs uloytei nlwms tr ( stars of low-mass high-efficiency in to nucleosynthesis linked these be young may the in and of occurs clusters overabundance open s-process The the by disk. generated the elements of respect stars with field 2360 NGC to in s-process elements the the by of generated overabundance We slight abundances. a disk code observed typical also ele- are analysis iron-peak 2360 NGC and spectral of alpha ments the of abundance and The MOOG. Kurucz atmosphere LTE of the abun- models using and determined were parameters Paranal dances at Atmospheric UVES/VLT with Only Observatory. observed (Chile). was Silla FEROS La star at with one telescopes obtained ESO were 2.2m the stars at N. 14 and of O C, spectra for The ab- synthesis of spectral widths and equivalent lines, of sorption measures with Nd and Ce itiuino hi ytmo trcutr n star and clusters in star complexes of forming system bimodal their a of show distribution galaxies spiral grand-design Several fspoeseeet ihrlto ofil tr of stars clusters. open field old to and relation disk with overabundancesthe elements slight the s-process 2360) confirm of NGC to (like necessary clusters are open intermediate-age ob- analysis of Additional spectroscopic resolution high models. and evolutionary servations stellar explained the been by not has high-efficiency this However, ˜ oCito˜o i eJnioR,Bai javco,cl (joaovictor, [email protected]). Brazil Janeiro-RJ, S˜ao Crist´ov˜ao, de Rio 1 eneetd nadto,terdeigfe index reddening-free the addition, Q In already have dust ejected. and been gas whose clusters, older than s( vs es tl mesdi hi aetlcod fgas ( redder of a clouds general parental in have their dust, in and immersed still ters, hi al vltoaysae.Sraephotometry Surface stages. evolutionary early their npriua,w netgt h ffcieeso the of effectiveness the Q investigate present Group. we Local the the particular, in In In systems cluster were star indices for ones. explored photometric older embed- aforementioned the the the work, differentiate from pro- to clusters thus way ded and effective clusters young an the vided for age with relate MEDDSA LSESFO OLDER FROM CLUSTERS STAR EMBEDDED .F .Sno Jr. Santos C. F. J. bevtoi ainl u o´ rsio 7 20921-400 77. Jos´e Cristino, Rua Observat´orio Nacional, d d ( = ne nsrigotcutr fdffrn gsat ages different of clusters out sorting in index H NSUIGNA-RPHOTOMETRIC NEAR-IR USING ONES − ICIIAIGLCLGROUP LOCAL DISCRIMINATING H Ks − iga eeldta meddclus- embedded that revealed diagram ) K s .8 ( 0.884 - ) 1 .Dottori H. , INDEXES JHK J − igas h ( The diagrams. H a hw ocor- to shown was ) 2 n .Grosbøl P. and , H − Ks < 1 colour ) J . 5 M − 165 ⊙ H au- 3 ). ) , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes h hnmnni nvra.W ofimteindex the confirm We Q universal. that is suggesting phenomenon galaxies, the distant more for found that hnaot7Mrfo le clusters. older from Myr 7 about than 57 acig emn ([email protected]). Germany Garching, 85478 1 in distribution bimodal same showed and the photometry magnitudes surface the integrated from extracted The colors available. whose are and Myr ages clus- 100 approximately populous than for younger out ters carried was images 2MASS on 166 u,A.BnoGncle 50 10-7 ot lge RS, Alegre, 3 Porto ([email protected]). 91501-970 Brazil Gon¸calves 9500, Bento Av. Sul, Horizonte, 2 Belo (jsantos@fisica.ufmg.br). 31270-901 Brazil MG, 6627, Antˆonio Carlos Av. Gerais, a odtosfudi hsojc.Fo h maps, the From object. physicochemi- provide this the in maps found of These conditions overview cal resolved maps. spatially flux a the cal- were from abundance chemical culated the Analysis of Empirical maps (Nebular the Tool), NEAT code the the temperature ratio. from Using [NII](654.8+658.4)nm/575.5nm map the the from density and map the ratio obtained the We [SII]671.7nm/673.1nm obtained we pixel. the by maps, from these extinction With interstellar observed extracted between positions. line interpolating slit emission cube, given data of a the image each from the in for reconstructed slit nebula then each We the for direction, cube. observed spatial data lines func- the the emission a of the to pixel to each data gaussians in the fit fit to - best aims the tion that that package of parameters software find position a - to each MPFIT for used created We was obtained slit. cube the spectra data of a the separation Initially, The with 4”. of it. were map along slits to 4” positions order in parallel object multiple the were for Observations taken ex- with posures spectroscopy telescope. long-slit traditional m with made col- 0.9 Observa- were Inter-American (CTIO) study Tololo tory this Cerro using in the used 1 in data lected spectrophotomet- Menzel The resolved mapping. nebula spatially ric con- of planetary physicochemical method the the the of of study ditions a prensent We ODTOSO H LNTR NEBULA PLANETARY THE OF CONDITIONS nttt eCˆnisEaa,Uiesdd eea eMin de Federal Universidade Ciˆencias Exatas, de Instituto nttt eFıia nvriaeFdrld i rnedo Grande Rio do Federal F´ısica, Universidade de Instituto uoenSuhr bevtr,Kr-cazcidSr 2 Karl-Scharzschild-Str. Observatory, Southern European d APN FTEPHYSICOCHEMICAL THE OF MAPPING sapwru olt itnus lsesyounger clusters distinguish to tool powerful a as .Santos P. EZL1 MENZEL 1 n .Monteiro H. and Hα/Hβ JHK 1 igasas diagrams ai pixel ratio ABSTRACTS as , com). hektor.monteiro@gm ([email protected]; Itajub´a 1 1 apsLbrae u ava un,88 iedd,S˜ao ([email protected]). Liberdade, Brasil 868, Galv˜aoPaulo, Bueno, Rua Liberdade, Campus td fpaeaynblei oedti hncon- than detail more methods. the in ventional nebulae allows planetary method of This study observations resolution. from spatial results without retrieved we literature, that the from showing diagnostics, values with main well the compared for which values mean calculated we tr fteesasta ilb sdt raethe create to used be will that param- spectra. stars atmospheric synthetic the these of of synthesis. study stellar eters spectral a the in present used to we Here be incorporated to the be models for can population spectra that synthetic stars In create BHB will systems. we these for project expected this determination than the ages the to younger that, induces of of stars Because these stars. of BHB presence the for account do models not population stellar powerful however very nowadays, a tool analysis is spectra population integrated stellar using technique The using objects spectra. these of integrated determination in age the present induce in can errors presence are their and They clusters galaxies), stellar elliptical and (e.g. old. systems population although stellar many a hot, and very and stars hydrogen these blue of makes This layer nucleus. thin external Helium burning a their only of leaving part layers, lost their and of process most are through evolutionary (BHB) being Branch having Horizontal by Blue characterized the of stars The ´ ce eAstrof´ısicaN´ucleo d Te´orica, de Cruzeiro Universidade nttt eFıiaeQ´mc,Uiesdd eea de Federal Universidade Qu´ımica, e F´ısica de Instituto OEIGBU OIOTLBRANCH HORIZONTAL BLUE MODELING HRETPRO CISN BINARY ECLIPSING PERIOD SHORTEST CRTO ICMPIGO THE OF MAPPING DISC ACCRETION .Schlindwein W. .G Santos G. R. DSJ0926+36 SDSS 1 STARS n .P Martins P. L. and 1 n .Baptista R. and 1 1 Sul, o ail. XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes msinaogtegssra ( stream gas the along emission an,co crto ic( disc accretion cool faint, MCnsasaeutaopc iais( binaries ultracompact are stars CVn AM h curneo a temoeflwa htepoch. suggesting that rim, at overflow disc stream outer gas of the occurrence at the point impact the opc orea iccnr ( centre disc at source compact of shows curve map a light eclipse corresponding orbital The an S/N. obtain improved to aver- runs all We the combined of curves. Accordingly, light that previous with superhump-subtracted consistent rim. the is level disc flux from out-of-eclipse at age emission spot anisotropic bright to or- a of due nor superhumps modulation of runs. bital evidence all no at show quiescence data in was Our object February The 2012 March. binary between and observations the of of nights orbits 5 over Liverpool 20 covering m 2.4 Telescope, the Robotic with of collected report curves light J0926+36, we optical SDSS of Here analysis mapping eclipse techniques. the en- mapping maximum of eclipse aid hydrogen- tropy the its with disc of accretion map distribution deficient to brightness and surface sources, emis- light the the unde- different al- disentangle several cases to from nature sion some opportunity eclipsing unique (in Its a a lows outburst. of previous prob- reminiscence tected) occasions, a some as in curve ably light quiescent its in every bursts cisn MCnsa n lotesots pe- shortest displays curve the light ( Its also deep known. and only binary eclipsing star the riod ac- currently CVn an is AM via J0926+36 dwarf eclipsing SDSS trans- white and disc. companion lobe a cretion Roche to matter its overfills fers star donor degen- low-mass, erate hydrogen-deficient a where min) 65 for aaia apsTidd,80090 Florian´opolis- 88040-900, com). Trindade, raybap@gm ([email protected], Brasil SC, Campus Catarina, 1 L 83(A13 (RA 2883 ALS M ntevsbernei msin hseiso sa is emission This profiles emission. line in all range has visible 2883 the ALS in 1992. of in companion discovered Be system, The companion B-type sion .R Silva R. A. eatmnod ´sc,Uiesdd eea eSanta de Federal Universidade F´ısica, de Departamento v L 83 NLSSO SPECTROSCOPIC OF ANALYSIS 2883: ALS 10 ∼ . ∼ )i h rtkonrdopla iha emis- an with pulsar radio known first the is 1) i,a elas well as min, 2 a)elpe vr 83mn hc last which min, 28.3 every eclipses mag) 2 1 ∼ .S Levenhagen S. R. , 100 .V Leister V. N. − FEATURES h 0 .Sprup eeseen were Superhumps d. 200 02 m ∼ 47 ∼ s 4000 a mltd out- amplitude mag 2 , DEC 3 2 ∼ .K¨unzel R. , K T b 6000 lsenhanced plus ) ≃ − 17000 K 63 beyond ) o 2 P 50 and , K orb ′ 08 ABSTRACTS ,a ), ail. ′′ < , il xlnto o h nicreaincnb the be can anti-correlation the for explanation sible ni bu naerneo 100 of range age an about until esvt ftedsrbtos( distributions the of tensivity of nepee saprmtro ogmmr.When long-memory. of parameter q a as interpreted ffcsaengiil.W on htfrsolar-type index for the clusters that open found in We stars negligible. are effects nnnxesv omls N)teindex the (NF) formalism nonextensive In idm,Dprmnod ieca xtsed Terra. da e Ciˆencias Exatas 3 de Departmento Diadema, Terra. da e 2 Ciˆencias Exatas de ([email protected]). Departmento Diadema, pus 1 V etslto o nevlp ihT with envelope an for to solution leads best with analysis a this circumstel- computations algorithm, the the downhill-simplex in Iterating a condition environment. radia- boundary lar The a Roche as the field. assuming model solved velocity is equation Keplerian transport tive a environ- with circumstellar ment disk-shaped equi- a trans- thermodynamic within radiative local librium the assuming of equation esti- solution port were the envelope through circumstellar mated physical the The of quadratic conditions of laws. limb-darkening linear, mean neutral square-root adopting of the and transforms profiles through Fourier rotation the estimated helium of been zeroes first velocity has the rotation i sin pho- Projected V JHK and calibrations. UBV tometric Johnson’s through performed T 5000 of to timations 4000 range Coud´e spec- ≃ the the the with in at made telescope trograph 2883 m ALS 1.60 of OPD/LNA XMM- we observations the study, this the by In present detected Center. been orbiting Operation cir- has Science is a Newton as of star source presence the X-ray the Also, a to this due environment. and be cumstellar to stars, thought Be is many effect among hallmark common aigwt V with tating a density gas r i IAG-USP. exp → NFS nvriaeFdrld ˜oPuo Campus S˜ao Paulo, de Federal Universidade - UNIFESP RSN RMTESELRROTATION STELLAR THE FROM ARISING NFS nvriaeFdrld ˜oPuo Cam- Paulo, S˜ao de Federal Universidade - UNIFESP V .R .Silva P. R. J. ≃ 0,promdi pi 01 is-re es- First-order 2011. April in performed 200, IEDPNETNONEXTENSIVITY TIME-DEPENDENT h ytmbcmsetnieadtememory the and extensive becomes system the 1 sin ≃ 8 0km 90 R i ⊙ erae ihtecutrae h ex- The age. cluster the with decreases Soares ρ n xenlradius external and . rot s ≃ eff − 1 1 ≃ .M .Nepomuceno F. M. M. , 1 . 2 n o aaeeshv been have parameters g log and n .B eFreitas de B. D. and , 4 km 140 × 10 − 15 . s g.cm − 1 q n xadn with expanding and q )i o present not is 1) = − − ftedistribution the of 3 r nenlradius internal , e 0Mr pos- A 700Myr. ≃ n S/N and A ˚ 2 30 ≃ 1 .B. B. , q 50K, 9500 R a be can ⊙ ro- , 167 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes g eainhpcnb erdcduigamodel index a the using model this reproduced In NF. be from Medeiros can rotation- De the relationship that & shown age Freitas 1789) de 433, MNRAS, 1023). (2013, 326, momen- A&A, age angular 1997, initial stars an these their until of fact, tum memory In the memory). retain no to corresponding 2 1 van- considering momentum ishing, angular stellar initial the of memory 168 ytei,frtelnsZI41.3ad6362.34 and 4810.53 ZnI lines the for 2013). synthesis, al. et manganese al. (Barbuy the et sample Hill analysed this and of have abundances (2008) we Recently al. et (2011). Zoccali metallicity in and derived gravity were temperature, effective eters 4800-6800 R is resolution coverage a wavelength spectrograph. high mean at FLAMES-UVES observed The stars, the field with bulge 56 resolution of sample a for metal-poor in metallicity and stars. as redshift evolution of their function compare a quasars to in allows lines which absorption (QSOs), from metallicity the rive processes. helps nucleosynthesis different metallicities, its in varying understanding abundance and abun- Zn populations, its of stellar trace derivation to the order dance, In sim- alpha-elements. ad- metallicity, to increasing neutron ilarly with by decreases produced It partially dition. et being (Cayrel 2004), stars metal-poor al. in overabundant is Zinc h aaesprmtrzto,where parameterization, Kawalers the q ae h auae antcfil eie n the by and given regime, is field one magnetic unsaturated saturated the cates ag,and range, h hoyo antcbaigo tla rotation. stellar of braking magnetic of theory the t parameters eFets&D eers oe odrv nempir- an derive between to relationship model ical the Medeiros’ used De We & Freitas de respectively. geometry, field magnetic 0 nvriaeFdrld i rned ot,Brazil. Norte, do Brazil. Grande Norte, Rio do do Grande Federal Rio Universidade do Estado do Universidade hseuto osiue rdebetween bridge a constitutes equation This . ICAUDNE NGLCI BULGE GALACTIC IN ABUNDANCES ZINC ≈ ocmueteZ bnacsw s spectrum use we abundances Zn the compute To abundances Zn derive we work, present the In de- to reference of element main the also is Zn q 0 (1 − .R Silveira R. C. q a ∆ 0 and t/q steindex the is ∼ K N 50.Teamshrcparam- atmospheric The 45000. > ,wee∆ where ), q sammr aaee ( parameter memory a as r eae otednm and dynamo the to related are 0 y eg,Buire al. et Bouvier (e.g., Myr 100 STARS 1 q n .Barbuy B. and q , a o h lse ihage with cluster the for q and K t = 4 + 1 = q N K t − steequation the as sdrvdfrom derived is t q 0 K 1 aN/ steage the is indi- 1 = .The 3. ,at A, ˚ q q ABSTRACTS and 1 = A. ˚ 4 S˜ao Paulo.3 de Universidade - ug tr ftepeetwr r ne analysis. under are work metal-rich present the the for litera- of behaviour stars the Zn bulge of from details obtained The in data ture. metallicity, the increasing abundance with the with agreement that decreases shows [Zn/Fe] data of our of analysis The mm ehd o h nlssw aeueof use made we (4026 Helium analysis of Max- lines the Half absorption For three at Width method. (Full Fourier FWHM imum) the the techniques, and two method used We distribution database. the tra) present rota- we critical work their this of at In rotate not rates. do episodes tion stars ejection Be the most explain as cannot alone rotation u apeaeB/2seta ye hs aethe have whose velocities. type, greatest spectral of val- B1/B2 the majority are have The sample not our published. do velocity stars rotational our of of ues 84 literature. the in eue1536 use We 300 to 4471 eatmnod srnma nvriaed S˜ao Paulo. de Universidade Astronomia, de Departamento tr nodrt eemn the determine to order in stars 1 2 1 sytukon nsieo hi high their of spite In are ab- unknown. phenomenon) the yet Be of as so-called (the causes loss The mass normal episodes. ejection mass spo- by radic concen- in- produced equatorially both near envelope, an circumstellar a trated in often which originating and V-III, excess class lines frared luminosity emission and Balmer A type exhibit early spectral to of O rotators rapid late are stars Be Classical .B Soares B. B. OEFITTING MORE nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto nttt o srnm nvriyo Hawaii. of University - Astronomy for Grossa. Institute Ponta de Estadual Universidade nvriaeEtda eLondrina. de Estadual Universidade .Sitko C. nttt eAtooi,Go´sc Ciˆencias Atmosf´er Geof´ısica e Astronomia, de Instituto v TD FRTTOA VELOCITY ROTATIONAL OF STUDY A sin ) tr ihpoetdrttoa eoiisup velocities rotational projected with Stars A). ˚ kms i f21B’ tr rmBS B trSpec- Star (Be BeSS from stars Be’s 261 of ITIUINO ESTARS BE OF DISTRIBUTION 1 .Janot-Pacheco E. , − VLE IL STARS FIELD EVOLVED 1 1 .R .Silva P. R. J. , V ge ihteoe led published already ones the with agree sin i V .Fran¸caA. esrmnso vle field evolved of measurements sin I ITIUINFOR DISTRIBUTION 1 2 .P Silva P. M. , 1 n .Emilio M. and , q aaee from parameter ,4388 A, ˚ v sin 1 n V. and , i rapid , and A ˚ 1,3,4 icas, icas XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes h omgrvSinvsaitclts ofidthe find fit. to best test statistical Kolmogorov-Smirnov the B ucinta dut h itiuino h pro- dif- of the the distributions compare of we ferent Then distribution velocity. the rotational jected distribution adjusts type that power-law a function 413), 364, A, Physica h named the ed oexhibit to tends B al u otepretg fsaswt relatively with stars low of for percentage speed the high long to with due distributions tails rotation indicates point this ra rn,bnre edt have to another tend As binaries ones. trend, single broad the than dis- wider rotation are their tributions that indicating singles than higher o tr fhigh of stars for rlbhvo htbnre present binaries that behavior eral yia fSeI-,wt h xeto fteap- the of exception at feature the a with of II-P, pearance SNe of typical sublumi- II-P. the SNe of normal those and between nous in was the phase during luminosity plateau sublumi- bolometric nar- of The II-P. typical had SNe velocities, spectra nous low optical with The features 2009N. row SN near-infrared of and spectra optical near-infrared with and together optical, photometry ultraviolet, collected We II-P TYPE SUBLUMINOUS AND NORMAL THE to: (Email Brazil Mossor´o–RN, Norte, do [email protected]). Grande Rio 1 hnterflo-oos nadto,teeeit an exists in there point addition, inversion In fellow-colors. their than hsln spoal u ohg-eoiyHe high-velocity that to due found probably we is modeling line spectral this Via explosion. the h rsneo hsln,tgte ihaH compo- HV H a with of together nent line, this of presence The ehdadtesadrie ademto as method candle standardized the photosphere and expanding method the both of versions multiple material. circumstellar with ejecta the of vle stelmnst class. luminosity the is evolved to switches N20N NTE UENV BETWEEN SUPERNOVA ANOTHER 2009N: SN − eatmnod ´sc,Uiesdd oEtd do Estado do Universidade F´ısica, de Departamento − eut eeldta,a vrl rn,low trend, overall as that, revealed Results h I pcr fS 09 oti features contain 2009N SN of spectra NIR The eetmtdtedsac oS 09 using 2009N SN to distance the estimated We V V o l lse fsasudrsuy Specifically, study. under stars of classes all for nevl ihtedsrbto oe using model distribution the with intervals α a ea niao fwa interaction weak of indicator an be can , q < q Mxela oe (Soares model -Maxwellian > q eie hti ihrtemore the higher is that regime, 1 B B B − .Tak´atsK. − − auswhile values 1 V V V SNE V utemr,i sagen- a is it Furthermore, . ∼ rmwhich from , sin n alesdistributions tailless and , 1 i . 055 bandfrdifferent for obtained 1 4 asafter days +48 m < q q < q ausslightly values auslater values 1 > q tal. et o high for 1 regime 1 i λ B 10830 2006, D ABSTRACTS − V = hl ([email protected]). Chile 1 h eaieysaletmtdrdu ttetm of time the ( at explosion radius while the estimated stars, small supergiant relatively red of the that with consistent is uegatstar. supergiant ( mass normal pre-supernova and The II-P. subluminous SNe of typical values the tween iklms a siae ob 0 be to estimated was mass nickel h oa xlso nry( energy modeling. explosion hydrodynamical total via The explosion the progen- at the itor of properties physical the determined We n enaeo 7 of and age 2000) mean age al. a estimated et find also (Siess se- We pre-main models from evolutionary 2006). members quence group moving al. TWA age et for traceback Reza previous La the (De with agreement good in n h iprinaottema ieadynami- a give 7 mean of the obtained age epochs about cal the dispersion of the calcu- mean ra- and and The the when stars minimum. convergence 16 is of dius our epoch the from each taken for lated stars random 13 2000 Jack- of a generating lists applied technique we resampling star the nife each of of rid influence get to particular and be may non-members stars by of contaminated the sample us our in allowed that member TWA Assuming 2013) as literature. proposed 31 2012, 44 containing the group among stars kinematic al. consistent et a define (Galli to team developed as our strategy by point in analysis convergent published the membership on those detailed based of very with and literature.A over 2010) performed the spread - Chile) (2007 2013) - years Silla three measure- (La we ESO al. astrometric way - NTT/EFOSC2 et own reliable (Ducourant our fully ments of a advantage in take objectives age.To evolutionary our and achieve membership dynamical Hy- detailed its TW very and analysis a association including stellar (TWA) drae the on and mainly of description focused previous understanding work the improving present and the refining in efforts Our 21 .Teixeira R. EIIIGT YREI IH FNEW OF LIGHT IN HYDRAE TW REVISITING .L Campion Le F. nvria nrsBlo va eulc 5,Santiago, 252, Republica Avda. Bello, Andres Universidad . 6 ± Zuckerman 1 . p ( Mpc 1 1,2 . 5 .Ducourant C. , SRMTI DATA ASTROMETRIC ± R 2 ini 0 4 .G .Krone-Martins O. G. A. , . .Chauvin G. , y o h soito htis that association the for Myr 7 ≈ 31 = 8 R 287 . 4 . ± 67 1 ⊙ ± . 2,1 a on oayellow a to point can ) y.Teeresults These Myr. 2 ∼ 0 5 .A .Galli B. A. P. , . n .Song I. and , 1.Teproduced The 11). 0 . . 8fe si be- in is foe) 48 020 ∼ 13 ± − 0 . 13 1,2,3 0 M 004 6 . M 5 1,2 B. , 169 J. , ⊙ ⊙ ) . XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 1 1 agreement. are good average models in evolutionary the theoretical and ob- from technique derived association age traceback the the of via age tained dynamical the that show 170 oesawd ag fae,s twl epsil to possible capture be neutron twins the will elements. of solar it evolution so of temporal ages, sample the of Our study range processes. wide study s a covers detailed and the r allows the of which elements, ul- transitions heavy atomic the of of number In large a precision. is and there our traviolet accuracy is high obtaining that with thus Sun, analysis, results differential the the that for config- observed reference same also the we In uration VLT/ESO. the UVES at the with spectrograph (310-400nm) region ultraviolet the in 6 5 4 3 2 (IAG/USP). a wn.W aeotie ihrslto R= (R resolution ( high S/N obtained high and have 60,000) We twins. lar Costa acso eto-atr lmns(Z abun- elements chemical neutron-capture differential of present dances we work this In nvriaed ˜oPuo u oMta,12,Cdd Uni- ([email protected] Cidade Mat˜ao,versit´aria, Brasil 1226, S˜ao do Paulo, Rua S˜ao Paulo, de Universidade ltos osdrn ag fselrwn speeds wind stellar of ∼ range sim- a We hydrodynamic Considering 3D ulations. using HD209458b. Ly problem of calculated the transit approach the the ef- on during have the plan- absorptions and structures of conditions wind study wind etary stellar hydrodynamic different that 3D fect a present We .S ilrelD’Angelo Villarreal S. C. nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto et fPyis&Atooy-Uiest fGeorgia. of University - Astronomy & Physics Grenoble. of de Dept. Observatoire UCLA. - - Astrophysique Astronomy Lab. & Lisboa. Physics de of Universidade Dept. F´ısica - Bordeaux. Depto. de - Observatoire SIM/IDL - UMR LAB, CNRS, nttt eAtooi,Go´sc Ciˆencias Atmosf´er Geof´ısica e Astronomia, de Instituto [350 IFRNILCEIA ABUNDANCES CHEMICAL DIFFERENTIAL ASLS AERNE:H 048 A 209458B HD RANGES: RATE MASS-LOSS FHAYEEET NSLRTWINS SOLAR IN ELEMENTS HEAVY OF NTESNIIIYO EXTRASOLAR OF SENSITIVITY THE ON 1,2 − .Vel´azquez P. , 0]k s km 800] .TciMaia Tucci M. − AESTUDY CASE 1 ooa temperature coronal , 3 .Raga A. , 1 > n .Mel´endez J. and 0)setao oa twins solar of spectra 100) 1 .M Schneiter M. E. , 3 n .Esquivel A. and , > 1 0 nso- in 30) ∼ 1,2 [3 ). A. , − ABSTRACTS icas, icas 7] α 3 3 2 CONICET-UNC([email protected]). 1 in hna stoi lntr wind. planetary isotropic an absorp- larger than yields tions hemisphere day the from its escape inhibits that and wind atmosphere planetary stellar the strong compresses a by produced side, through night and the processes, emission reconnection es- the with the resembling associated regions, both, polar that through showing cape out, carried were anisotropic atmo- escaping sphere with planetary the models for several profiles evaporation Also, system. tary Ly in absorption vational e tla topeemdl ofidaphotomet- a of fit- find distance and to parallatic fluxes, models H ric and atmosphere J stellar the ted to to contribution secondary its the in infer by and caused modeled We variations June, ellipsoidal quiescence. 2005 in the in was object outburst the an when 2008 of decline the dur- m ing J 1.6 Dias/Brazil, the dos the Observat´orio at Pico of CAMIV in the telescope Oph with obtained V2051 bands, fast nova H of and dwarf sec- time-series the the report of We from photometry mass-transfer model). a enhanced (MTI to of ondary or due burst model) either a (DI 100 disc to the to in 20 instability accretion thermal-viscous factors the by where years, brightens to recur disc weeks which of outbursts timescales show on They disc. via primary) accretion (the an dwarf transfers white companion and a lobe to Roche matter its late-type fills a secondary) where (the star binaries compact are novae Dwarf ∼ × asls ae efudata a that a found we rate, loss mass Γ ncnrdcint ai rdcinfo h DI the from prediction basic a model. to contradiction in – oln aewhich a wave shows temper- decline cooling cooled radial outburst the disc disc along the non-negligible distribution the of ature evolution a as time had The decreased down. disc which angle accretion sug- outburst opening the 2005 that the from gest decline the eclipse along H-band and maps J in asymmetries brightness back NRRDACEINDS APN OF MAPPING DISC ACCRETION INFRARED nttt eCeca ulae,UNAM. Nucleares, Ciencias UNC. de Naturales F´ısicasInstituto y Exactas, Ciencias of Faculty 10 ∼ [3 nttt eAtoo´aT´rc Experimental, y Te´orica Astronom´ıa de Instituto H WR OAV01OHUH IN OPHIUCHI V2051 NOVA DWARF THE 6 − [1 n w auso h oyrpcindex polytropic the of values two and K UBRTADI QUIESCENCE IN AND OUTBURST . 5] 01 .Wojcikiewicz E. × − 10 1 . 10 3,wiekeigfie h stellar the fixed keeping while 13], s g accelerates − 1 ieacutfrteobser- the for account give 1 α d n .Baptista R. and esrdfrteplane- the for measured (111 = si rvl inwards travels is as M ˙ ± p ag between range 14) pc 1 Front- . XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes cl). 1 [email protected]) ([email protected]; Brazil rina, 1 ino on trcutr sulkl ob purely be to unlikely is clusters segrega- still star dynamical. mass are young that of they conclude tion while we Therefore, segregated can- clusters mass fractal. star highly young young be that of find not evolution We early clusters. the star of degree segregation the the mass and on of morphology focus the we between particular, correlation In seg- clusters. young-mass star for regated model theoretical further our to parameters constrain seg- investigate initial different We mass of influence timescale. be the short can very within clusters regated star cool sub-structured dynamically initially and suggest simulations body ealct,B-MB ol erlvn oexplain decreasing to relevant with be luminosity could BH-HMXBs X-ray pro- metallicity, their and of rate increase suggested duction Further- the of in medium. because re-ionization more, intergalactic and and heating interstellar of the sources potential (BH-HMXB) binaries role as X-ray the high-mass suggested black-hole have works of many years, recent In Recent evolution. re- dynamical i.e., from fast dynamical, segregated from formation or sulting mass star cloud, form molecular the parent of stars their result which this a pri- in is of either process it origin as is, suggested The that been mordial, has clusters. segregation star dynam- mass and of process evolution forming ical star tool of the important one investigate an is is to which cluster properties star dynamical young the the of segregation Mass rp eAto´sc,Uiesdd eea eSnaCata- Santa de Federal Astrof´ısica, Universidade de Grupo TLA EDAKFO BLACK-HOLE FROM FEEDBACK STELLAR otfii nvria a´lc eCie([email protected] Chile Cat´olica de Universidad Pontificia IHMS -A IAISI GALAXY IN BINARIES X-RAY HIGH-MASS ASSGEAINO ON STAR YOUNG OF SEGREGATION MASS .C Artale C. M. OMTO MODELS FORMATION .J Pellizza J. L. GALAXIES CLUSTERS 1,2 .B Tissera B. P. , .Yu J. 1 1,3 1,2 and , . ABSTRACTS N - . 2 Argentina. 1 h nryi eesdit h neselrmedium. interstellar the into released how is and energy redshifts, the high numeri- at high future, in simulations BH-HMXBs resolution the of cal In role the explore. study will to we schemes there different events, still physical are different needed properly range describe dynamical wide to the the and problem modifying the complexity of the at due However, efficient activity. formation not star BH- is that feedback suggest HMBXs results preliminary SNe Our include feedback. also which simulations hydrodynam- cosmological using ical study feedback we work, BH-HMXB this kinetic In the galaxy. host form- the star on regions modify medium, ing could interstellar BH-HMXB local that the suggesting in sources deposited mean- these be a by released could indicate, energy observations the of As amount ingful at stages. Universe early the of its history ionization and thermal the n et fteLCds.A yrdc four of byproduct a As disk. inclination LMC the the as of well depth as and SFH extension components its outer estimate LMC spa- and the the recover of to 2005). dependency able tial were al. we et technique this (Girardi With TRILEGAL mod- by with account them into elling stars We foreground MW diagrams. the take colour-magnitude LMC SFH the observed the of the recover outskirts the to from in 2005) variations al spatial et its Javiel and 1999; In al (Gal- method et models lart detail. partial the unprecedented forma- employ we star with work this LMC (SFH) outer opened history the region tion study surveyed to large possibility This the center. its from apealreadcniuu rao h M disk LMC the of to area data continuous down available and the large LMC, a the sample of main regions and (DES). forming bar Survey the star misses Energy footprint DES Dark the the Although for Magellanic preparation data, Dark Verification in Large by Science covered (DECam) the Camera been Energy recently of have (LMC) regions Clouds outermost The gentina. 3 Argentina. .Balbinot E. OUAINI H IH FTEDARK THE OF LIGHT THE IN POPULATION nttt eAtoo´ayFıiadlEpco unsAires Buenos Espacio, F´ısica Astronom´ıa del y de Instituto osj ainld netgcoe in´fia T´ecnic Cient´ıficas y Investigaciones de Nacional Consejo nttt retn eRdosrnmı,Brztgi Ar- Radioastronom´ıa, Berazategui, de Argentino Instituto H M UE IKSTELLAR DISK OUTER LMC THE r Costa ≃ 1,2 4a itne rae hn5degrees 5 than greater distances at 24 .Santiago B. , NRYSURVEY ENERGY 2,3 n .A .Maia G. A. M. and , 1,2 .Girardi L. , 2,3 4 .N da N. L. , 171 as, , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 1 4 3 2 1 stellar LMC new of catalog clusters. a assembled we analysis 172 hc ih niaelwrds xicinat extinction dust colours, lower UV indicate might rest-frame which blue have found galaxies also have these We star-forming that Universe. for the reionize required current to be galaxies our would below limits galaxies detection faint from contribution at inadsa omto aedniyo hspopu- this of density rate at func- formation lation luminosity star UV and the tion but identified, robustly be our of some review failures. will and I accomplishments at bursts. surveys recently gamma-ray more deep using and via wavelengths, highest-redshifts, radio boundaries X-ray, the optical, the At pushing are appar- them. we monsters with central growth their very ently that to back and look times, we Uni- early as the precariously of drops age and the verse half star roughly as that at demonstrate content, peaked now formation studies gas of wealth black and A supermassive central stellar holes. their of their evolve, growth the galaxies of as how well terms of in picture complete both more a high giving us at spectrum, electromagnetic galaxies the across star-forming redshifts charactering find- in and progress ing tremendous seen have years Recent unPtro ffc weeteIMi pqeto opaque is IGM Lyman- this the see (where we effect where Gunn-Peterson galaxies at of drops fraction line the but sion, hs ya ra aaistruhLyman- of through galaxies confirmation break spectroscopic Lyman some these been has There EA-ORATV AATCNUCLEI GALACTIC ACTIVE METAL-POOR otfii nvria a´lc eChile. Cat´olica de Universidad Pontificia INAF. Padova, di Astronomico Osservatorio Observat´orio Nacional. e-Astronomia. de Laborat´orio Interinstitucional F´ısica, UFRGS. de Instituto z eecp aeealdLmnbekglxe to galaxies break Lyman enabled have Telescope 2 = α AAISA IHREDSHIFT HIGH AT GALAXIES ). z − .C Bicalho C. I. 6 = .Hg saefatosadalarge a and fractions escape High 4. > z − ,prasdet h ne fthe of onset the to due perhaps 7, em ob uhlwrthan lower much be to seems 8 .E Bauer E. F. 1 n .Telles E. and 1 1 α > z emis- ABSTRACTS 5. xsec fa G nti ea-orgalaxy. metal-poor this the with in well AGN agree an analysis of this existence re- of central results unresolved The the gion. from only comes emission fsa omto urudn t otytruhthe through mostly regions Paschen- it, the studying surrounding and formation are region star We nuclear of that the analysis. of benefits cube kinematics the the data to to due provides tomography it methods PCA unconventional use as atypi- We such is regions. which HII wings, for cal extended permitted with strong lines shows galaxy emission this of spectrum The Inova¸c˜ao. 1 1 DSJ0703 1 o O/H log galaxy + Field HII (12 Integral metal-poor J1047+0739 Infrared the SDSS analysis of Near (NIFS) on Gemini based Spectrograph from results host data the they of present if We see to AGN. galaxies an dwarf nu- infrared peculiar near galaxy obtaining of We by active spectra statement galaxies. this the supermassive test that to in aim found fact usually the are to clei due supersolar. is slightly to This solar with from metal-rich, ranging be metallicity to considered are galaxies Active esddCtoiad Chile. Cat´olica de versidad obn h A e.W n httepcla velo- 170 peculiar is the galaxy WAT that the find of mechanism We city this jet. WAT for the needed ICM bend is (ICM), the to km/s and medium 800 galaxy intra-cluster than the greater the between velocity of relative and a properties jet the the Given galaxy. of elliptical in located central bending source the jet radio in (WAT) the Tailed for Wide-Angle the determine responsible the to of is intended pressure dynamics 562 ram the if Abell of galaxies study of recent cluster a present We mswihsol eeog oepantebending jets. the the explain to 1000 of enough than be greater should which velocities km/s peak bulk produces with typically motions merger flow of this type in This occurred merger system. off-axis Chandra an archival that and our suggests data data However, velocity these North. of Spec- Gemini analysis Multi-Object at mem- Gemini (GMOS) cluster the trometer galaxy with 146 obtained of the velocity bers on based the is of This analysis bending. the produce to enough bevtoi ainl iitei eCˆni Tecnolo Ciˆencia Minist´erioObservat´orio e de Nacional, nttt eAto´sc,Fcla eF´ısica, Pontificia de Astrof´ısica, Facultad de Instituto NLSSO H EOIYDT OF DATA VELOCITY THE OF ANALYSIS .Calder´on Espinoza D. α n elns efidta h ra line broad the that find We lines. He and LSE A562 CLUSTER 1 ± n .G´omez P. and 4 mswihi not is which km/s 140 ∼ 7.85 ± 2 0.02). i e gia Uni- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 2 aeadselraeadANfato l correlate all fraction AGN and age star-formation stellar and and observed rate widely en- pas- are dense in to vironments Trends populations spheroidal effects. more and/or external sive or internal more is to evolution prone galaxy whether debated widely is It les-Brazil. - Ilheus - 1 H raeigosre neiso ie rmteuse the diagrams: diagnostic from kinematics lines of emission on observed broadening IFU. an instru- with GMOS equipped the ment using telescope South Gemini the H velo- monochro- radial maps. obtained and city we dispersion lines velocity intensity, these matic emission on observed Based the using lines. realized be these may of kinematics objects internal of study stellar The weak a bycontinuum. on dominated superimposed lines, spectrum emission strong with rate formation stellar aigds ihavlct mltd of ro- amplitude velocity a a with with consistent disc gradient tating velocity a shows 1020 the σ vs V clpten lhuhbt r H are both kinemat- although different pattern, a show ical galaxy, each for maps, sion shells expanding of winds. presence stellar the and example, for tify, eoiygain nbt msinnuclei. emission observed both the in of gradient despite typical velocity system, a rotating exhibit not a does of 461 pattern UM hand other the On NENLKNMTC FH OF KINEMATICS INTERNAL MSINLN MGN UVYO THE OF SURVEY IMAGING LINE EMISSION Arag´on-Salamanca eiiSuhObservatory. South Gemini ii ii aoaoi eAtosc erc bevcoa UESC - Observacional e Teorica Astrofisica de Laboratorio .Chies-Santos A. eamt netgt h rgno h line- the of origin the investigate to aim We ehv tde h nenlknmtc ftwo of kinematics internal the studied have We efudta ailvlct n eoiydisper- velocity and velocity radial that found We oeaySirn Model Stirring Cometary aaisaedafglxe hrceie yhigh by characterized galaxies dwarf are galaxies aais M41adCS12,osre with observed 1020, CTS and 461 UM galaxies: h nlsso hs igaswsbsdon based was diagrams these of analysis The . BL 0/0 SUPERCLUSTER 901/902 ABELL .S Carvalho S. M. 1 .RdiuzdlPino del Rodriguez B. , 1 .Bamford S. , 1 n .Plana H. and htalw st iden- to us allows that 1 ii n .Gray M. and , sσ vs I II aais CTS galaxies. GALAXIES ∼ 1 0k s km 40 , sV vs I 1 A. , ABSTRACTS − 1 e , 1 . u niiulaayi sn eiiGO data Gemini/GMOS using carried ( analysis we features, individual lensing out strong with all clusters, h ag f3 of range the asv hntepoethl.As ehv found have we Also half. poorest the than massive risi hsfil.I hstl ilpeetthe formation. present star will and regions AGN I density probing talk high A902 the this and on A901a survey In the prop- of such results field. first of this census full in a erties rate for formation diagnostics star AGN needed and urgently the provide will etyo h esit edt be to tend redshift, results indepen- the clusters, Our of the of dently richness. half richest and/or the that redshift indicate stacked we per clusters, Given data per the velocities data. of (47 number spectroscopic sample low SDSS the SOGRAS whole used the we For clusters) them. of one in red- with 82 0 stripe z= SDSS around among in shifts are structures and richest 2013) the Survey al. Arcs et Gravitational (Furlanetto SOAR (SOGRAS) the to galaxy clus- belong These of ters data. analyses spectroscopic optical dynamical using clusters performed have We utpecutrsse at 901(a,b)/902 system Abell cluster of The multiple effect the properties. from galaxy separated internal be very could still proper- and are galaxy important effects of environmental determinants Nonetheless form- key ties. the stellar start of making peaks earlier one mass densest mass assembling the and stars in ing forma- galaxies galaxy the of framework tion hierarchical How- the density. in galaxy ever, local the of measurements with agtdteH have the We OSIRIS targeted GRANTECAN. the the on with imager region filter the tunable currently of are survey We a undertaking ones. redshift-related ob- from galaxy mass study effects by stellar to and Therefore able environmental is decoupling one evolution redshift. region single single this a serving field at The environments masses galaxy groups. of and range related broad very few a a comprises main includes three it Besides clusters evolution. galaxy for laboratory 1 ∼ .Cibirka N. nvriyo otnhm UK Nottingham, of University 5vlcte e lse) eotie assin masses obtained We cluster). per velocities 25 AAYCUTR RMTESOAR THE FROM CLUSTERS GALAXY YAIA NLSSO =0 Z= OF ANALYSES DYNAMICAL RVTTOA RSSURVEY ARCS GRAVITATIONAL 1 .Cypriano E. , − α 8 n [NII] and × 10 . rz 0 z= or 3 14 Makler M λ ⊙ 1 54lnsTgte,these Together, lines 6584 n in fsubstructure of signs and .Caminha G. , z 2 . .Frtreo those of three For 5. ∼ 0 ∼ . 6 saunique a is 165 2 . ie more times 5 2 . n M. and , 3 , 0 . 5 173 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes l asssaitclycnitn ihec other: each with consistent 6 statistically masses all hi oor(-)o acu rpe bnacsand abundances triplet kinematics. calcium betweentheir half or trend and any (b-r) disk find colour don’t the their we to but belongs spheroid, stars. the light GCs to 3115 the the most of NGC from that half of drawn Nearly find distribution We being velocity of weighted system. consistent the are spheroid to GCs the general to in disk, the and its to estimate belonging can 3115. we of velocity NGC probability and in position population GC a GCs Given the spheroid. studied the of then and We disk thick the ve- of and dispersion velocity locity the overall recovered the we of populations, tracers stellar as (PNe) 3115, nebulae multi- NGC planetary of a and images Performing infrared of disk spheroid. decomposition the the band each or to: thick) assign belongs or it to component (thin galaxy necessary correct the is to the star recover it To though, galaxy. kinematics, host their evolution of the history to connected directly is kinematics Star Romanowsky 7 6 5 Australia. Hawthorn, versity, 4 3 Nottingham. Park, University 2 1 1 0 z= the that 174 2 S˜ao Paulo. de Universidade TRFRIG G N ASV PHASES PASSIVE AND AGN FORMING, STAR H ONCINBTENTEORIGINS THE BETWEEN CONNECTION THE . Coccato colo hsc n srnm,Uiest fNottingham, of University Astronomy, and Physics of School FGOUA LSES(C)ADTHE AND (GCS) CLUSTERS GLOBULAR OF etefrAtohsc uecmuig wnun Uni- Swinburne Supercomputing, & Astrophysics for Centre FGLX VLTO IC . AS 0.5 = Z SINCE EVOLUTION GALAXY OF nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto utainAtooia Observatory. Astronomical Australian University. State Germany.Michigan Garching, Observatory, Southern European USA. Cruz, Santa Observatories, California of University Brasil. Paulo, Sao USP, IAG, etoBaier ePsussF´ısicas. Pesquisas de Brasileiro Centro 3( Chies-Santos VLTO FTERHS GALAXY HOST THEIR OF EVOLUTION − +3 2 .Cortesi A. . . 9 1 n 8 and ) 5 .Brodie J. , 3 ODB DSDATA SDSS BY TOLD . .Arnold J. , n h =0 z= the and 3 . 2 6( .Bamford S. , 1 .Mne eOliveira de Mendes C. , − +5 1 . . 2 6 .Foster C. 3 ) .Usher C. , × 3 10 .Pota V. , 14 2 M 6 .Merrifield M. , . lseshv over- have clusters 5 ⊙ 4 .Strader J. , respectively. 4 .Forbes D. , 1 A. , 6 2 and , A. , 4 ABSTRACTS icas, L. , ttehgetselrms bins. mass stellar highest population the galaxy at the Retired in- dominate mass significant. galaxies lineless the more and as becomes while AGN bins the mass creases dom- stellar galaxies low forming at star dia- inates Purely WHAN used. the be purpose, can that gram For hosts. galaxies However AGN retired from distinguish objects. cannot these diagram BPT for the time forma- star with versus erroneously increases AGN can tion of importance one right the and the that decreases infer to gener- redshift migrates is mass as it stellar wing as hosts, Higher diagram AGN used. BPT and ally the In forming considered first star bin. we each distinguish for to obtained order were properties values average galaxy and of database STARLIGHT taken the were measurements from line emission the and mass aaisw on mle ausfrtelwrred- lower the for clusters. values shift C smaller found we clus- galaxies redshift the low to these related (C in ters be galaxies at can giant galaxies of that lenticular presence 0.3, and than early-type lower incre- for redshifts an observed C we of the Mainly, ment of percent flux. two 20 Petrosian of and total ratio 80 contain the which as radii , circular (C) index concentration galaxy eSS/R ewe 0.05 between from SDSS/DR7 sample galaxy red- de our and extracted and We spec- evolution mass mass-dependent completeness. galaxy stellar with deal of into to bins database sample shift wide the evolution. a binning galaxy need tra, of we phases that passive For form- and star between AGN interplay the ing, study to is goal Our 3 S˜ao Paulo.2 de Universidade - nardhf ag f0.185 members of as range redshift classified studied a galaxies we galaxy in 146 2013B), luminosity of x-ray properties al. the low Castell´on et 10 (Nilo of clusters sample a Using 1 .V Costa-Duarte V. M. AAYCNETAINIDXI LOW IN INDEX CONCENTRATION GALAXY nvriaeFdrld at Catarina. Santa de Federal Universidade Paris. de L’Observatoire LUTH- nttt eAtooi,Go´sc Ciˆencias Atmosf´er Geof´ısica e Astronomia, de Instituto -A UIOIYGLX CLUSTERS GALAXY LUMINOSITY X-RAY olwn oclc ta.20,w en the define we 2000, al. et Concelice Following .Cuevas H. .CdFernandes Cid R. > ) otayt hs eut,frlate-type for results, these to Contrary 4). 1 .L ioCastell´on Nilo L. J. , 1,2 Alonso .Stasi´nska G. , 3 n .Sodr´e Jr. L. and , < 2 < z z < < .0 h stellar The 0.50. 0.701. 1 2 n .V. M. and , .V Asari V. N. , 1 icas 3 , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 1 Argentina. CONICET), 2 1 2009) al. et clusters. Dressler rich 2009, for al. different et by (Poggianti proposed authors as galaxies, of evolution logical pia ein o h td fhg esitgalaxies. redshift the high to of UV study the the for from regions to optical models is study spectral this realistic of in- obtain motivation this main accomplish the The to show vestigation. order we in presentation, challenges dif- current the upcoming this of In nature and ferences. satel- systematics GALEX the the photometry studying by measured lite, UV galaxies the same ultraviolet, op- to the the the of predictions to fits our extended best compare be that we also model can within region the stars tical Since the of galaxy. motion the the velo- to the also due and dispersion It dust city by (2003). caused Charlot reddening the & population considers Bruzual stellar as simple such using libraries, optical by the fitting on et consists spectrum Fernandes synthesis Cid Spectral spectral by Digital al.(2005). empirical described the Sloan approach using the synthesis by a (SDSS) from Survey almost extracted Sky analyzed spectra has million Project STARLIGHT The aUiesdd eS˜ao Paulo de Universidade da ehiushv aue vrteps eae and decade, synthesis past the spectral over on matured have based techniques methods record Fossil EOVN AAISI IEADSPACE: AND TIME IN GALAXIES RESOLVING H EAINBTENTESPECTRAL THE BETWEEN RELATION THE YTEI FGLXE NTEVISIBLE THE IN GALAXIES OF SYNTHESIS eatmnod ´sc,Uiesddd aSrn,Chile. Serena, La de F´ısica, Universidad de Departamento nttt eAtooi,Go´sc Ciˆencias Atmosf´er Geof´ısica e Astronomia, de Instituto nttt eAtoo´aT´rc xeietl(IATE- Experimental Te´orica Astronom´ıa y de Instituto Falc´on Barroso PLIGSALGTT AIADATA CALIFA TO STARLIGHT APPLYING Delgado .L eAmorim de L. A. hs eut ol eascae otemorpho- the to associated be could results These P´erez EINADTERU EMISSION UV THEIR AND REGION .L Dantas L. M. 2 2 .Garc´ıa Benito R. , .F S´anchez F. S. , Walcher ,6 5, .S´anchez Bl´azquez P. , 1,2 4 n .Mast D. and , CUBES .CdFernandes Cid R. , 1 n .Sodr´e Jr. L. and ,3 2, 2 .Husemann B. , .M Gonz´alez M. R. , ,3 2, 1 ,2 1, 7 .J. C. , 4 E. , J. , ABSTRACTS icas 7 6 5 4 3 2 1 ti rca oko risotie rmproper from obtained orbits know arms, to spiral crucial the pat- in spiral is stars the of it of permanence speed the and such the disk, tern of Galactic determination the the of dynamics as the of studies In lms fwa st oefo AIAadfuture and CALIFA from surveys. come a IFS to providing is combina- synthesis, what spectral the of with glimpse of data richness IFS of the tion etc. illustrate diagrams, results radius-age The onto mass and cubes light (x,y,t) stellar growth the spatial of and dif- temporal projections the in dimensions, in normalized averages and 1D ways, scales ferent time formation different star on densities, rates and ages surface mean mass extinction, metallicities, properties stellar stel- v-field, galaxy the the of as of maps such 2D cubes history, 3D its formation include and lar These pipeline whole products. this data of description work a This provides coordinates. spatial and metallicity, multi-dimensional time, into properties population and stellar spectral the unpacking zone-to-pixel and reconstruction of image including series a operations, performs (v) all file, post-processing for single results STARLIGHT a into the the zones packs galaxy into (iv) code, spectra synthesis the spectral bad-pixel feeds extracts and (iii) (ii) errors flags, S/N, propagated the including account increase due spectra, taking errors, and correlated necessary of when to, zones Voronoi order into in cube (i) data which: observed the pipeline galaxies, partitions end-to-end 600 an of developed extent have optical Spec- we full Field the Integral over gathering troscopy CAL- is the which by survey, Motivated IFA the galaxies. about limited of information the physics are no internal providing of studies view, global these because a resolution, Yet, to spatial of evolution. lack of their understanding fos- and the spectra galaxies on advances galaxy substantial integrated tered to application their .A .Faria F. A. M. EEMNTO RMOSRAIN AT OBSERVATIONS FROM DETERMINATION nvria u´nm eMadrid. Aut´onoma Tenerife. de Universidad Laguna, La de Universidad Canarias. Astrof´ısica de de Instituto Potsdam. f¨ur Astrophysik Leibniz-Institut Alto. Alem´an, Calar Astron´omico Hispano Centro Andaluc´ıa. Astrof´ısica de de Catarina. Instituto Santa de Federal Universidade PNCUTRRDA VELOCITY RADIAL CLUSTER OPEN OBSERVAT 1 .Monteiro H. , .D L´epine D. R. ROPC O DIAS DOS PICO ORIO ´ 1 .S Dias S. W. , 2 1 n J. and , 175 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes .Fellhauer M. 2 1 spa- (and velocities. radial cluster’s cial) open libraries. the different present we from Finally spectra determina- velocity synthetic radial using and tion reduction analysis detailed data the the present of we di- work, HR’s this the In in agram. position their their of and/or analysis motions statistical proper by own concerning obtained our information clusters, from relevant the selected on standard were based using stars database speeds The radial techniques. their calculated and and telescope Dias m dos 1.60 Coud´e Pico spectrograph. the the the with at (LNA) obtained Observatory 4000, with of spectra using resolution clusters a open be- research of stars group our of a velocity to by longing radial maintained the determined clusters, we cat- group, our open the of of of statistics the potential alog improve the to Aiming and Galaxy. velocities radial motions, 176 aebihns n h cl-egho h luminous the of sur- the scale-length how the trends and see brightness We morphol- face dynamics. their their like Way, and Milky ogy the of classical galaxies pro- the dSph of our features many that star explains find scenario different We posed and (SFE). halo efficiencies DM formation the of masses different scale-lengths depen- with and the quantities investigate observable We of of dency numbers clusters. different star consider cusped dissolving and and profiles cored halo adopt we DM galaxy. survey dwarf the parameter dissolving of our halo by In DM formation isolation the of within the in clusters extension galaxies study star an dSph we as classical where of simulation model, of fiducial set our full we Here the or interactions. show galaxies of large mechanisms these orbiting other invoking that found fact mainly the are to forma- galaxies resorting the galaxies explain dSph to of attempt tion poor theories Many are and gas. content, in stellar lowest systems the dominated have (DM) matter known, believed dark most are the galaxies be These to model. hierarchi- cosmological Matter) cal Dark Cold (Lambda process ΛCDM formation the galaxy in the of the blocks considered building are basic galaxies (dSph) spheroidal Dwarf nvriaeFdrld Itajub´a. de Federal Universidade nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto eosre h pncutrsmme stars member cluster’s open the observed We H OMTO FDP GALAXIES DSPH OF FORMATION THE 1 .Assmann P. , 1,2 n .I Wilkinson I. M. and , ABSTRACTS icas. 3 iee sakyfauefrftr bevto with scenario. observation our validate future to for resolution feature high key con- a are the motions as alter streaming sidered which These conditions, results. stemming initial expected and unique remnants our fossil from named space, ve- in locity curves. substructures pa- cold dispersions kinematically the our velocity recognize identify We flat in we to vary leading space, ellipticity their rameters velocity and in In clumpiness irregularities simulations. how i.e. identify also shape, simula- We our of parameters tions. the with vary component on ouainrsds n h tla spheroid stellar population. the intermediate-old the the and containing where resides, disk population HI rotating young the different distribution: with least spatial systems at has kinematical different 6822 very NGC two kine- that confirm a and we is Thus distribution which matics. spatial stars, C different closer of with is spheroid system kinematics the of their behavior and moving the gas not to are HI PNe the contrary, with the On along rotation disk. the HI closely the the of of follow analy- members population The other stellar and galaxy. regions young HII this that in the shows found of sis kinematics disk of the HI velocities to extended radial compared better are heliocentric resolution objects The these a km/s. have 10 data than an- The telescopes- is from spectrographs. OAN-2.1m-MES spectroscopy 6822 and resolution NGC LCO-Clay-MIKE high galaxy through irregular alyzed the HII and in (PNe) nebulae regions planetary of kinematics The e,UK. ter, 3 2 Chile. 1 2 M´exic M´ex.(sfl[email protected]). D.F., 04510 70264, Postal M´exico, Apartado de 1 Spain. eatmnod srnma nvria eConcepcion, de Universidad Astronomia, de Departamento eateto hsc srnm,Uiest fLeices- of University Astronomy, & Physics of Department nttt eAto´sc eCnra,L aua Tenerife Laguna, La Canarias, Astrof´ısica de de Instituto nttt eAtoo´a nvria ainlAut´onoma Nacional Astronom´ıa, Universidad de Instituto OUAIN NTEGLX G 6822 NGC GALAXY THE IN POPULATIONS eatmnod srnma nvria eCie Chile. Chile, de Universidad Astronomia, de Departamento Hern´andez-Mart´ınez IEAI TD FDIFFERENT OF STUDY KINEMATIC A .Flores-Dur´anS. 1 n .Garc´ıa-Rojas J. and , 1 .Pe˜na M. , 1 L. , 2 o. , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ofr h ring. the form to material A donating may AM2217-490, galaxies with these group. interacted of have a one that featuring is hypothesis speeds, other plausible three similar objects, are there with other arcmin 5 galaxies to of radius galaxy a the in however, tails connecting no show bridges galaxies. SDSS ring or the of polar images among low-resolution The trend an a harbors following region nuclear AGN, the a Diagnos- that and show galaxies. galaxy, diagrams interacting tic host of the typical of value axis mean vari- of major little the that shows along density than ation electron al. lower The et and ones. Krabbe isolated Accepted), and MNRAS; MNRAS to et 2013, submitted (Freitas-Lemes galaxies 2013, interacting al. in that to lar fteinzto aaee (log parameter ionization the of eecp hl.Fo hm emaueahelio- a measure 9152 we of velocity them, radial From the centric on Chile. - spectra on telescope based 6250–7250 is the study range with This equilibrium in galaxy. yet not host of is PRGs), (characteristic of galaxy. rings structure the host bluish the still this surrounds a Apparently, is with that formation, AM2217-490 ring in galaxy. PRG asymmetrical of host case at the interesting approximately of an orbiting plane stars and polar gas the of surrounded ring elliptical), a type or by early lenticular an Po- by (e.g. of formed is galaxy GAL-1: studies PRG host A Posters case 178). also of (see GAL-2: series 163, (PRGs) a Galaxies of Ring part lar is work This M21-9:APLRRN AAYUNDER GALAXY RING POLAR A 2217-490: AM 2 irapuan@uivap. [email protected] [email protected], SP, - Campos Jos´e dos 1 eAooCetıc.RaEtdsUio 5 tjba-MG, Itajub´a - - 154 [email protected] Unidos Estados Cient´ıfico. Rua Apoio de cino h ieaisadceia bnac of abundance chemical and kinematics inter- of the effects on the action about is study observational This .Freitas-Lemes P. NVP/P,A.Sihm iui 91-Ubnv S˜ao - Urbanova - 2911 Hifumi, Shishima Av. /IPD, UNIVAP CILbrtoi ainld srfıia Coordena¸c˜ Astrof´ısica, de Nacional MCTI/Laborat´orio H FET FITRCINO THE ON INTERACTION OF EFFECTS THE IEAISADAUDNEOF ABUNDANCE AND KINEMATICS .Freitas-Lemes P. Fa´undez-Abans CONSTRUCTION 1 bandwt h TO15m 1.5 CTIO the with obtained A ˚ Fa´undez-Abans .Rodrigues I. , M2229-735 AM 1 .Rodrigues I. , 2 n .Dors O. and , ± 1 8k/.Tevalue The km/s. 18 .Dors O. , U 2 = − 1 3 M. , 1 . )i simi- is 5) 1 n M. and , ABSTRACTS br, ao 2 irapuan@uivap. [email protected] [email protected], e SP, - Campos Jos´e dos 1 eAooCetıc.RaEtdsUio 5,Itajub´a, MG, 154, Unidos Estados [email protected] Rua Cient´ıfico. Apoio de omaueteipc fgsbl oaino the on rotation Lyman bulk the gas of of impact morphology the calculations transfer measure radiative to of results present We oiiso 17518 of locities as Our imagery range band wavelength 4100-8600 the broad galaxies. in spectroscopy BVRI long-slit lu- the as on well very po- connect based is a to was tail of study seems sky-projected progenitor and The a minous be galaxy. fea- could ring arc-shaped system lar counter-tail This and lat- tail the ture. a com- NED02, a showing galaxy, and ter Sb(s)-like NED01, galaxy, sys- perturbed disk This a pact by formed 2229-735. AM is of tem galaxies component the n eta yrgnotcldph nterange the in depths optical τ hydrogen neutral and rsnsarneo ige obeadtil peaked triple and double single, of range morphology a line presents the off-center, located sources increases condi- ation same fraction the escape Under the center. tions a line to the at peak double peak a single from transforms line ho- the rotational velocities of large center for case sources, line’s the distributed the In mogeneously velocity. at rotational intensity with the that increases and find We width line homogeneous. the and central to respect sphere: with the sources radiation the for distribution ehd,w on htteHIrgosi AM2229- 12+ in metallicity: regions high HII have the 735 that found empirical two we Using methods, stars. are massive regions by selected all ionized that of mainly out source turns It ionizing regions. main emission-line the classify were to diagrams used diagnostic Standard (NED02). km/s aiu eoiisi h ag 0 range the with tempera- in rotation constant solid-body velocities a a maximum have at spheres hydrogen These and ture. mix- homogeneous dust a of with sphere ture a as galaxy a model dex. H H MATO A UKRTTO ON ROTATION BULK GAS OF IMPACT THE NVP/P,A.Sihm iui 91-Ubnv S˜ao - Urbanova - 2911 Hifumi, Shishima Av. /IPD, UNIVAP .N Garavito-Camargo N. J. CILbrtoi ainld srfıia Coordena¸c˜ Astrof´ısica, de Nacional MCTI/Laborat´orio 10 = 5 − 10 .W siae eicnrcrda ve- radial heliocentric estimated We A. ˚ 7 eas osdrtoknso spatial of kinds two consider also We . H LYMAN- THE ± n .Dijkstra M. and 5k/ ND1 n 17326 and (NED01) km/s 25 1 .E Forero-Romero E. J. , α α iei aais We galaxies. in line log LINE 2 ( O/H ∼ − 0.Frradi- For 30%. 0 ms km 300 8 = ) . 3 − ± 177 1 8 − 27 , ao br . 6 1 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes trfriggalaxies. forming star Chile. Brazil. SP, Campos, S˜ao Jos´e3 12244-000, dos Cep 2911, 2 Alegre Brazil. Porto RS, 91501-970, Cep Gon¸calves, 9500, Bento Av. Sul, 1 Bogot´a, Colombia. Ip, 2 Edificio 18A-10, No. 1 inter- distant to of useful results are spectroscopic results recent these pret how show We lines. 178 iccmoet.Tepol hw ih excess light a and shows bulge profile into The of decomposed was components. disc 1219A AM material pro- of brightness of surface file bridge the The a in galaxies. tail the and connecting tidal 1219A) (AM a Gemi- galaxy detected the We main at GMOS Telescope. the South ni with obtained spectra slit on ihMLfrbleadds fΥ of disc and bulge was for 1219A AM M/L of best-fitting with distribution overall found mass The the gas for a solution interaction. suggesting by asymmetric, quite curve perturbed rotation is The 1219A AM disc. and of bulge the structure brightness to lens addition surface a shows in the galaxy secondary hand, the of other profile the On regions. t.1 54,Grhn,Germany. Garching, 85741, 1, Str. hswr sbsdon based is work This of n Υ and .A .Lacerda D. A. E. .M Cendron M. M. IO EGRA 2940WT GEMINI WITH 1219-430 AM MERGER MINOR .R Herpich R. F. eiiOsraoy / UAIc,Csla63 aSerena, La 603, Casilla Inc., AURA c/o Observatory, Gemini a lnkIsiuefrAtohsc,Karl-Schwarzschil Astrophysics, for Institute Planck Max nttt eFıia nvriaeFdrld i rnedo Grande Rio do Federal F´ısica, Universidade de Instituto eatmnod ´sc,Uiesddd o ne,Ca 1 Cra. Andes, los de F´ısica, Universidad de Departamento nvriaed aed aaıa v hsiaHifumi, Shishima Para´ıba, Av. do Vale do Universidade HSCLPOETE FGLXE IN GALAXIES OF PROPERTIES PHYSICAL .Rodrigues I. M HTMTYADDNMC FTHE OF DYNAMICS AND PHOTOMETRY ∼ .A Hernandez-Jimenez A. J. 200 3 u otecnrbto fstar-forming of contribution the to due 53% H LA IIA K SURVEY SKY DIGITAL SLOAN THE d 2 = 2 = EETDI INFRARED IN DETECTED . . 0 4 − +0 − +0 2 1,2 0 0 .C Krabbe C. A. , 3 . . . . 5 4 3 2 .B Klein B. V. , 2 .Mateus A. , epciey n F profile NFW a and respectively, , × .L eAmorim de L. A. , .Bonatto C. 10 .J Braz J. F. GMOS-S 12 r M ′ and ⊙ 1 2 and .G Pastoriza G. M. , 3 .CdFernandes Cid R. , 3 2 .M Parize M. M. , 1 g .Winge C. , ′ c mgsadlong- and images 16 = 2 .L Rossi L. L. , . b 0 − +1 2 = z 3 1 . . and , ∼ 2 1 3 . . and , 8 1 2 , ABSTRACTS − +0 − 2 0 , 3 d- . . 3 4 4 , , hswr,w rsn h aetrslso h analysis data. the of this results of latest the present we In star work, (RT). this between galaxies “retired” separation and (SF) clear galaxies forming a first the obtain In we Institute. analysis, Federal Sci- Catarina Computer Santa of of ence Department in done the to is with This order conjunction in infrared. the an- tools in properties are computational the identify new objects ga- a These SDSS using of objects. alyzed subsample 000 300 a match about creating the laxies of made the catalog and with the WISE in database the our from obtained increase data We the mission, recently project. a WISE obtained inclu- catalogs font the of with sion spectrum re- this electromagnetic infrared continue the the of we in gion work, attention our this focusing broad- In expansion, spectral coverage. ultraviolet, analyzing our GALEX started ening the also we from com- Recently is data which objects, public. million properties pletely 1 physical nearly this of to of database galaxies result a of The build spectro- to data. was the SDSS effort the with of especially analysis following scopic in challenges, researchers successful new other was group these France, with and research collaboration Brazil Our from in UFSC, regions. at spectral projects and different incon- data almost in observational a an of of experiencing amount availability ceivable the is with age astrophysics golden extragalactic The 3 Cam- 203 Sala 2 – ([email protected]). 88040–900 G CEP Brazil Florian´opolis, – Bloco SC, 476 – Postal Catarina Universit´ario Cx. pus Trindade, Santa de Federal dade 1 omn tr hnteS aaisbcueteSFR the because galaxies Sm the when than efficient is more stars result are and forming main galaxies galaxies spiral The dwarf of galaxies. the type that Sm other both to for similar also similar the very of were are values at The they SFR acquired MIDAS. and software were SPM-OAN the with have the images reduced of galaxies The telescope late-type 1.5m not. the of or kind SFR two similar these determined if is check Sm H dwarf late-type the nine ten from of and sample a galaxies of spiral Rate Formation Star The TRFRAINRTSO SGALAXIES DS OF RATES FORMATION STAR .M Hidalgo-G´amez M. A. nttt eea aaies F apsVideira. Campus IFC – UFSC. Catarinense – Federal Catarina Instituto Santa de Federal Universidade etod ieisFıia ae´tcs-CM Universi- CFM, Matem´aticas Ciˆecias - F´ısicas e de Centro α uioiy h anitrs a to was interest main The luminosity. .Maga˜na-SerranoA. 1 .Vega-Acevedo I. , 1 1 n M. and , , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes pia ais agrsml snee nodrto order answer. in conclusive needed more is ab- a sample obtain the the larger with A with relationship radius. as no optical but well magnitude, as blue brightness solute SFR the surface between the relationship a and ga- only per the is SFR of There the properties laxies. global addition, are with In compared SFRs were galaxies. the area Sm However, the in spirals. den- larger dwarf gas same for the with than latter sity the for lower are are per vlto fdafglxe,a ela nteheavy medium redshifts. the intergalactic high in at the as of well contamination as chemical element galaxies, model, the dwarf each about of in understanding evolution RTI our the change of may importance the com- result, to galaxy This bined the quantities. those from on removed depends the varies is of matter most which of galactic rate in baryon the epoch and the mass Besides, halo the supernovae. both the and between rate correlation loss a mass found have pre- very we in for works reported even vious already as on systems, However, role these haloes. massive of major out a matter play pushing may Rayleigh- (RTI) the Instability that Taylor This revealed simulations expected. our be because would the the as on that potential, independent find ubiquitous, gravitational We is winds rate. of formation existence star halo im- the matter and and dark rates mass the loss as mass parameters physical the portant of correlation and simula- the numerical supernovae, tions, hydrodynamic 3D from on based (dSph) study, dwarf the in study galaxies winds we galactic spheroidal work phases triggering this of the evolutionary models In of early current winds. at most galactic lost if increased through is haloes the matter these ga- is visible of detecting explanation Group of possible Local difficulty One the in observed haloes laxies. matter been dark has mass a than low predict of number models larger cosmological much CDM Λ Theoretical 1 Polit´ecnico Nacional. 1 H FET FDR ATRHL ON HALO MATTER DARK OF EFFECTS THE A nvriaeCuer oSl P Brasil. SP, Sul, do Cruzeiro Universidade - NAT sul ueird ´sc ae´tcs Instituto Matem´aticas, y F´ısica de Superior Escuela H ASLS RCS NDWARF IN PROCESS LOSS MASS THE YRDNMCLSIMULATIONS HYDRODYNAMICAL Falceta-Goncalves AAIS EUT RM3D FROM RESULTS GALAXIES: .A Lanfranchi A. G. 2 1 n .Caproni A. and , .O Ruiz O. L. , 1 D. , 1 ABSTRACTS R7(iaae l 01 esuytemorphology the study we 2011) al. ongoing et SDSS the (Aihara of from 7 sample lack DR E+A the an With and formation. formation star star recent gest aaiswt + pcrmhv epBle ab- no Balmer deep and have sorption spectrum E+A with Galaxies 2 ye S 60 Australia. 1670, NSW Ryde, 1 lte oteeio”(aaLpz .A ta.2013, al. a L35). et in A. 433, recently M. MNRAS, (Lara-Lopez, publish mass. editor” were the stellar study to similar “letter this a of of differences galaxies results for drastic The SSFR those and to Z related in is gas the of that Using amount find we metallicities. of counterparts, low GASS and amounts and ALFALFA SSFR metallici- small low show with high will galaxies and gas of massive SSFR In amount while moderate large ties, show metallicities. a will with high gas galaxies and massive gas SSFR metallicities, of contrast, lower low amounts show small and with will SSFR galaxies amount high low-mass large show while a will be- with gas on opposite galaxies of depending follow Low-mass will mass, galaxies stellar haviours. gas, given of that amount a relation the at Z-SSFR the that on shows based model We a catalogues. present public Fast (GASS) Galex Survey Legacy SDSS and (ALFALFA) Arecibo Arecibo Array the Feed from L-band detection Arecibo HI as galaxies, as star-forming well (SDSS) data Survey Sloan Sky spectroscopic and Digital (GAMA) uses Assembly different Mass study and of Galaxy Our from galaxies and for masses. (SSFR) (HI) stellar rate metal- gas formation hydrogen phase star neutral gas specific between (Z), interplay licity the study We .A Lara-Lopez A. M. PCFCSRADHIGSI GALAXIES: IN GAS I H AND SFR SPECIFIC AHUP P Brasil. SP, EACH/USP, utainAtooia bevtr,P o 1,North 915, Box PO Observatory, Astronomical Australian AAYADMS SEBY(GAMA): ASSEMBLY MASS AND GALAXY H ONCINBTENMETALS, BETWEEN CONNECTION THE + AAISI H DS STELLAR SDSS. THE IN GALAXIES E+A OUAINADMORPHOLOGY AND POPULATION H -SRRELATION Z-SSFR THE .Leiva R. H α 1 .M Hopkins M. A. , n [ and 1 team n .Galaz G. and OII msin hssug- This emission. ] 1 1 n GAMA and , 179 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes hs nidpneteeto ooaini mini- minimum a the is with associated corotation formation of star Besides of effect mum gradients. the independent of an slope the this, in break which a at is radii there the is and correlation radii good corotation between very found A literature. the Oxygen in of available there gradients which abundance for of measurements and which are radius, galaxies, corotation of known sides sample a coro- have two at a observed investigated the gas We of on tation. void the directions ring-shaped of the opposite The by result in and the gas way. is of independent regions flow two an the that in so between evolve other, barrier sides the from corota- two one in the outside isolated galaxy and are a which corotation tion) coro- of (inside the disk regions because the metal- two is separates in step resonance step This tation abrupt corotation. abun- an the at also of licity slope one but the Way, gradient, in Milky change dance a the only radii. including not larger observes at galaxies, rising several or flat In in- become the and in regions decrease ner belief. usually common gradients recent metallicity a The to find contrary the we long-lived, which estimate be structure, to to arm spiral tool present the chemical a of the even age in on is and effect gradients galaxies, Its abundance spiral Galaxy. of our disks of particular, the in of role evolution important an the plays resonance corotation The 1 to included parameters be Additional to fitting. need the improve past. extinction internal the formation dust in like star Gyr increased 2 an around indicating spectra re- galaxies. the E+A is the mechanism of part interaction least scenario the at the for z, sponsible with low consistent at seems where, last the ga- interacting of laxies, overpopulation an and galaxies like (2003). Charlot his- & formation Bruzual star from the models and fitting data tory 1 Zoo Galaxy with 180 eCie iun akna46,7246Mac´ul, Santiago, 7820436 ([email protected]). Chile 4860, Vicu˜na Mackenna Chile, de .C Junqueira C. T. EOAC NTESCLREVOLUTION SECULAR THE IN RESONANCE .R .Lepine D. R. J. nttt eAto´sc,PnicaUiesddCat´oli Universidad Pontificia Astrof´ısica, de Instituto h trfrainhsoy(F)fisms of most fits (SFH) history formation star The disk and spiral of underpopulation an found We H OEO H COROTATION THE OF ROLE THE FDSSO PRLGALAXIES SPIRAL OF DISKS OF 1 1 .S Dias S. W. , .SaaoJr. Scarano S. , 3 n .Andrievsky S. and , 2 .A Barros A. D. , ABSTRACTS 1 , ca 4 ahns.Silaohreeti h cteigof radii. migration galactic scattering their different causes the to which is resonance, the effect by another star-formationstars and spi- Still wells the potential feeds machines). as gas (seen interstellar arms ral the which at velocity dsaNtoa nvriy dsa Ukraine. Odessa, University, National Odessa 4 Brazil. jub´a, Itajub´a MG, 1 Brasil. 2 Spain. 1 3 S˜ao Brazil. Cristov˜ao,DFI/CCET, SE, Brazil. SP, 2 S˜ao S˜ao Paulo, Paulo, de Universidade AIAi pcrsoi uvyo 0 eryga- nearby 600 of (0.005 survey laxies spectroscopic a is CALIFA 1 a,alrerneo ass(0-2M (109-12 masses of range Mr large to a mag the mag, -23 covering -18 = = galaxies Mr for from data diagram of color-magnitude set useful very and ihanwvrino h tigcd STARLIGHT. code fitting filters the GALEX of UV version two new synthesis the a the spectral plus with full range in optical a extent the perform at lesser We a range. to popu- optical contribute stellar young which the lations, ad- about provide information that data ditional break to including order degeneracies, in range these mission ultraviolet GALEX the the with in obtained spectroscopic data CALIFA photometric combine with data we stellar the So of properties population. physical the of estimation age-metallicity- in uncertainties are produce which there degeneracies, However, extinction 4000 tracers. the useful the and contains series it Balmer because for ideal populations is stellar sample CALIFA galaxies. studying the of of range to properties spectral us resolved The allow spatially and Sc), the to obtain E (from types morphological .L´opez-Fern´andezR. i Fernandes Cid H ORGAIAINLACSURVEY ARC GRAVITATIONAL SOAR THE nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto nttt eFıiaeQ´mc,Uiesdd eea eIt de Federal Qu´ımica, F´ısica Universidade e de Instituto nttt eAto´sc eAdlcı,CI,Granada, CSIC, Andaluc´ıa, de Astrof´ısica de Instituto nvriaeFdrld at aaia Florian´opolis, Catarina, Santa de Federal Universidade nvriaeFdrld egp eatmnod F´ısica de Departamento - Sergipe de Federal Universidade eateto srnm n srnmclObservatory, Astronomical and Astronomy of Department TRFRAINHSOYO CALIFA OF HISTORY FORMATION STAR AAISI H PIA N UV AND OPTICAL THE IN GALAXIES < z 2 .P´erez E. , < .3.CLF rvdsaunique a provides CALIFA 0.03). 1 .M Gonz´alez Delgado M. R. , 1 n .Garc´ıa Benito R. and , ra,aogother among break, A ˚ ⊙ and ) 1 R. , icas, 1 a- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes lsesi w esititrascnee at centered intervals Gravita- redshift SOAR two 47 in imaged the survey clusters The of (SOGRAS). Survey results Arc first tional the present We and 4 3 Sul. do Grande 2 1 nevl mgswr bandi the in obtained were Images interval. ad ihamda eigo 0 of seeing median a with bands 6 5 S˜ao Paulo. de Universidade 8 7 Laboratory. tor h aefrtesrn esn aueo h candi- the of survey. nature this lensing in strong found dates the for case the meeting al.). same this et are to (Cibirka masses submitted follow-up poster dynamical a spectral derived in presented the a and of Gemini analyses with The mass their on distribution. Fi- constraints providing systems, light. to best techniques cluster the inversion lensing galaxy strong of apply we 2012), subtraction nally, al. the et (Furlanetto for ArcFitting (Bom and and 2012) method al. Mediatrix et the apply including arc We gravitational candidates, the characterize Stripe-82. to in methods several surveys other with the synergy exploiting etc.), X-ray clusters, Zel’dovich bands, Sunyaev several and in photometry (spectro- redshifts, samples clusters scopic complementary the with of lensing galaxies matches cross and strong and sample, best of galaxy catalogs 6 the morphometric results the and first photometric including the systems, survey, present We the are them of footprint. of SDSS all the and in Sky region Digital Stripe-82 Sloan (SDSS) the sur- Survey within the located of are Most clusters vey filters. these in respectively, arcsec, .Makler M. .Caminha B. Hao nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto eatmnod srnma nvriaeFdrld Rio do Federal Universidade Astronomia, de Departamento etrfrPril srpyis em ainlAccelera National Fermi Astrophysics, Particle for Center aoa´roItrnttcoa ee-Astronomia. de Laborat´orio Interinstitucional F´ısicas. Pesquisas de Brasileiro Centro nttt ainld eqia Espaciais. Pesquisas de Nacional Instituto eateto hsc,Uiest fMichigan. of Observat´orio University Nacional. Physics, of Department Pereira H NIOMNA RPRISOF PROPERTIES ENVIRONMENTAL THE Brandt eprflo-piae ihGmn strengthen Gemini with images follow-up Deeper z 6 0 = AAISPOE YMARKED BY PROBED GALAXIES .M McKay M. T. , 1 1 . 1 .R .Bom D. R. C. , .F Neto F. A. , 5 agtn h ihs lsesi each in clusters richest the targeting 55, .Furlanetto C. , 1 .Cypriano E. , .A .Maia G. A. M. STATISTICS 7 .A .d Costa da N. A. L. , 3 .Estrada J. , 1 2,3 .P Lima P. M. , 4 .Cibirka N. , .X Santiago X. B. , 3,8 . 3 0 83, 6 .Lin H. , . g 6ad0 and 76 1,5 4 ′ .E S. E. M. , , .H. C. , 3,8 r z ′ 6 and , 2,3 0 = and J. , G. , ABSTRACTS icas, . . 71 27 i - ′ 1 tla as(aoszs hr h orltosap- correlations the dramatically. in where more range sizes) pear wide (halo a hand, span mass other regions stellar density the low On in galaxies clustering). cor- average (marked = clustered relation equally conclude are We galaxies massive by objects, dominated mean. clusters, galaxy the nearby in to that show relative don’t correlations difference halos the massive any where to than clusters, pairs in galaxy is found close instance, in for halos individ- ual to mass, associated implies environments stellar to This sensitive of more clustering regions. the dense that are local to mean the compared the in to stronger relative regions correlations the density mark to universe, low respect For with quantify them to environment. of as importance well relative as lu- the masses, like stellar re- variables and to for minosities powerful trends are environmental statistics produce marked that environment. show large-scale be- We and correlations attributes the these quantifying mass, tween directly stellar and more luminosity thus like particular by properties, weighted where from galaxy was 7, galaxies drawn Release of Data sample clustering Survey the galaxy Sky Digital a method- Sloan to This the applied function. based was correlation ology properties marked galaxy the driving on in role environment the investigate work,of to this method statistical In a envi- applied evolution. the we galaxy study to on wants effects one ronmental if have account must into objects that taken properties be these population stellar in However, and particles physical point analysis. as treated clustering generally are Galaxies lblrcutrlmnst ucin a l UCDs the all of Can tail function. bright luminosity the cluster follows luminosity The globular the UCDs whether 1. of test distribution introduced to recently aspects. allows a two that - summary,quantity on UCDs overall of particular brief frequencies in specific a focus After truncated will tidally I both. universe, or, the mas- in galaxies, most clusters the either star be to sive ga- believed dwarf are and UCDs clusters laxies. star dwarf between defin- ultra-compact systems interface stellar the on of ing class review new a a (UCDs), give galaxies to propose I nvriaeFdrld at aaia Brazil. Catarina, Santa de Federal Universidade E LS FGLXE (?): GALAXIES OF CLASS NEW A LR-OPC DWARFS ULTRA-COMPACT .Mateus A. .Mieske S. 1 1 181 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 1 ga- progenitor 1 UCD of holes relicts black fossil central laxies? the be massive of would to variation due that a ele- maybe, matter, The or due dark IMF, they clustered 2. Are highly UCDs. to of clusters? ratios star M/L dynamical bright vated as explained be 182 4 3 2 ([email protected]). Chile Chile, 6 Argentina. 5 Chile. Chile, de USA. La Astrof´ısica de de Instituto 7 and Argentina. Plata, Plata, La de Nacional dad uin ihosrainldt,tebs rx can proxy best found. the distri- be data, mass observational halo with host and butions de- recov- mass the the stellar Comparing redshift, from ered proxy. derived each for properties sources galaxy tected the as of counts, as recovered effects well the the in study process we observational differ- a the this perform the With we by extraction. maps, source given sub-millimeter fluxes into catalogs proxies and the ent positions turning galaxy After of reproduced. number combined are observed the counts ALMA assum- that bright-end so plus fluxes, relationship LABOCA sub-millimeter monotonic model their a the ing for by given proxies properties vari- as choose galaxy We physical model. ous light-cones semi-analytic now- a through from the approach drawn to Matching” “Count analogy perform a in we approach, the matching and abundance exploring standard SMGs, of aim of the With properties mul- sources. from fainter emission by tiple comprised single- are by telescopes brightest detected dish the (SMGs) that galaxies show sub-millimeter South Field Deep Extended Chandra the of observations interferometric Recent .M Mu˜noz Arancibia M. A. ONSI EIAAYI OE:THE MODEL: SEMI-ANALYTIC A IN COUNTS eateto hsc n srnm,RtesUniversity, Rutgers Astronomy, and Physics of Department etod sr-neirı,PnicaUiesddCat´o Universidad Astro-Ingenier´ıa, Pontificia de Centro a-lnkIsiu ¨rRdosrnme Germany. f¨ur Radioastronomie, Max-Planck-Institut Germany. f¨ur Astronomie, Argelander-Institut osj ainld netgcoe in´fia T´ecnic Cient´ıficas y Investigaciones de Nacional Consejo nttt eAto´sc,PnicaUiesddCat´oli Universidad Astrof´ısica, Pontificia de Instituto autdd inisAto´mcsyGeof´ısicas, Univers Astron´omicas y Ciencias de Facultad S Chile. ESO UMLIEE AAYNUMBER GALAXY SUBMILLIMETER Padilla CUTMTHN”APPROACH MATCHING” “COUNT Kurczynski 1,4 .A Cora A. S. , 7 n .N Ruiz N. A. and , 1 .P Navarrete P. F. , 5,6 .Gawiser E. , 8 7 2,3 P. , .D. N. , ade ca ABSTRACTS lica as, i- rw ihteices ftepyia radius. physical the of increase the the groups with non-Gaussian that grows as show classified results systems Our 2-4 of number in radius. group physical the of its center times checked the was to distance gaussianity the of varying as behavior classified is The hy- group the proveGaussian. the system, tests the confirms other of test all normality and the Dip unimodality the the of When pothesis test. D’Agostino Dip Mises, and tests: Cramer-von statistical Jarque-Bera, Shapiro- following Wilk, the Kolmogorov-Smirnov, classi- on This Anderson-Darling, based distributions. is based velocity fication not) galaxy or their evolved on (dynamic non-Gaussian and (M mass o ahgopw siae t rprissc as such properties ( its Mpc. dispersion 4 estimated of velocity we radius a group in the each members For using 8 least (2012) galaxy at 105 with al. groups selected We et Gerke Method. by Voronoi-Delaunay sam- obtained This in- was (EGS). Strip ple (DEEP2) Groth Extended 2 the cluding Probe Deep groups the Evolutionary galaxy of release of Extragalactic data sample fourth a the from analyze constructed we work, this In rsn h rtrslso u praht td the we study work to approach this our In of results first galaxies. the of present record for- evolution the fossil and with a mation associated par- processes are physical is several they galaxies of since in interesting, populations stellar ticularly of study The iaeEtda eSnaCu,RdvaJreAao Km Amado, Jorge Ilh´eus-BA, Rodovia Brasil. 45662-900, Cruz, Salobrinho, Santa 16, de Estadual sidade RPRISO AAISADGOP AT GROUPS AND GALAXIES OF PROPERTIES 2 ([email protected]). Brasil Rio Janeiro-RJ, Sa´ude, Antˆonio, 20080-090 43, Pedro Ladeira Janeiro, 1 inld C´ordoba, Argentina. de cional 8 .S Nascimento S. R. aoa´rod srfıiaT´rc bevcoa,Un Astrof´ısicaLaborat´orio Observacional, Te´orica de e bevtoi oVlno nvriaeFdrld i de Rio do Federal Universidade Valongo, Observat´orio do bevtroAto´mc eCodb,UiesddNa- Universidad C´ordoba, de Astron´omico Observatorio OUAIN IHNGALAXIES WITHIN POPULATIONS H ITIUINO STELLAR OF DISTRIBUTION THE 200 .M Novais M. P. .W locasf h rusa Gaussian as groups the classify also We ). 1 .A .Lopes A. A. P. , σ Ribeiro ,pyia ais(R radius physical ), Z 1 < n .Sodr´e Jr. L. and 1.4 2 1 n .L B. L. A. and , 1 200 and ) iver- de XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes hsapoc seetv n ilb xlrdand explored that be show works. will results future and first in effective improve This is approach popu- center. this stellar the young while in have galaxies, lations to spiral late seem and galaxies spiral elliptical in from out types evolve different to to tend of inside populations galaxies stellar 15 the of that sample show analy- small pixel-by-pixel a how The of on sis evolve. hints are and bringing grow populations galaxy, galaxies stellar a different within esti- the distributed quantitative how conventional obtain the on to to mates allowing respect with fitting, forward profile step a be to the aims and approach Indices Our Gini vari-Euler-Poincar´e including characteristic. a of tools, with statistical distribution investigated of ety then The are populations galaxy. these dis- each their and inside pixel-by- populations tributions stellar obtain the to of proxies (PCA) pixel analysis component using pal ga- are inside We populations laxies. stellar of distribution spatial nvriaed ˜oPuo u oMta,12,Cdd Uni- SP. Cidade Mat˜ao,versit´aria, - 1226, S˜ao do Paulo Rua S˜ao Paulo, de Universidade 1 ieu ihauiu potnt oda analogies draw to pro- opportunity they unique LBGs, a than with 0.2) us signifi- vide At (z Galaxy redshifts lower the satellite. cantly (GALEX) by Explorer uncovered Evolution recently galaxies were luminous UV (UVLGs) These (LBAs). Lyman- Analogs as break denominated hence high- are and with LBGs luminosity) redshift brightness, super- surface (mor- phology, UV-selected properties many We low-redshift share that of starbursts instruments. compact sample current of a sensitivity study lim- the are galaxies by distant morphol- ited these the of of kinematics in and studies objects galaxies ogy detailed important massive However, them the study. making of of pro- universe, part the local large be the may a galaxies in of of these genitors peak rates that formation its suggest star through LBGs The going activity. formation was star time universe a at the galaxy when starburst typical the of represent that population ( a objects are distant (LBGs) galaxies Lyman-break .S Oliveira S. C. IHRDHF YA-RA GALAXIES LYMAN-BREAK HIGH-REDSHIFT nttt eAtooi,Go´sc Cieˆncias Geof´ısica Atmosf´er e Astronomia, de Instituto O-ESITCMATU LUMINOUS UV COMPACT LOW-REDSHIFT TRUSS ORT UNDERSTAND TO DOOR A STARBURSTS: 1 .Men´endez-Delmestre K. , z ∼ Gon¸calves ugriz )slce trs-rm UV rest-frame at selected 3) antdsadprinci- and magnitudes 1 1 n .S. T. and , ABSTRACTS icas, ldn bu 4 bet,as oelmnu than luminous more an also in- objects, from, 24M galaxies about neighboring cluding the to count used and was extract SDSS-DR7 the of catalogue photometric aisfrwihw aeamaueeto environ- of measurement a density. ga- have mental target we 527,074 which leaving for galaxies edges, laxies avoid survey We tar- the target). to the redshift the close a of around and that radius around Mpc apparent range an 1.5 to of (translated within get distance galaxies all absolute counts dis- code an a The as serve estimate. to tance available was redshift photometric 1 E 08-9,Rod aer,R,Bai (carolyne13@astro Brasil RJ, ufrj.br). Janeiro, de Rio 20080-090, CEP a aaisi h oa nvreadt Bsi the in LBGs to and universe. universe distant local differ- nor- the and to in galaxies relative similarities mal populations the two these explore and between to ences masses order stellar in derive ages to of galaxy of (SED) individual process distribution each the energy in spectral compact the are 40 analyzing we UVLGs for supercompact photometry optical and and Based Ks, H, UVLGs. J, supercompact on than galaxies, extreme normal less than but magnitude brightness of pop- orders surface two wider with or the one UVLGs, to compact work of this ulation extend now We Observatory, the Campanas Chile). on (Las instrument Telescope Fourstar obser- Baade on 6.5m the based with LBAs photo- taken of sample near-IR vations a the of undertaken analysis metric distant have the We in observe universe. we activity to formation lead in star that the conditions study astrophysical and the detail counterparts great high-redshift their with bouemgiueo 1 nteSDSS the in -19 than of luminous magnitude more absolute the and red- 0.30 from and with se- 0.03 galaxies SDSS-DR7 between we shifts the 666,387 targets, of of catalogue As sample spectroscopic ga- large neighboring galaxy. developed a of target lected we number a galaxies, the around counts of laxies environ- that sample the code large of a re- a density and of the homogeneous ment of a obtaining measurement of liable aim the With bevtoi oVlnoUR,LdiaPdoAntˆonio, Pedro 43 Ladeira Observat´orio Valongo/UFRJ, do .A Ortega-Minakata A. R. AAIS EUT N COMPARISONS AND RESULTS GALAXIES: r EST FTEEVRNETOF ENVIRONMENT THE OF DENSITY bn bouemgiueo 1,frwiha which for -19, of magnitude absolute -band NAPOC OMAUIGTHE MEASURING TO APPROACH AN IHOHRMEASUREMENTS OTHER WITH n .Andernach H. and 1 .P Torres-Papaqui P. J. , 1 r ad The band. 1 183 , . , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ieatvt fglxe n hi min density. ambient their and galaxies emission- of of activity types line the different the study the test between to to relationship and results our relation use density to morphology–local of aim members We of clusters. compilation Abell a a from to galaxies also from of and galaxies sample galaxies, of isolated sample of of a catalogue control 2MIG to the a it apply As we cat- method, galaxies. MaxBCG our cluster the brightest environ- in of those the as alogue of such galaxies, density of the ment of measurements other aii,AeiadsAtoats15,12700S˜ao Jos´ ([email protected]). 12227-010 Brazil SP, 1758, Campos Astronautas dos dos Avenida paciais, 1 (rene,papaqui,[email protected] mx). Mexico Guanajuato, 36000, 1 184 fporsint h piu ouino multi- a of solution optimum terms model. the parameter in to robust with progression out very carried of method, is Sampling values Nested parameter the best pinpoint- the The of uncertainties. ing exploration realistic further provide to for to space, interest and parameter of the regions of overview a constrain an of looks for excess method ideal in Carlo like Monte parameters when Chain free Markov complex the of pretty dozen, number be can a model have a we of fig- which the merit for parameters of landscape ure of the Since set Galaxy. limiting the best describes several the using over of magnitudes effects the and investigate to uncertainties, approach also their conservative and values a parameter used derive have galac- We the the in plane. of used region tic is complex the the method is including counts sky, It star whole the impor- Galaxy. that the most time first of the parameters sky, structural whole J, tant the in of over data model lines-of-sight 2MASS K the the and of the and version H L´epine (1993) modern to & a approach Ortiz uses counts new It star a the method. via work parameters galactic this of derivation in present We eatmnod srnmı,Uiesddd Guanajuato, de Astronom´ıa, Universidad de Departamento ii˜ od srfıia nttt ainld Pesquisas de Nacional Astrof´ısica, Instituto Divis˜ao de epeetorrslsadcmaete to them compare and results our present We AAYMDLI INFRARED IN MODEL GALAXY S oetmt,bsdo eua rdof grid regular a on based estimate, to .Polido P. 1 n .Jablonski F. and 1 ABSTRACTS Es- to. e h iecl o ahwv akti fteodrof order the of is 10 spirals. packet some wave trailing each wound for tightly and timescale The as amplitude away maximum fade their finally, trail- reach into patterns, wound waves ing tightly leading the as open Afterwards, to amplified unwound structures. be and spirals to leading ef- begin wound the Indeed, waves show mechanism. density amplification to the swing applied the also of speeds. char- fects is pattern bar analysis and quantify 2D strength, Fourier to present length, analysis We as Fourier acteristics 2. 2D Gadget and for Hern- using evolved 1D spherical were Gyr models a 5 The bulge, approximately used. a was having profile Spitzer’s quist models NFW In a disk, and direction halo. exponential vertical were the in with models an sheet isothermal simulations The with SPH constructed of models. particles results multi-million the present We rmvr eet( luminosity recent bolometric esti- very the an from to epochs contribution different the in mate rates formation for star (PDFs) the functions pos- obtaining distribution by probability systems terior star these the of histories reconstruct In- We forming Luminous (ULIRGs). Ultra of Galaxies counterparts redshift frared local high the and in intermediate of formation understanding star the massive in fundamental techniques. are Bayesian results state-of-the-art and Our using models systems transfer these radiative of spectra IRS eselrMdu rsue opcns Parame- Compactness In- ter Metallicity, Pressure, as Medium such terstellar parameters physical derive tion aigtedrvdPF ihpriua spectral particular with PDFs com- By derived cases. the some in paring significant Hydro- is Aromatic which Polycyclic carbons, of contribution the and 2 1 epeetamdifae td fasml f19 of (z sample local a the of in study galaxies Starburst mid-infrared a present We .F ao P. Ramos F. A. nvriaed aed Para´ıba, Brazil. do Vale do Universidade Mexico. INAOE, HSCLPRMTR FGALAXIES OF PARAMETERS PHYSICAL C A N PRLAM YAISIN DYNAMICS ARMS SPIRAL AND BAR f IHSA OMTO THROUGH FORMATION STAR WITH DR P rltdt h uthaigflx,PRFrac- PDR flux), heating dust the to (related 8 I-NRRDSDMODELS SED MID-INFRARED Higuera-G. years. UEIA SIMULATIONS NUMERICAL n Extinction and .Puerari I. 1 .R Mart´ınez-Galarza R. J. , < 3 1 n .A Quintero A. S. and , y)sa omto events, formation star Myr) 1 n .Rodrigues I. and A V yfitn h Spitzer- the fitting by < .)uies.We universe. 0.2) 2 4 2 .A. M. , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes pce ie[eI n NII,adteH the atomic and [NeIII], of and emission [NeII] nebular like the species as such signatures, ini trus aaiswt h nenlphysics internal the ISM. with the forma- of galaxies star of Starburst pattern in global tion the relate also we tures niu ro1 oatita uba ´xc ..72840. M´exico C.P. Puebla, Tonantzintla, 3 1, Erro Enrique 1 1 in´ fia iddUiestra ´xc,DF,CP 045 C.P. M´exico, D.F., Universitaria, Cient´ıfica, Ciudad 2 Brazi Gerais, Minas ([email protected]). , Na¸c˜oes, Itajuba das 37.504-364 Bairro tet S5,Cmrge A018 S (jmartine@cfa. USA 3 02138, MA harvard.edu). Cambrigde, MS-51, Street, 2 ([email protected]). Colombia Bogot´a D.C., te h MR fNC57 ntecs fmore of case the in 5278 mass. NGC disk of 30% RC DM the fitted n lota h oe ( cored the that also and ooba oo´ .. ooba([email protected] Bogot´a Colombia Colombia, D.C., 4 co). ([email protected]. Colombia Bogot´a D.C., Colombia, de te h MR fNC57 ntecs fdisk of case the in 5278 better NGC halo of DM mass RC HH DM the that the re- were fitted main work The this (EH). of Einasto sults and Frenk ha- (NFW) Navarro, (DM) White (BH), and Burkert matter RC (HH), dark matter Hernquist of dark los: profiles the the density only four from fitting with disk and 5278, baryonic RC NGC observed extracted of the decomposition subtracting the (RC) performed curve We 5278 rotation models. NGC synthesis of stel- 2D population and lar disk observations the photometric stellar obtaining band broad the distribution 5278, using of mass NGC distribution the galaxy mass spiral on the study of the extended We .Repetto P. aoaoi ainld srfıia .EtdsUio,1 Unidos, Astrof´ısica, Estados de R. Nacional Laboratorio TLA OUAINSNHSS DARK SYNTHESIS: POPULATION STELLAR eatmnod ´sc,UiesddNcoa eColombia de F´ısica, Nacional Universidad de Departamento nttod srnma NM iciod aInvestigaci´o la de Circuito UNAM, Astronomia, de Instituo nttt ainld Astrof´ısica de Nacional Instituto bevtroAto´mc ainl nvria Naciona Universidad Astron´omico Nacional, Observatorio avr-mtsna etrfrAtohsc,6 Garden 60 Astrophysics, for Center Harvard-Smithsonian EEMNTO FHL OCCUPATION HALO OF DETERMINATION eatmnod ae´tcs nvria ainlde Nacional Universidad Matem´aticas, de Departamento .Rodriguez F. IKMS-OLGTRTOTHROUGH RATIO MASS-TO-LIGHT DISK M ATRCNETO G 5278 NGC OF CONTENT MATTER d 5 = 1 .Mart´ınez-Garc´ıa E. , . 6 × 1 .A Sgr´o A. M. , 10 DISTRIBUTION .F Gabbasov F. R. 10 M ⊙ < n n es3%o hsvalue, this of 30% less and 1 piayEetoia,Luis , Electronica y Optica )E Mhl better halo DM EH 4) ´ n .Merch´an M. and , 2 3 .Rosado M. , 2 tempera- 3 and , 10. ABSTRACTS 1 54, o). n , l l ino h trus aayM2 edtc line detect HCN, We tracers gas molecular HCO M82. dense galaxy the from starburst emission the of gion osuyti ffc ehv band3m maps mm 3 ( obtained gas have dense we effect of evolution. this from galaxy study gas in To role remove How important winds an these plays stars. galaxies amount form inner which to the in material from and available intergalactic gas to the removes the galaxies regions, process reaching of This even regions medium. regions, inner energy outer the carrying the from of matter responsible and are winds Galactic osdrbeaon fHCO of amount considerable a ard 5,Codb,X0BR retn (fa- Argentina X500BGR, C´ordoba, 854, [email protected]). C´ordoba. de Astro´omico Laprida Observatorio (UNC-CONICET), 1 h O nohrrne faslt magnitudes. absolute of ranges calculate and other (2008) in al. HOD com- et the Yang DR7, of Survey results the Sky to Digital pare Sloan the sub- in background applying traction implement we by this Finally, results compare method. obtained our We the con- HOD. with groups HOD imposed fiducial and an galaxies with of structed catalogs procedure, mock the ranges used evaluate more To we is in magnitudes. this HOD absolute of the of advantage estimate to main possibility the the galaxies, from of information photometric catalogs allows with This catalogs groups galaxy from this. of information to spectroscopic belong combine pro- to to be- for seem or but, effects, front galaxies), jection in (background It are group calcu- that the (HOD). to hind galaxies Distribution method subtract new Occupation of consist a Halo propose the we late work, this In h aso oeua yrgnotietecentral the is outside outflow. Hydrogen starburst the molecular in of entangled mass is The gas dense indi- the disk, that star-forming cating central the bellow and above aeo aatcscales. formation star galactic star observed on and average rate the gas the dense drives between is what law It formation gas dense edges. of the star- amount towards gas the less the of and center that the burst dense revealing towards of concentrated disk, more amount starburst is the the of over variations gas show also maps eta trus is starburst central .Salas P. nttt eAtoo´aT´rc Experimental y Te´orica Astronom´ıa de Instituto + N,C,HC CS, HNC, , 1 .Galaz G. , H ES A NM82 IN GAS DENSE THE M n out crit .Herrera-Camus R. ≈ > M 1 .Salter D. , 3 3 disk 10 n C and N ± 4 1 ≈ cm × 8 − 10 ± + 3 6 2 6 ntecnrlre- central the in ) .Ormp reveal maps Our H. 2 .Bolatto A. , msinextending emission × M 2 ⊙ 10 hl nthe in while , 6 M ⊙ These . 2 and , 185 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ne,Uiest fSa al,Bai (jullian.santos@us Brazil S˜ao Paulo, of University ences, 1 1 186 h orlto ewe tla asadgas-phase ( and abundance mass oxygen stellar between correlation The eglci a.I atcul fyas the years, of couple last secular In its in- gas. and on galaxies tergalactic forma- depends other with star turn interaction its and in evolution by which driven history, is is Chemical tion trend galaxy this a evolution: of in galaxy enrichment scatter on and dependent slope strongly The decades. for aeAtooy nvriyo ayad olg ak MD Park, USA. College 20742, Maryland, of University Astronomy, Wave Chile. 2 Santiago, 782 Macul, 4860, Vicu˜na0436 Mackenna Av. Chile, Cat´olica de versidad h hresaeo As paety nosand anions cations. Apparently, over check favored PAHs. to are used of neutrals be state could charge features the PAH the obser- In the of applications, vations models. cosmological energy the dark test to redshift to addition high used for be way could this objects in instru- derived satellite ages The and ments. ground future with for cal- both both our observations benchmarks that some expected provide We culations galaxies. redshift high of ino h upto h aay npriua,the particular, In galaxy. 11.3/7.7 the ratio of line emis- output stellar the and on AGN assessment sion of the for allowing importance to relative the addition for- star in galaxies, sig- rate, of good mation stage a evolutionary the provide star of lines nature PAH distinguishes to The associated It clouds regions. forming molecular molecules. the silicon PAH ISM and diffuse also carbon high and considers at model grains, lines PAH The of formation redshifts. evolu- the galaxy studied for we tion, models chemodynamical in Based A IE THG ESITA GALAXY AS REDSHIFT HIGH AT LINES PAH OMTO AERLTO NE THE UNDER RELATION RATE FORMATION nttt eAto´sc,Fcla eF´ısica, Pontificia de Astrof´ısica, Facultad de Instituto eateto srnm n aoaoyfrMillimeter- for Laboratory and Astronomy of Department nttt fAtooy epyisadAmshrcSci- Atmospheric and Geophysics Astronomy, of Institute .Schlickmann M. .H .Santos B. H. J. H MASS–METALLICITY–STAR THE Fernandes TRIH MICROSCOPE STARLIGHT VLTO MARKER EVOLUTION M sago akro h age the of marker good a is m 1 1 n .Stasi´nska G. and , 1 .Vl Asari Vale N. , – Z n .C .Fria¸ca S. C. A. and eain a enknown been has relation) 1 .Cid R. , 2 1 M p.br). ABSTRACTS Uni- – Z - o ie bevdadlbaytmlt aa hsis This data. template library and observed given module: (PDFs) for fitting functions Bayesian distribution probability 2) calculates libraries. template theoret- and ical empirical library generates template A module: (Ma- our 1) generation Analyser build modules. three to Magnitudes has which decided gAl), code: we scale), SED-fitting petabyte own the to up be properties data. physical to photometric invaluable from on galaxies be information of will retrieve it to DES, able and J-PAS BRA, eomn frdhf uvy sn h technology ( the filters using ultra-narrow de- surveys of recent the redshift to with of However, properties velopment detail. our physical of hinders degree galaxy’s a and a such limited recover more to the much ability on is photometry, hand, Braad-band other for- histories. main star the and mation thus enrichment abundances, They chemical gas-phase sources, content. derive radiation stellar to the lines, us about gas allow absorption us ionised plus tell the continuum which about the us and tell content, features: which two mainly lines, find emission can one spectra, galaxy On trt lc ue ase,91 edn France. Meudon, 9210 Janssen, Jules Place eterot; Brazil. 2 Florian´opolis, SC, Catarina, Santa 1 aaysfl trfrainhsoy n o only not and history, SFR. formation recent its star full galaxy’s a aini oedtie fashion: detailed more a re- in mass–metallicity–SFR lation the the exploring prelimi- use results some nary who present authors also We by catalogue. reported similar MPA/JHU ones recover we the that as find We results group. our by gether nlgto the of relation light accept- mass–metallicity–SFR in are the gas informing explore of We outflow redshifts, able. and high infall evo- of and tight. galaxy models low very which on in be constraints models to strong lution puts reported mass–metallicity– result been This This has Myr. relation 10 last SFR the third in as a formed H (SFR) of rate the function by formation calibrated star a recent as the studied parameter: been has relation .Schoenell W. UH bevtied ai,CR,UiestePrsDi- Universit´e Paris CNRS, Paris, de Observatoire LUTH, eatmnod ´sc F nvriaeFdrlde Federal Universidade - CFM F´ısica - de Departamento oiae yti aaaaace(hc goes (which avalanche data this by Motivated AA:ANWTO OANALYSE TO TOOL NEW A MAGAL: AAISPOOERCDATA PHOTOMETRIC GALAXIES 1 .Ben´ıtez N. , S S–TRIH aaaeptto- put database DSS–STARLIGHT α uioiy hc rcsstars traces which luminosity, ≈ 100 1 n .CdFernandes Cid R. and , ) uha ALHAM- as such A), ˚ s algtrecovers tarlight 2 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes esrdb ud ta.(2006). al. et masses Bundy COSMOS by when like measured dex results AL- 0.2 previous of the to accuracy to comparing an with code masses mea- the can stellar we sure apply that show we and catalog Also, survey less HAMBRA of dex. precision 0.3 a than with ages, extinctions stellar and measure metallicities can sam- we our galaxies for simulated of that ple show We recover system properties. to filter physical galaxy their survey tried mock ALHAMBRA and a (http://alhambrasurvey.com) the created have for we sample MagAl, by tained also is are data tests 3D preliminary manage few shown. a to and module developed fourth being output A large the files. mod- from PDFs result-analyser analysis A data streamlines 3) red- ule: photometric (2000). measure Benitez to by shifts method the to similar F´ısica. Espa˜na,2 (william@iaa. Granada, E-18008, tronom´ıa, s/n, 1 idti oki opoueraitcsetafrtests for spectra realistic produce to be- is motivation work main this dex hind The 0.24 lines. equivalent and emission 0.12 different the between for accuracy and an components with widths, principal four between the relations functional provided analysis software which regression same Eureqa, symbolic con- The the with the performed between widths. was equivalent correlation strong and a tinuum is demonstrating there results, the that excellent of with neu- widths equivalent lines, artificial the emission an estimate train and to to network spectra components ral 10 continuum Analysis to synthesized up Component We used the Principal spectra. of a galaxy (PCA) also, of region done, optical have de- the usually in lines be- tected emission correlations prominent strong most the indeed tween are there that corre- information lation, maximal the and as such correlation tools distance statistical star- using and Starlight show, 70,000 We the spectra with software. than SDSS performed synthesis more S/N spectral of high with with sample galaxies a forming for emis- correla- optical lines the of widths sion of equivalent the analysis between quantitative tions a present We nvriaeFdrld at aaia eatmnode Departamento Catarina, Santa de Federal Universidade nttt eAto´sc eAdlcı,Goit el As- la de Glorieta Andaluc´ıa, Astrof´ısica de de Instituto oivsiaeterlaiiyo eut ob- results of reliability the investigate To AADIE PRAHT THE TO APPROACH DATA-DRIVEN A .SdeJr. Sodre L. MSINLN RPRISOF PROPERTIES LINE EMISSION TRFRIGGALAXIES STAR-FORMING 1 n .Abra Sirico Albernaz A. and 1 ABSTRACTS es). fdt euto ieie ftenwgnrto of PFS/SuMIRe. generation and J-PAS new like the surveys, of galaxy pipelines reduction data of 1 ieo;PaeJlsJnsn910Muo,France M´exico. Meudon, 04510 M´ex. D.F., 70264, 92190 Postal M´exico, Apdo. de Janssen Jules 2 Place ([email protected]). Diderot; 1 aial itntsseso ie r dnie in identified kine- are Four lines of region. systems circumnuclear distinct the matically in nar- with lines zone nuclear low-ionization row dense the less in a dense and lines very region, broad a with distinguish zone spatially high-ionization can we From maps, properties. the 996 kinematic Mrk their with in correlated regions are the different that of imaging properties limit ionization density new a electron by of and technique maps, ratio and intensity emission-line Mrk galaxy (BCD) dwarf 996. compact of blue (GMOS) unusual Spectrograph the Multi-Object with Gemini study the spectroscopic field integral an present We nvriaed ˜oPuo .d a˜o12,Cdd Uni- Cidade Mat˜ao 1226, Brazil. do SP, S˜aoversit´aria, Paulo, R. 05508-090, S˜ao Paulo, de Universidade nteUies.Te a edwlae from downloaded be can They https://sites.google.com/site/nebulatomtools/ Universe. the in objects for emission-line on workshop astronomers 3-16 development American Latin capacity NEB- (Venezuela, a the Choroni 2013), nebulae. that at March in of proposed tools workshop analysis bet- been some nebulae, ULATOM the have insight a problems for ionized proper These developed to the in with been of student use play have roles to the at respective and lead processes the to of different python. understanding is in ter solutions aim physics and nebular Their comments on problems detailed of with series a present We IHETARIAIYDNENUCLEUS: DENSE EXTRAORDINARILY WITH .Telles E. HSCLCNIIN FAHIGALAXY HII A OF CONDITIONS PHYSICAL nttt eAtoo´a nvria ainlAut´onoma Nacional Astronom´ıa, Universidad de Instituto nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto UH bevtied ai,CR,UiesteParis Universit´e CNRS, Paris, de Observatoire LUTH, eso hog eoiyaddseso maps, dispersion and velocity through show We H EUAO COOKBOOK NEBULATOM THE 1 .Stasi´nskaG. .X Thuan X. T. , Carrasco MRK996 1 n .Morisset C. and 2 .I Izotov I. Y. , 4 3 n .R. E. and , 2 icas, 187 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ail 0,L eea hl,([email protected]). Chile, Serena, La 603, Casilla Ukraine, 03680, 4 Kyiv, 27, ([email protected]). Zabolotnoho Sciences, of Academy ([email protected] USA, 22904, 3 VA Charlottesville, 400325, ([email protected]). Brazil, 2 20921-400, RJ, Janeiro, 1 of population a derive we bumps, ∼ red of and intensities an blue the on the From superposed pattern. region, Wolf-Rayet rotation nuclear of underlying the population in a stars from (WR) stel- outflows suggesting wind 996, lar Mrk of spectrum integrated the 188 h anpoeio aais n nodbi stars endo-debris of and radius galaxies) virial progenitor the main outside the were sub-galactic they in while (formed systems stars debris from con- received tributions have populations inner- stellar simulated outer-halo and Our characteristics. chemical differ- kinematic particular comprise and with which dif- sub-populations haloes, stellar the outer ent and populations: two inner defined fuse stellar to distinct adopted simulated are dynamically six criteria Project. of energy Aquarius the Binding haloes from prop- stellar galaxies Way-like diffuse kinematic Milky the and of chemical erties the investigate We Z eetdnro [O narrow detected xgnaudne12+log(O/H)=7.94 abundance oxygen o WE tr ntenceso r 9,resulting 996, high Mrk a of in nucleus the in stars (WCE) bon r 9 s oee,ntoe-nacdb factor a by nitrogen-enhanced of however, is, 996 Mrk eddt ute xli h elho information is spectroscopy. of field methodology wealth integral new the by provided high-density exploit data, further and our to low- analyze needed to mapping – for clouds method a tomography and (PCA) methods Analysis new Component two Principal of – here use made have environment. we high-density Although enhanced a to in emission also line nitrogen but to ejecta, due WR probably is nitrogen-enriched enhancement nitrogen This eling. .B Tissera B. P. H OMTO FSELRHLE OF HALOES STELLAR OF FORMATION THE ⊙ eiiOsraoyAR,Suhr prtosCenter, Operations Southern Observatory/AURA, Gemini 7 aentoe WL tr and stars (WNL) nitrogen late 473 srnm eatet nvriyo igna ..Box P.O. Virginia, of University Department, Astronomy bevtoi ainl u o´ rsio 7 i de Rio 77, Cristino, Jos´e Rua Nacional, Observat´orio ∼ anAtooia bevtr,UriinNational Ukrainian Observatory, Astronomical Main yuigtedrc T direct the using by ) edrv,frteotrnro-iergo,an region, narrow-line outer the for derive, We 0 nareetwt rvosCOD mod- CLOUDY previous with agreement in 20, ASV PRL NHIERARCHICAL IN SPIRALS MASSIVE N (WR)/ 1,2 .C Beers C. T. , N Scannapieco SCENARIO OW)o 0.19. of (O+WR) iii ] λ 33ln.Tencesof nucleus The line. 4363 e ehddrvdfo the from derived method 4 .Carollo D. , 3 ∼ ± 8erycar- early 98 0 . 5 0( 30 n C. and , ∼ ABSTRACTS u). 0.2 19NW Australia. NSW, 2109 5 USA. Germany. Garching, 4 D85748, 1, Str. oro 7 u.2,12,Beo ie,Argentina. Aires, Buenos 1428, 28, 3 Suc. 67, Correos 2 Argentina. CONICET, diinlcnrbto rmds-etdsasi the 3 in range stars an disc-heated possess from haloes contribution inner The additional haloes). matter inside dark systems the sub-galactic gas-rich in formed (those 1 h itr fasml ihni irrhclclus- hierarchical in within scenario. assembly tering to of linked with history be character- can vary the the distributions metallicity how haloes the and stellar of radius istics virial the the in to up abun- stars radius the the how show of results dances Our energies. system, enrichment lower chemical halo of and levels main higher have the to into tend satel- and farther massive sink more which in con- lites, formed to due stars primarily from arise tributions profiles outer- steeper the the of relatively mild, are case gradients [Fe/H] the although In regions, halo binding stars. lower debris at found than be energies to tend which endo- stars, and debris disc-heated the from re- contributions are to regions lated inner-halo the con- Steeper in relative gradients sub-population. the abundance the stellar both each and from by enrichment tributions chemical influenced of are level in regions gradients inner-halo abundance the sub- observed disc-heated The or populations. endo-debris the mainly from ratios, with [alpha/Fe] contributions low associated to outer-halo detect moderate and with we inner- stars the populations, both stellar In stel- insitu populations. so-called lar the define Endo-debris stars ones. disc-heated youngest plus support, the kinematical among particular of in signatures exhibit can stars n C3,rsetvl.UigGemini/GMOS Using NGC6845 NGC92, respectively. merger: the HCG31, galaxy in a and and of systems in interacting body two distribution main of metal tails the tidal of the analysis an present We EALCT RDET NTDLTAILS TIDAL IN GRADIENTS METALLICITY Alfaro aqai nvriy et hsc srnm,Sydney, Astronomy, & Physics Dept. University, Macquarie .Torres-Flores S. osj ainld netgcoe in´fia T´ecnic Cient´ıficas y Investigaciones de Nacional Consejo a-lnkIsiuefrAtohsc,Karl-Schwarzchil Astrophysics, for Institute Max-Planck ainlOtclAtooyOsraoy usn 85719, Tucson, Observatory, Astronomy Optical National nttt eAtoo´ayFıiadlEpco ail de Casilla Espacio, F´ısica del Astronom´ıa y de Instituto .R Carrasco R. E. 1 − .Mne eOliveira de Mendes C. , 0,wt enof mean a with 30%, N EGN SYSTEMS MERGING AND 1 5 .SaaoJr Scarano S. , .Amram P. , ∼ 6 3 n .Plana H. and , .F eMello de F. D. , 2 0 Disc-heated . 20% .Olave D. , 1 M. , 7 4 as, , d XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes xgnaudneo hs structures. these the of enhancing abundance in for- oxygen mechanism star important an the is that in metal mation suggest the scenario we in However, the flattening a distribution. support produces results mixing of gas our case which the tails, In tidal suffered. the system this gravitational that strong interaction the despite abundance keeps metal complex its forming star found central each Apparently, we the 31 for region. distribution HCG For metal inhomogeneous distribution. suggest- an lo- metal also galaxy, source flat this a one of ing region to inner the abundances in in similar cated located have regions tail that the found the we For NGC6845, system. this system of distribution flattening mix- metallicity a the gas produces in that interaction the suggests by fact triggered central ing This the the in by NGC92. displayed abundances of values The regions the to NGC92. similar gradi- are of tail metallicity tail no the for found ents we data, spectroscopic H NRMD AAYM1I H ERA THE IN M31 GALAXY ANDROMEDA THE 3 S˜ao Cristov˜ao,Sergipe, Brazil. 2 ([email protected]). Chile ena, 1 7 France Marseille, Universit´e, CNRS, 6 Chile. Serena, La 5 Brazil. S˜ao S˜ao Paulo, Paulo, 4 de Universidade da hog h nlsso h oormgiuedia- populations. colour-magnitude stellar the resolved of of galaxy grams analysis the the across vari- histories through the star-formation establishing of (3) hence ations and and (2) constant; distance disc; Hubble its thin the measuring and for indepen- vast methods three dwarfs using dent a the accurately in very of M31 orbiting half anchoring be where to M31, appear around satel- system the lite of un- structure (1) 3-dimensional the at the of attempts derstanding recent tests review further we for Here of understanding essential level paradigm. be same percent, to the appears few to to detail evolution a out and of formation carried galaxy level be precision can a pre- measurements where cosmology, and precision dictions of advent the With iaeEtda eSnaCu,Ilh´eus, Brazil. Cruz, Santa de Estadual sidade aoa´rod srfıiaT´rc bevcoa,Un Astrof´ısicaLaborat´orio Observacional, Te´orica de e eatmnod ´sc,Uiesddd aSrn,L Ser- La Serena, La de F´ısica, Universidad de Departamento ahlcUiest fAeia ahntn USA Washington, America, of University Catholic nttt eAtooi,Go´sc Ciˆencias Atmosf´er Geof´ısica e Astronomia, de Instituto eatmnod ´sc CT nvriaeFdrlde Federal Universidade CCET, F´ısica - de Departamento eiiOsraoyAR,Suhr prtosCenter, Operations Southern Observatory/AURA, Gemini aoaor ’srpyiu eMrele i Marseille Aix Marseille, de d’Astrophysique Laboratoire FPEIINCOSMOLOGY PRECISION OF .Valls-Gabaud D. 1 ABSTRACTS iver- icas hsscd CdFradse l 05 ocompute to In 2005) al. 2008). et Fernandes syn- (Cid spectral al. code STARLIGHT thesis the et use (Yan we research, Seyferts this rarely, (LINERs) more “low- regions” and, harbor emission-line This may nuclear galaxies hosts. ionization PSB (AGN) most typical Nuclei that with Galaxy suggests lines Active emission of nonzero ratios but weak hibit h la iia k uvy(DS nyb re- by only (SDSS) in [OII] Survey identified minimal galaxies Sky quiring Post-starburst Digital Sloan 2004). the al. el n ruso galaxies. galaxies of sev- isolated groups by of and samples studied different different been for the authors has eral for correlation correlation This this samples. of behavior In- variations the Wide-field show We on the in- (WISE). from Explorer and microns Survey (NVSS) frared 22 Survey at Sky fluxes fluxes VLA GHz frared 1.4 NRAO ga- use the We of from groups galaxies. compact isolated and of far laxies, samples and in radio fluxes the statistical between infrared correlation the the from of analysis results preliminary present We int ii trfraini olmtteequiva- the limit [OII] to the is of formation width star lent limit to rion 1 inld C´ordoba, Argentina. de cional 2 Argentina. ICET, 1 eetbeeiso ie htcaatrz trfor- [OII] star characterize (e.g. mation that no but lines selecting lines, emission by absorption detectable Balmer generated by strong usually with Samples produced are spectra is galaxies Gyr. PSB flux 1.5 than of their younger of star populations 70% ongoing stellar in- over of (SFH) that histories sign formation dicate no star but popula- Their stellar spectra, formation. young their of of in class traces tions strong a with comprise objects galaxies (PSB) Post-starburst bevtroAto´mc eCodb,UiesddNa- Universidad C´ordoba, de Astron´omico Observatorio nttt eAtoo´aT´rc xeietl CON- Experimental, Te´orica y Astronom´ıa de Instituto EM,Osraor ePrs France. Paris, de Observatoire LERMA, I/AI ORLTO NCOMPACT IN CORRELATION FIR/RADIO TLA OUAINPOETE OF PROPERTIES POPULATION STELLAR .R eaValdarenas Vena R. R. OTSABRTGALAXIES POST-STARBURST RUSO GALAXIES OF GROUPS .Werle A. λ 77adH and 3727 1 λ λ n .Mateus A. and 77eiso eeal ex- generally emission 3727 77asrto ie(Goto line absorption 3727 1 n .Valotto C. and α .Teuulcrite- usual The ). 1 1,2 189 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ln it E H (EW width alent ihlweiso ie r nfc asv galaxies, hosts. passive AGN fact weak in as are misclassified galaxies frequently lines post-starburst dia- emission of WHAN low most the with that using show However, we by (2008). gram, found as al. high hosts, et a Seyfert Yan identify and we LINER diagram, of plotting BPT occurrence When the in 2011). sample al. for- this et star Fernandes current (Cid without mation galaxies select criteria last 1 find grow. to and hole quest black structure the how in the tech- out engines into central the these light review of I shed behavior work have this directly that In material niques the region. of this details outside disc, important started accretion reveal have the to observations fueling, interferometric of although source final re- Their to the impossible observe. solve it en- makes to nature central difficult compact the remarkably extremely evident, is influence is itself hole’s structures gine clus- black large the host these Although in their and galaxies. into galaxies, of energy host ter significant their of inject evolution even the large a in had impact have holes black supermassive Accreting Braz Catarina, ([email protected]). Florian´opolis, Santa 88040-900, Ferrei CEP: Jo˜ao David Lima, Universit´ario Reitor Campus Catarina, 1 70%, than larger LFYS with log([NII] galaxies those classify then PSB We volume-limited as catalog. a DR7 SDSS in the from LFYS, sample by popu- denoted stellar young here from lations, coming light of fraction the 190 .Audibert A. ETN H HSCLPOETE OF PROPERTIES PHYSICAL THE TESTING otfii nvria Cat´olica, Chile. Universidad Pontificia eatmnod ´sc,Uiesdd eea eSanta de Federal Universidade F´ısica, de Departamento CIEGLCI NUCLEI GALACTIC ACTIVE H NFE OE O AGN FOR MODEL UNIFIED THE λ 6584/H CIEGLCI NUCLEI GALACTIC ACTIVE 1 .Riffel R. , α ihrta 04adH and -0.4 than higher ) α .Ar´evaloP. mle hn5 than smaller ) .Sales A. 1 .G Pastoriza G. M. , 1 1 .Teetwo These A. ˚ 1 n D. and , α equiv- ABSTRACTS ra il G 51 h obde ie show of lines nucleus forbidden the The towards 4501. inflows NGC as structures, spiral blueshifts interpreted along observed redshifts being we side locations. galaxy near the some the on of and at side seen far the are On rotation from viations n rm5 o10k s km 150 to 50 from ing [S ihavlct mltd f10km 100 galaxy at of the nuclear amplitude be- of velocity the similar, plane a are the of with in lines flux rotation all by of for dominated field peak ing velocity the gas 5” The to it. up to sion l mle aus ihtehgetoe reaching ones s highest km the 100 with values, smaller all GO)a eiiNrhtlsoe h nldata final contains The cube Spectrograph telescope. Gemini-North Multi-Object at (GMOS) Gemini galaxy Spectroscopy 2 with Field Seyfert Integral obtained the optical kine- of from region 4501 gas NGC central and the in stellar matics two-dimensional present We 7” i aafo pte eecp ntemdinfrared mid the pub- in using telescope galaxies Spitzer (5.2-38 Seyfert from 100 data about lic of of parameters region. sample physical torus, line a the broad the a statistically the analyze obscure of and We can presence hole angles black the view different supermassive to different that under due suggests which are (UM) classes Model AGN Unified The h pcrleeg itiuin SD)with (SEDs) distributions energy spectral the rned u,Cmu oVl,CiaPsa 55,91501- ([email protected]) 15051, Brasil. Postal RS, Caixa Alegre, Vale, Porto do 970 Campus Sul, do Grande 1 iesoa asfrteflx eoiyadvelocity and velocity ( flux, dispersion 2.7 the of for resolution maps spectral dimensional 5600 a at from region A ˚ spectral the covering msinln rfie fH of profiles emission-line ie r bevda - rscnrhatfo the the in from seen distortion northeast a arcsec with co-spatial 2-3 being nucleus, at observed are lines omdb ut lusadpeetterslsfr8 for is results the torus present the CLUMPY and clouds that dusty by consider formed which SEDs theoretical .Brum C. eatmnod srnma nvriaeFdrld Rio do Federal Universidade Astronomia, de Departamento W-IESOA IEAISO THE OF KINEMATICS TWO-DIMENSIONAL ii × ] ETA EINO G40 FROM NGC4501 OF REGION CENTRAL λλ 5 tsailrslto of resolution spatial at 15” MSGMN NERLFIELD INTEGRAL GMOS/GEMINI 7763.Allnspeetetne emis- extended present lines All 6717,6731. cnr Muller Schnorr )i re ovrf h M ecompare We UM. the verify to order in m) − 1 .A Riffel A. R. , 1 h highest The . σ parameters. eeotie rmtefitn fthe of fitting the from obtained were ) ∼ SPECTROSCOPY 60 pcr oeigteinner the covering spectra 16000 1 2 − .SociBergmann Storchi T. , n .Robinson A. and , 1 α hl h H the while σ [N , ausfralemission all for values ii FH) Two- (FWHM). A ˚ ] λλ − 1 5868 and 6548,6584 ∼ σ lhuhde- although , α ausrang- values hw over- shows 0p and pc 50 o7000 to A ˚ 3 2 ∼ A. , . 10 ∼ 6 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes eoiyfil.Teeeto est a obtained map density [S electron the The from field. velocity ewe 0 cm 100 between fhg densities. high of ohse,N 42 USA. 14623 NY Rochester, Brasil). Brasil RS, 91501-970, 3 Alegre RS, Porto 15051, F´ısica, CP Maria, Santa 2 97105-900, (carine.fi[email protected]). F´ısica/CCNE, de 1 cto ihteclr h paetadabsolute and distributions. apparent redshift classi- the the morphological and color, magnitudes, obtained the the with com- fication e.g. galaxies, host for the paring of properties discuss host, further QSO Lyman the the from for ex- and or dust intergalactic for either corrections tinction, account ob- into we that tanking magnitudes tained absolute on magnitudes based dis- apparent colors We SDSS and from filters. derived the Gaia colors over cuss the all including extrapolated window, be do- can optical filters method SDSS The to the main. database, on quasar magnitudes, Gaia absolute a the derive present on We based galaxy. method, host as new the well of properties as derive schemes, to of against classification performance QSOs morphology the compare other certified to DR7, ex- spectroscopically SDSS being the the are on parameters plored These ”real and the circularity param- QSOs. distinguish point-like” to sharpness, morphological us PSF 3 enable which the of gaussianity, on use based each made eters for We budget error object. astrometric vari- the and define morphology, are ability Brightness, QSOs fidu- fundamental, the grid-points. of role cial all this fulfill Not to suited be equally interpreted. upon will frame and observations reference independent combined the several build the QSOs to 500,000 which used least be at will be that will there will later Gaia the objects. Among extra-galactic mode, of survey measurements provide repeated also Op- all-sky stars. in billion erating 1 for information astrophysics dynamics, and astrometrics, delivering Way, census Milky complete the a of furnish will Gaia mission ESA The ohse nttt fTcnlg,5 obMmra Drive Memorial Lomb 54 Technology, of Institute Rochester nvriaeFdrld i rned u,Isiuode Instituto Sul, do Grande Rio do Federal Universidade .Coelho B. nvriaeFdrld at ai,Departamento Maria, Santa de Federal Universidade ANTDSO H DSD7QSOs DR7 SDSS THE OF MAGNITUDES OPOOYADABSOLUTE AND MORPHOLOGY ii 1 .H Andrei H. A. , ] λλ − 3 7161 iertososvalues shows ratio line 6731/6716 h ulu o90cm 900 to nucleus the α oet nteftr ewn to want we future the In forest. 1,2,3,4 n .Ant´on S. and , − 3 naring a in 5,6 ABSTRACTS xiainadknmtc fteinr2.5 inner the of kinematics gaseous and the excitation of analysis two-dimensional a present We o,Portugal. bon, 6 Portugal. Porto, 5 4 3 ([email protected]). de Brazil Rio 2 RJ, 20080–090, – CEP Janeiro Antˆonio, 43, Pedro Ladeira Janeiro, 1 h icmula a,gvn rgnt h nuclear the to pushing origin is giving arms. jet trig- gas, nuclear and circumnuclear A 102B the disk activity. Arp a nuclear of in its nucleus gering settling the 102A, around Arp rotating with 102B scenario interaction Arp a by an captured propose recently in We been sky. has gas the launched which of is in plane outflow the the ra- to that the close the by also pushed in suggesting outflow jet, originated an dio of as walls loca- interpreted back jet and be and front but arm can eastern blueshifts which the show tion at maps redshifts Channel some with also interacting disk. the is This in jet jet. gas the radio that and suggests arm correlation blueshifts eastern lower the with with east, correlated the to blueshifts and west pcrgaho h eiiNrhtlsoea a at telescope of North field resolution Gemini integral spatial the GMOS the on with spectrograph opti- obtained from spectra 102B, Arp cal galaxy 1 LINER/Seyfert the of otgsi nrtto na nlndds ihline with disk inclined angle an position along that in to nodes rotation suggest seems of in jet maps is radio velocity gas the Centroid most the where of region deflected. border a be northern high- at the is in arm, density and east gas nucleus The the line at with 8.4 for- LINERs. est low, a the is of arms typical with with the ratios correlating west, along excitation jet the Gas the radio to mer. to bent pc 500 kpc VLA 1 other GHz reaches the arm the and One east with we observations camera. spiral previous HST-ACS nuclear in two-armed discovered same have the show maps .S Couto S. G. ULA PRLI H CIEGALAXY ACTIVE THE IN SPIRAL NUCLEAR I/audd eCˆnisd nvriaed iba Lis- Lisboa, de Universidade Ciˆencias da de SIM/Faculdade A/nvriyo etodhr,Hted UK. Hatfield, Hertfordshire, of CAR/University France. Paris, Paris, de SYRTE/Observatoire Brazil. Janeiro, de Rio Observat´orio Nacional/MCTI, bevtoi oVlno nvriaeFdrld i de Rio do Federal Universidade Valongo, Observat´orio do IG/audd eCˆnisd nvriaed Porto, do Universidade Ciˆencias da de CICGE/Faculdade IEAISADECTTO FTHE OF EXCITATION AND KINEMATICS .Robinson A. 1 .Storchi-Bergmann T. , 2 .Kharb P. , R 102B ARP ≈ 5 c msinln flux Emission-line pc. 250 3 n .A Riffel A. R. and , ≈ 88 ◦ esit othe to redshifts , 1 .J Axon J. D. , × . kpc 1.7 1,4 191 2 , 2 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes msinln rfie yGusHriesre.The series. H Gauss-Hermite by profiles emission-line bevto,wieteBr the while observation, aoi E 70-0,SnaMra S Brasil. RS, Universit´aria, Maria, Bairro Santa Cidade 97105-900, 1000, CEP Roraima, Camobi, Av. 8000, 3220 1 97105-900, Exatas, Brazil. e RS, Maria, Naturais Ciˆencias Santa de Centro F´ısica, 4 India. 560034, Bangalore USA. 14623, NY Rochester, 3 Dr., Memorial Lomb Brazil. RS, 2 91501-970, Alegre Porto 1 192 otes otws ieto.TeH The direction. northwest – southeast h G rsok.W siae nexcitation an estimated We from X-rays of by shocks. temperature ther- heated or by gas AGN excited as the gas such of processes, emission mal with consistent is nerlfil pcrsoywt h eiiNF at of NIFS resolution Gemini spatial the a K-band with using spectroscopy 2110, NGC field galaxy integral active the of central the region of mapping two-dimensional a present We nepee sa jcino a rmtenucleus rate outflow the mass from a of with gas bi-cone of a within ejection (outflows) an as interpreted yfitn h H the obtained distribu- were fitting 2110 flux NGC for by and gas kinematics emitting the the of for tions kinemat- maps stellar The the as well ics. as ion- lines, and emission molecular gas ized the for kinematics and tributions inptenta hs bevdfrtesas In stars. the rota- for H similar observed the a those addition, present than fields pattern velocity tion gas The gas. aay nti ae h asiflwrt sesti- is rate inflow the mass of the (inflows) be case, to nucleus this interpretedmated the In be towards can located galaxy. they flows galaxy, gas gas the of of as emission plane struc- the from kinematic in these originated and If are nucleus it. the of tures ob- of south the north are to the redshifts structures to blueshifts spiral in Two served components. matic ai opnn bevdfrH for observed component matic nvriaeFdrld at ai FM oe 5 55 +55 Fone: UFSM, - Maria Santa de Federal Universidade nvriaeFdrld i rned u,I,C 15051, CP IF, Sul, do Grande Rio do Federal Universidade hsc eatet ohse nttt fTcnlg,85 Technology, of Institute Rochester Department, Physics ninIsiueo srpyis n lc,Koramangala, Block, 2nd Astrophysics, of Institute Indian 2 nvriaeFdrld at ai,Dpraet de Departamento Maria, Santa de Federal Universidade ≈ FTECNRLRGO FNC2110 NGC OF REGION CENTRAL THE OF rsnsetne msini h hl edof field whole the in emission extended presents 4 W-IESOA KINEMATICS TWO-DIMENSIONAL . 6 .R Diniz R. M. × 10 ≈ − 4 2 4 Storchi-Bergmann ≈ M . 2 1 eoiyfil rsnsohrkine- other presents field velocity λ ⊙ × 2100 1 2 yr .A Riffel A. R. , . 1218 10 ≈ − 1 − 5p.W rsn u dis- flux present We pc. 25 − . γ 4 M 70KfrH for K 2700 setne nyt the to only extended is n H and m ⊙ yr 2 − 1 2 mtiggswas gas emitting 1 n T. and , nte kine- Another . i λ 2 2 2 . emission emitting 1661 ABSTRACTS m 3863,A.BnoGncle 50 ax otl15051, Brasil. Postal RS, Caixa Alegre, Gon¸calves 9500, Porto Bento 91501-970, CEP Av. 6439, 3308 2 ouain swl sdsnagigtefeatureless components. the dust disentangling hot as and stellar well dominant as the map population, to NIFS spectroscopy, gemini field results with integral taken preliminary resolution present spatial we high ionizing of 1052 dominant NGC the of LIN- discriminate and source to Seyfert Aimed galaxies of ERs. spectra detected nuclear commonly NIR also Hot in is unresolved populations. emission stellar dust age contri- intermediate the by of dominated bution NIR is galaxies Besides, active con- of the tinuum that stars. revealed have age studies population intermediate shows stellar AGNs (iii) of of and excess (SP) disk, an accretion population an stellar into The matter shocks. of by fall powered (AGNs) in nuclei the galactic active branch (ii) expanding giant rapidly shells, their asymptotic ionize that post explain (post-AGB) to stars i) possibilities Gyr spectra: three 1 mainly LINER’s about are 1052 event There merger NGC ago. a works, experienced previous have to may according and Myr, fmgiueaoeta siae o nevolved Their an H stars. for branch horizontal estimated extreme of that population above magnitude of ihte en on tla lsesaged clusters stellar young consistent being are them distributions with energy spectral (NIR) NELN H IE AUEO NGC1052 OF NATURE LINER THE UNVEILING at Maria. Santa 2 Sul. do Grande 1 inln a ean nla.Acrigt recent to H According exhibit 1052 emis- unclear. NGC its remains studies of gas nature line the sion lines, with unusual emission optical spectroscopically However, broad is disk. region typical rotating central a stellar the as classified a and harboring galaxy LINER E4 an is 1052 NGC .I .Diniz F. I. S. A OMTO NCRUBNR AGN CIRCUMBINARY IN FORMATION GAP eatmnod srnma nvriaeFdrld Rio do Federal Universidade Astronomia, de Departamento Riffel α eatmnod srnmaI-FG,Fn:+551 +55 Fone: IF-UFRGS, Astronomia de Departamento eatmnod ´sc/CE nvriaeFdrlde Federal F´ısica/CCNE, Universidade de Departamento qiaetwdh n pia-ona infrared optical-to-near and widths equivalent 2 .R Diniz R. M. , .Escala A. 1 .G Pastoriza G. M. , 1 2 n .Storchi-Bergmann T. and , DISKS n .DlValle Del L. and α uioiisa order an luminosities 1 .Riffel R. , 1 1 .A. R. , < 1 7 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes asi h nlsprtosadpsbemrigof merging posible and failed AGNs. separations binary and final the opened the discuss of in We gaps occurence gap. the succesfully a for which opens implications that disk, disks the the predicts in per- enhanced non-axisymetric against the turbation results on our based contrast models We analytical gap the them. prevent in to able most formation are that disks thicker found and and massive etc.) thermodynamics, (mass, ubnr ik fcmaal asmsieblack ( massive cir- binaries mass in hole comparable gaps of of disks formation cumbinary the study numerically We 1 nte“rdtoa”aayi ftecube. seen the hot of was analysis north- structure “traditional” to This the nucleus in southwest. the from to 1.5” and to east up to extend of and radius (with hydrogen molecular ∼ of from ring originated nuclear arms a spiral two in concentrated sion rp)a pta eouinof resolution the spatial with a obtained at graph) 1066, Spectro- Mrk K Integral-Field (Near-Infrared galaxy and Gemini/NIFS 2 inner J Seyfert the Anal- the analyze for Component to datacubes (Principal band technique PCA tomography the ysis) used We adadistmga hw htteH the that shows the tomogram for its eigenspectrum and fifth the band of K line-emitting analysis the The by with jet originated gas. radio probably the band), of (K interaction (for 4 the 3 and eigenvector band) the eigenspectrum. J in the next seen are the profiles line for Double radio observed and respec- are line their among emission and Correlations band) band) J K tomograms. (in tive (in 2 rotat- 3 A eigenspectrum eigenspectrum in torus. and observed dusty is the disk of ing emission as eigenvector the this due interpret we being thus dominated and is part, emission red nuclear by tomogram, the that corresponding observed In is it blue K wavelengths. the the red between for anti-correlation and eigenvector second an The presents vari- the band data. of the 95% of to corresponds ance and AGN galaxy the host from and emission by dominated is eigenvector ULA OEUA IGI MRK1066 IN RING MOLECULAR NUCLEAR A nvria eChile. de Universidad .”)sronigtenceso h aayring galaxy the of nucleus the surrounding ) 0.2” EELDB C TOMOGRAPHY PCA BY REVEALED .G Hennig G. M. q Storchi-Bergmann ∼ ) evr h ikproperties disk the vary We 1). 1 .A Riffel A. R. , ≈ ≈ 2 5 crdu of radius pc 350 1 5p.Tefirst The pc. 35 n T. and , 2 emis- ABSTRACTS htpoue hteiso.W on hti all in that found We Ly the emission. cases derive that to produces mechanisms the lines different that correlate the iron of We optical contribution BLR. relative and the NIR the the emission of of FeII portion strength the outer for the responsible smaller is gas considerably the assump- is that previous and tions confirming Hydrogen, CaII of and that approaches OI than systematically of iron that show of to results FWHM Our BLR. with the in lines that emitted FeII lines individual other of the that of We width the respectively. study the ion, proba- to compare that most and of the region mechanisms derive emitting formation the to of intensity order location and in ble width lines the FeII of the this analysis In of a AGNs. made other in we time work first is the it by and tem- IZw1 applied, in now particular FeII That the accurately reproduces emitter. plate galaxy prototype active the FeII considered of ob- is which template IZw1, semi-empirical from a tained utilize we AGNs 21 of itn nlsso hteiso.Wt h i of aim the 0.8-1.2 With con- range the more in of FeII emission. a the free that studying to of but window analysis intense a sistent infra- is opening near emission the effects FeII In blending the region. that (NIR) of red cooling contribu- the important there- to most and the tors the of one one prominent (AGN) constitutes most nuclei fore the galactic is line emission active broad FeII the in by (BLR) emitted region lines spectral the Among ae vnd et ocle,90 rtsoAvs Porto Brasil. Alves, 91509-900, Protasio Cep 9500 RS Goncalves, Alegre Bento Avenida Vale. Cep 2 RS Brasil. Maria Santa 97105-900 camobi universit´aria bairro cidade 1000 1 3 2 1 .A .Marinello O. A. M. HSCLPOETE FFI EMISSION FEII OF PROPERTIES PHYSICAL uoenSuhr Observatory. Southern European Astrof´ısica. de Laborat´orio Nacional Itajub´a. de Federal Universidade nvriaeFdrld i rned u apsdo Campus - Sul do Grande Rio do Federal Universidade nvriaeFdrld at ai,AeiaRoraima, Avenida Maria, Santa de Federal Universidade H RHTCUEO H ACTIVE THE OF ARCHITECTURE THE AATCNCESO G 1068 NGC OF NUCLEUS GALACTIC NATV AATCNUCLEI GALACTIC ACTIVE IN α ursec ly nipratrole. important an plays fluorescence Garcia-Rissmann 1 .Rodr´ıguez-Ardila A. , 3 nasample a in m 2 n A. and , 193 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes rmr idadinzdb h eta source. the central by the impacted by AGN, cloud, ionized the and emitting of wind H2 north primary is the an to wind from 1” originated secondary about be the to while likely asymmetry originated probably this not is are from wind disk, primary possi- accretion The axis, central co-planar. the ionization suggests to the image associated and fills bly this torus of dusty emission the shape velocity that The high “hourglass”. the the while [Fe velocity emission, low resembling the II] structure for clear shape lines. “glowing-hourglass” a a different found we the analysis particular for The In VI]. behavior [Si distinct line very ionization [Fe shows line high ionization the analysis low and the our II] lines, arc- concentrated H2 0,1 molecular We of the on resolution pc/spaxel). spatial (1,7 with sec bands archives, HK public cen- the SINFONI North) in the the (GEMINI from from NIFS how taken and ejected and data (VLT) and hole re-analyzed black ionized We central being ter. the is how to gas of fed the details being the is understand near gas to the in us spectrographs allow IFU infrared, an with of object, study- prototype such of opportunity ing the The as galaxy. of 1 AGN development Seyfert for obscured the AGN motivated Model studied study Unified most Its the and sky. brightest the the in is 1068 NGC 1 194 a eoeacnieal muto h infalling the outflows of amount the considerable that a suggesting remove pc, may to 10–25 rates but inflow central estimated rates, the the accretion to orders comparable the are 2–3 than they are greater rates magnitude outflow mass of estimate The unifica- to test models. and used tion AGN are the outflows from parameters the feedback model mechanical of mod- The kinematics successfully 3D. and are in geometry we resolving the parsecs, By eling 10–20 of gas. inner evidence ionized the clear of revealed outflows AGN-driven recently have Seyfert Galaxies of observations integral-field optics Adaptive aUP u oMta,12 iaeUiestai S˜ao Universit´aria Cidade ([email protected]). - 05508-090, 1226 - Mat˜ao, Brasil do - Paulo-SP Rua USP, da .Mueller-Sanchez F. .May D. nttt eAtooi,Go´sc Ciˆencias Atmosf´er Geof´ısica e Astronomia, de Instituto H OEO G EDAKI THE IN FEEDBACK AGN OF ROLE THE VLTO FSYETGALAXIES SEYFERT OF EVOLUTION 1 .Steiner J. , 1 .Davies R. 1 .Malkan M. , .B Menezes B. R. , Ricci 1 3 1 .Hicks E. , 1 n .V. T. and , 2 and , ABSTRACTS icas ein efudadaaye osberelations possible analyzed parameters. and this line found between narrow We the in densities region. accre- electronic (b) (c) masses, rates, hole tion black central (a) determined hn01 bl–terdojti ekadcompact. and weak less is is jet power radio outflow the – the Lbol which in 0.1% in jets, than – radio AGN extended other with the objects in observed are yoto oe aitoswt ai u.While powers flux. kinetic radio (with differ out- outflows with which powerful The variations groups power distinct outflow disk. two by form accretion to the seem reaches flows it before gas ntelcluies (z catalogued universe class local such the of on objects sample the This all (SDSS). Survey comprehend available Sky NLS1 Digital 130 Sloan of the synthesis in sample a the spectral chose We of the technique. determination using the 1 continuum approach Seyfert non-stellar we lines. with work broad AGN this prominent In of nu- without subclass galactic but a active characteristics are (NLS1) (AGN) 1 clei Seyfert Line Narrow 3 2 1 i.31,Asrla([email protected]) Australia 3010, Vic. 1 pe iiso h ieo h msinregion. emission the establish of to size intend the mod- I on lens galaxy, limits a intervening upper to the comparing two for in and els ratio images flux lensed the the measuring of By QSO. of lensed structure microarcsecond the the on statis- information provides tical QSOs Earth. micro- of from at microlensing unresolvable Gravitational are scales, disks arcsecond accretion to-nano the and environ- However, QSOs galactic of their ments. onto power feedback the great energetic understanding the their in behind essential force and driving physics, frontier the new at of both is accretion QSO Understanding RVTTOA IRLNIG FQSOS OF MICROLENSINGS GRAVITATIONAL .A Oio A. G. colo hsc,TeUiest fMlore Parkville, Melbourne, of University The Physics, of School P,Germany. MPE, Washington. of Angeles. University Los California of University HRCEIIGTECNIUMIN CONTINUUM THE CHARACTERIZING .Neri-Larios D. RBN G CRTO THROUGH ACCRETION AGN PROBING ARWLN EFR GALAXIES 1 SEYFERT LINE NARROW 1,2 .Vg Neme Vega L. , 1 .Webster R. , .Ferreiro D. < .) ihti ehdwe method this With 0.1). 1,3 1,3 .Schmidt E. , 1 n .Floyd D. and , > .%Lbol) 1.0% 1,4 and , 1 . XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes efudago eainbten[eI n PAH and [NeII] between relation (11.2 good [OIV]. and a [NeIII], found starbursts [NeII], We PAHs, the of of the emission behavior account line into the taking objects, discriminate al- LIRGs-ULIRGs and diagram to diagnostic us aromatic The di- low polycyclic new features. the a on hydrocarbon propose based We diagram galaxies. agnostic Seyfert, radio in and also quasars and galaxies-ULIRGs, star- used infrared of ultralumi- was nous sample galaxies-LIRGs, data infrared a luminous in spectroscopic burst, processes ga- way, those in this discriminate activity to In formation star laxies. to associated pro- energetic cesses the investigate we contribution, this In f6 msinln aaiswt nrrdTelescope Infrared with galaxies emission-line 67 of samples. 3 Colombia. Bogot´a D.C., 2 Colombia. Bogot´a D.C., bia, 1 2 C´ordoba, Argentina. 1 4 3 (CONICET). tet S5,Cmrge A018 USA. 02138, MA Cambrigde, MS-51, Street, 4 Colombia. Bogot´a D.C., Colombia, fmlclrhdoe n [Fe and hydrogen mechanisms molecular excitation of and kinematics the study We RMTCHDOABN NDIFFERENT IN HYDROCARBONS AROMATIC .Riffel R. IGOTCDARMWT POLYCYCLIC WITH DIAGRAM DIAGNOSTIC Brotherton eateto ahmtc,Ntoa nvriyo Colom- of University National Mathematics, of Department ertrı eCecayTenc SCT-UNC). - T´ecnica (SECYT y Ciencia Secretar´ıa de C´ordoba, Astron´omico C´ordoba Argentina Observatorio - ainlAtooia bevtr,Ntoa nvriyo University National Observatory, Astronomical National osj ainld netgcoe in´fia T´ecnic Cient´ıficas y Investigaciones de Nacional Consejo nttt eAtoo´aT´rc xeietl(AE - (IATE) Experimental Astronom´ıa Te´orica y de Instituto eateto hsc,Ntoa nvriyo Colombia, of University National Physics, of Department avr-mtsna etrfrAtohsc,6 Garden 60 Astrophysics, for Center Harvard-Smithsonian OEUA YRGNAD[EI]IN II] [FE AND HYDROGEN MOLECULAR GSADSA OMN GALAXIES FORMING STAR AND AGNS .A Quintero A. S. m+11.3 Higuera-G. 1 .Rodr´ıguez-Ardila A. , 3 .G Pastoriza G. M. , YE FGALAXIES OF TYPES )i trus,LNRadSeyfert and LINER starburst, in m) 3 .R Mart´ınez-Galarza R. J. , 1 .Dors O. .F ao P. Ramos F. A. , 4 1 2 ii .Bonatto C. , .Aleman I. , ie nasample a in lines ] 2 M.A. , 4 1 1 .S. M. , and , ABSTRACTS as . f rmtenceswihi anhdperpendicular launched outflow is an which to nucleus velocities the these ve- from attribute systemic the We to relative locity. blueshifted redshifted one other components, the and velocity and value, two this to due twice are are jet radio FWHMs the emission-line do the perpendicular structure linear the at oto h edteeiso-iepolshv full- have of profiles (FWHM) emission-line -half-maximum jet, the widths-at field radio the the of over most While to profiles. perpendicular emission-line broadened showing oriented width a in of discovery the structure report We linear NIFS. Gemini the with eghitra ewe 0.8 between wave- interval the length in models, to- photoionisation new spectroscopy with gether (NIR) near-infrared SpeX Facility rsneo uenv ennscoet h region the to H the close with emitting remnants excitation associated supernova thermal be of ga- may the presence galaxies forming of forming star star importance in in The in also only but not laxies. nuclei role galactic important ther- an active the plays new that excitation show The mal ratios are, emission-line both and disconnected. that models kinematically suggesting likely, lines, very narrow- (NLR) than region narrower line systematically are lines sion oainltmeaue fH and of vibrational temperatures the rotational between similarity the by ported G 99a pta eouinof resolution spatial a at 5929 NGC iga novn h ierto H ratios line the involving diagram o nds14 arodsNcos E 70-6,Itajub´a,3 37504-364, Nac˜oes. CEP Brasil. das MG, Bairro 154, Unidos dos RS, Alegre, 2 Porto Gon¸calves 9500, Bento Brasil. Av. - Sul do Grande 1 91 e 24-0,Sa o´ o aps P Brasil. SP, Campos, S˜ao Jos´e 12244-000, dos Cep 2911, USA. 82071, 4 WY Laramie, Wyoming, r fteinr3 inner the of tra spec- near-infrared (2D) two-dimensional present We [Fe and r ugse,i re odsrmnt ewe the activity. between nuclear ratios, discriminate of line to types the different order to in limits suggested, New are activity. dom- of their type to inant according objects emission-line rating .A Riffel A. R. eatmnod srnma nvriaeFdrld Rio do Federal Universidade Astronomia, de Departamento aoa´roNcoa eAto´sc/C u o Esta- dos Rua Astrof´ısica/MCT - de Laborat´orio Nacional nvriaed aed aaıa-A.Sihm Hifumi Shishima Av. Para´ıba - do Vale do Universidade ULA UFOSI H EFR 2 SEYFERT THE IN OUTFLOWS NUCLEAR eateto hsc n srnm,Uiest of University Astronomy, and Physics of Department ii 1.257 ] 2 1 .Storchi-Bergmann T. , ie.Ti yohssi ute sup- further is hypothesis This lines. AAYNC5929 NGC GALAXY ∼ /Pa m ′′ 0 ci xetadof and extent in pc 300 × β 3 ′′ sa ffiin olfrsepa- for tool efficient an is fteSyet2galaxy 2 Seyfert the of n 2.4 and m 2 ecnr htthe that confirm We . 2 2 ∼ n .Riffel R. and , 0p obtained pc 20 2.121 ≈ .H m. 0k s 200km ∼ /Br m 2 emis- 0pc 50 195 − 1 γ 2 , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ot lge95190 S Brazil. RS, 91501-970, Alegre Porto 2 (rogemar Brazil. @ufsm.br). RS, Maria, Santa 97105-900, F´ısica, CCNE, is torus 1 the (3) or 5929. flow; NGC the as accretion in from absent an outflowing, winds of as also parts tori is of outer torus models ra- recent the the by (2) proposed to and/or perpendicular ioniz- jet; torus both escaping dio the (1) are in particles that: holes relativistic through means and This radiation jet. ing radio the to 196 h rbblt fr of probability the roso r on logarithmic and priors linear with magnification crolensing e h ie Mtae.a 02,w on evi- with systems found we 2012), al and SDSS1155+6346. HE0047-1756 in et. microlensing chromatic (Motta of dence lines un- the continuum the cores der in line differences emission magnitude the the Comparing with in cores differences software. magnitude line DIPSO them the emission under using flux integrated of continuum and the flux MMT/Blue- from The separated was and obtained (2008). (2007) spectra Channel used Magellan/IMACS We with SDSS1155+6346. and image. halo, lensed galaxy quasar lens a the across hap- in passes object, Microlensing compact a arcs. when pens or gen- images field, multiple gravitational a erating is of light presence the the when in deflected occurs effect lens gravitational The crto ika asinitniypol I(R) profile intensity Gaussian exp(-R a as disk accretion to clus- ter. due J178.81693+63.83446 MaxBCG shear, of large presence the a shows literature. with model agreement in SDSS1155+6346 are which cases, both in rto iksz n stepwrlwrltdto 1/ related = law p power disk the the is of p temperature and the size disk cretion rfie ausbten1ad12 hs ausare values These temperature 1.2. and and days 1 light between values 15 profiles and 3 between sizes HOAI IRLNIGI HE0047-1756 IN MICROLENSING CHROMATIC nvriaeFdrld i rned u,I,C 15051, CP IF, Sul, do Grande Rio do Federal Universidade .Rojas K. nvriaeFdrld at ai,Dpraet de Departamento Maria, Santa de Federal Universidade msinln oeflxsaeue omdlthe model to used are fluxes core line Emission HE0047-1756 systems: double two analyzed We eflo eivlae l 01 oeigthe modeling 2011, al. et Mediavilla follow We 2 /2r 1 s 2 s .Motta V. , ,wt r with ), efudwti 1 within found We . lensmodel N SDSS1155+6346 AND n .A Mu˜noz A. J. and s s n sn h esrdmi- measured the using p and ( 1 λ I + SIS . .Mediavilla E. , ) ∝ λ p γ hr r where , r h etmodels best the are 4 σ β funcertainty, of eestimate We . 2 .Falco E. , s steac- the is ABSTRACTS 3 , ∝ Valencia. 4 3 2 Valpara´ıso. de versidad 1 2 1 e ohv rtkoldeo h eea charac- general environments. the immediate of their knowledge of first teristics a for or- have look in to to blazars der both is around goal galaxies Our of concentrations telescope. in- 8m GMOS North the at Gemini camera) with and taken spectrograph images (multi-object i’ strument 3C66A, and and g’ PG1553+113 on blazars based the of galaxies have fields the We the of in study redshift. photometric a similar undertaken a thus having host the could besides with field galaxy, properties chemical blazar’s and the physical in share information, galaxies of valuable that of analysis give considering the measurement may However, environments the galaxy; their prevents redshift. host this spectroscopic the a cases from ra- or many line nucleus or in the thus continuum from is either It diation detect jet. to relativistic electro- challenging a beamed from by emission to characterized magnetic respect are with observer, orientation the particular be- their which, of (AGNs) cause nuclei galactic active are Blazars etod srfıia nvria eValpara´ıso. de Astrof´ısica, Universidad de Centro Sun- prediction. & (1973) Shakura and yaev literature the with agreement in H LZR G5313AD36AFROM 3C66A AND PG1553+113 BLAZARS THE HRCEIIGTEEVRNETOF ENVIRONMENT THE CHARACTERIZING nttt eFıiayAtoo´a autdd inis U Ciencias, Astronom´ıa, F´ısica de Facultad y de Instituto avr-mtoinCne o Astrophysics. for Center Harvard-Smithonian Canarias. Astrof´ısica de de Instituto nvria ainld aplata-Argentina. La de Nacional Plata. Universidad La Astrof´ısica de de Instituto eatmt eAtoo´ayAto´sc,Uiesddde Astrof´ısica, Universidad Astronom´ıa y de Departameto .J .Vera C. J. R. HL NSYET N IESI THE IN LINERS AND SEYFERTS IN FHILS eakoldet ODCT1271and 1120741 FONDECYT to acknowledge We EIIGO AAI H ’ADG’ AND I’ THE IN DATA GEMINI-GMOS .Tre Zafra Torres J. PIA SPECTRA OPTICAL 1,2 .M Rodr´ıguez M. A. , Andruchow 1,2 Portilla BANDS .A Scellone A. S. , 1,4 1,2 1,3 1,2 n .G. J. and , n I. and , ni- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes nyti ido ie a efudi ea&Por- & Vera in found be prep). can using (in lines diagrams tilla of diagnosis kind and this study, only with of catalog com- the objects A including the study FHILs. this present of LINERs version to plete that enough idea energetic not general study present are the the support spectra, to optical continues the in least At (5) f3t 0 hl h aisbtenio ie (i.e., lines iron between ratios the while Fe 10, to 3 of a pcr fSyetadLNRglxe ae from 9 taken galaxies opti- the LINER of and selection Seyfert of a spectra from cal results main the present We la orltosbtenteflxrto.()I is It (4) Ne of ratios. ratio the flux diag- that the observed present between indicate We correlations which (3) lines clear inner FHILs the between torus. diagrams from obscuring nostic comes the FHILs of of major- part the emission not the but of important, ity, to an sug- anisotropy that seems This idea Sy1 (2) the gests (2012). Sy2. than Portilla FHILs and more (2002) Na- emit by al. found et results the gao with FHILs agrees Sy2 between which and ratios Sy1 galaxies, between fol- flux emission of the The anisotropy and found suggests (1) we spectra literature results: their the lowing analyzing from By data utilizing emis- presented. FHILs with is galaxies 1 sion (Sy2) Seyfert 345 2 of Seyfert catalog and A (Sy1) bet- lines. (FHILs), coronal as lines known ionization ter high forbidden of sion 1 eto trfilsdcyvr lwy fa l.We “black the of all. evolution at long very if the slowly, that very show decay shall fields isolated star while decay, field neutron mass be- magnetic generally of in is result process to Accretion filling lieved the pulsar. of the initiating point onto thus accretion the lobe, reaches Roche solar-type) In its the companion wind. the (of of pulsar star evolution companion (recycled) the systems the the binary by these systems ablated effect: relativistic being widow” is binary “black the the of display fraction small A 4 Colombia. Bogot´a3 DC, 26-85, No 45 2 Carrera Colombia de [email protected] [email protected] [email protected] bevtroAto´mc ainl nvria Naciona Universidad Astron´omico Nacional, Observatorio VII EA FMGEI IL NBLACK IN FIELD MAGNETIC OF DECAY .M Castilho M. C. IHEEG ASTROPHYSICS ENERGY HIGH th Fe , ees fteSS ihdtcal emis- detectable with SDSS the of release X Fe , Vito IO PULSARS WIDOW XI 2 1 n .E Horvath E. J. and , .G Benvenuto G. O. , r ogl rudteunity. the around roughly are ) V /Fe VII 2 1 .A De A. M. , so h order the of is ABSTRACTS l a ainld aPlata. La de Nacional dad aUiesdd eS˜ao2 Paulo. de Universidade da io”sse,satn rmaslrtp trand star solar-type a lasting from starting system, widow” es nadto,temse fte“lc widow” be “black to the predicted of naturally sys- masses are younger the pulsars addition, from extending In drawn , tems. value conclusions bottom previous field the magnetic the below the decay that not conclude does to us allows plane, en oepantesicigmcaimamong mechanism states. switching X-ray various the other the with explain us to quasi-periodic presents means existence of its signs and shows the oscillations tail behind This tail gaseous unstable companion. an of to formation leads the the companion compact by compan- the wind of stellar compact field the gravitational the of of focusing Additionally, rate and ion. accretion donor the the that of sub- by mass-loss force Coriolis the the influences E.g. stantially process. have accretion phenomena the these on effects the darkening, investigate gravity ioniza- we the the and medium, force, the of Coriolis structure the tion account rate. into accretion physi- take the various We e.g. on processes, of constrains and set reliability parameters as cal the well test as We model the model. our from Dopplerograms tomograms obtained synthetic with inter- Doppler comparison data observed direct a via of introduce We method radiation-emitting pretation system. of the structure tomog- in the Doppler material the probe use to Cygnus and ion- raphy simulations of and our parameters distribution in adopt density X-1 We the structure. e.g. sim- ization to wind, model the characteristics the of other use and anisotropy We dynamics, three- ulate HMXBs. the in improved of wind our stellar model using radiation-hydrodynamic obtained dimensional were presented The results for observations. with Dopplerograms comparison synthetic direct generating by addressed of is bina- method diagnostics X-ray spectroscopic the its in and matter ries circumstellar of topic The 1 h crto itr,i ulareetwt recent with agreement full measurements. in history, accretion the nttt eAtooi,Go´sc Ciˆencias Atmosf´er Geof´ısica e Astronomia, de Instituto auddd inisAto´mcsyGeof´ısicas, Univers Astron´omicas y Ciencias de Faculdad AITO-YRDNMCMDLOF MODEL RADIATION-HYDRODYNAMIC > IHMS -A BINARIES X-RAY HIGH-MASS y orahteosre oiini the in position observed the reach to Gyr 5 J. Cechura ˇ 1,2 n .Hadrava P. and > odeto due Mo 2 1 197 icas i- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes etbesucsi rdo ie fsgt The sight. counts of of lines estimates reliable of produce grid to de- a all is up challenge in summing of sources such method of tectable the distribution on galactic based the sources of modeling a form the Telescope pri- on Space the (LAT), instrument Telescope science Area mary Large the by tected 1 CLASS NEW A AS STARS RUNAWAY MASSIVE Republic. Czech Prague, 16 121 3, Karlovu Ke Prague, Republic. Czech Prague, 2 31 141 Boˇcn´ı 1401, public, II 1 198 h eodctlgo high-energy of catalog second The uaa tr aehg pta velocities, spatial high have stars Runaway ics h bevtoa prospects. and observational objects the stellar discuss these non- to relevant related all processes thermal calculate We diffuse into sources. by become non-thermal illuminated might particles clouds relativistic Molecular these sec- and particles. rays gamma ondary p-p yield via These matter collisions. the inelastic with en- interacting surrounding the on cloud in molecular loss diffuse might much escape protons without easily These region ergy. can emitting Protons the velocity. from medium stellar the on the in inhomogeneities depending and density scales of scales time the variability gamma-ray variable with be re- sources, Run- might ra- been stars wavelengths. at early-type gamma-ray has away observations even This of and bunch X-ray energies. dio, a by of confirmed range cently wide a emission non-thermal over produce rel- can radiation. The accelerated particles locally ativistic thermal of population velocity. emits a Additionally, stellar matter shocked supersonic same piled-up the the as in pointing direction structures arc-shaped de- bowshocks as These velop ISM. surrounding the in shocks ms km srnmclIsiue cdm fSinilh zc Re- Czech Scientitlehe of Academy Institute, Astronomical aut fMteaisadPyis hre nvriyin University Charles Physics, and Mathematics of Faculty H AATCDSRBTO FFERMI OF DISTRIBUTION GALACTIC THE nttt retn eRdosrnma(IAR). Radioastronomia de Argentino Instituto FGLCI AM-A SOURCES GAMMA-RAY GALACTIC OF − 1 n fteaemsie a rdc bow- produce can massive, are the if and , .V e Valle del V. M. .Jablonski F. losu o h rttm oper- to time first the for us allows , ON SOURCES POINT 1 1 n .E Romero E. G. and n .Polido P. and em Gamma-ray Fermi γ rysucsde- sources -ray 1 1 > V ABSTRACTS 30 oiyfnto.Telmnste oe h range the cover luminosities lumi- The the 10 for function. forms tested Power-Law nosity We and Galaxy. Gaussian the in both typical populations scale, young height radial very short of very a a near- to and from counts point obtained infrared that conclusions with consistent scale Our length the above distribution plane. direc- exponential radial galactic an as the well in as which distribution tion model exponential a an of counts predictions has source the with estimated galactic compared the and are of results longitude The galactic latitude. both along sources ihsaedniis(nteslrnihoho)of neighborhood) solar the (in ∼ densities space with at cieoratmt oetmt h est of density the estimate to attempts our scribe counts/deg rmsalnmes h aao otis1873 contains 0 of catalog average an giving The sky, whole the over sources numbers. small from 1 iiin ([email protected]). Division, rbto o w irqaas(ynsX,Cygnus- in dis- (Cygnus-X1, energy microquasars rates two spectral for loss observed tribution relevant the reproduce correspond- the to and the order rate compute We acceleration ing fields. matter inter- field, radiation non-thermal magnetic and surrounding to the due with substantial energy actions their lose of In particles amounts accelerated the ac- AGNs. the of and this microquasars region addition, discuss around we coronal disk work, the accretion this in pro- In mechanism Fermi celeration first-order occur. a may because can cess efficient reconnection rather magnetic magneto- fast be cosmic Recent by that acceleration revealed ray have questions. fascinat- studies many important hydrodynamical as raises and AGNs acceleration ing and particle sources. microquasars their of of sites of scales identification characteristic The com- the regions compact to very accelerated pared in TeV are above particles acceleration) energies how to explain shock to on have particle which based of (mostly theories micro- current acceleration and challenging AGNs are of quasars observations energy high Very .Khiali B. ANTCRCNETO OE FOR MODEL RECONNECTION MAGNETIC A nttt ainld eqia saii/CI Astrophy Espaciais/MCTI, Pesquisas de Nacional Instituto XLIIGMCOUSR RADIATION MICROQUASARS EXPLAINING 33 10 | b | − − < 8 /pc 10 0 . 1 5 36 3 .M eGueaDlPino Dal Gouveia de M. E. , ◦ 2 . efid18sucs nti ok ede- we work, this In sources. 128 find we for r/ nte10MV10GVband GeV MeV–100 100 the in erg/s | Valle b | > 60 2 n .Sol H. and , ◦ nanro ti centered strip narrow a In . 3 1 .V del V. M. , γ . -ray 036 s XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 3,cnieigtemdlaoeadlpoi and leptonic and above processes. hadronic model the considering X3), egp,Brasil. Sergipe, Brasil. Janeiro, de 2 Rio Janeiro, Ciˆencia, Tecnolog Inova¸c˜ao de Minist´erio da Rio - (MCTI), (ON) vat´orio Nacional 1 3 2 br). 1 fmgei ciiisna h esa sbigthe being as emission. X-ray star the Be of the source near activities and magnetic interpretation understanding the of current strengthen our emit- that the by results X-ray presented discuss emphasize of We results class recent new very group. this some of and sample ters a prop- we X-ray of and Here, erties optical the occurs. of emission compendium parameter tested a X-ray present the the further which of in be space characterization can careful this through Be/WD and of number observed, mag- missing of binaries the progenitors for be account could or they netars that years. seven possible in is ten It to one from increased Cassiopeiae h ubro esaswt nsal hard- unusually of with that like stars emission X-ray Be variable and of thermal number The h ag hticue orcutr n groups. and clusters over poor function includes mass that the range determine addi- it the in to groups, of Thus, important characteristics is the structure. determining scale to build- large tion the of are blocks they groups ing clustering, galaxy hierarchical understand in to evo- since, important group’s is the It in role lution. important an play feedback processes potential, Due gravitational shallow 2005). group’s Voit a versions 2000, to Mulchaey down (e.g. scaled clusters simply rich of not are groups Galaxy oreaca eAtooi srfıia(OA Obser- - Astrof´ısica (COAA) Coordena¸c˜ao e Astronomia de bevtied edn France. Meudon, de Observatoire Argentina. CONICET, IAR, nvriyo a al IGUP rzl,(bkhiali@usp. Brazil), (IAG-USP, Paulo Sao of University nvriaeFdrld egp US,Sa Crist´ov˜ao, S˜ao (UFS), Sergipe de Federal Universidade .Vajgel B. .M Ribeiro M. E. BEVTOSO H BO THE OF OBSERVATIONS EETDFO HNR X-RAY CHANDRA FROM SELECTED IHIHSON HIGHLIGHTS RPRISO AAYGROUPS GALAXY OF PROPERTIES 1,2 Forman .A .Lopes A. A. P. , 1 .Lpsd Oliveira de Lopes R. , 2 n .S Murray S. S. and , Dupke γCAS 1 1 .Jones C. , LK STARS -LIKE TSFIELD OTES ¨ 2,1 2 2 n R. and , .R. W. , ABSTRACTS ae ia γ - 2 ([email protected]). Janeiro, 1 xrml rcs omcbcgon radiation background from cosmic data (CMB) precise Extremely t htaynnpioda otmnto ol be could contamination possibil- the non-primordial is any detection that positive ity a with of inherent confidence problem the A of deviations. hy- presence Gaussian Gaussian the weak exclude the not do with they consistency although pothesis show and NG of a analy- Recent dis- signify from to ses models. CMB allowing competing universe, the between early in tinguish detection the NG to robust probe primordial the unique of this, in- not– For the –or on depend models. depen- expected flationary scale intensities primor- types, and the after) dences, where soon inflation, (or cosmic during dial field originated Possible CMB be the could to contributions fluctuations. sec- (NG) and temperature non-Gaussian primary CMB the of con- ondary features tight several established for and straints ΛCDM model mological t ( ity h ru ihes( richness estimate to group 1999) the Field Dey & Wide (Jannuzi use Deep (NDWFS) We NOAO Survey the data. from spectroscopic data 2012) photometric al. AGES the et from (Kochanek measured are se- redshifts Group groups al. et 2005). galaxy X-Bo¨otes (Kenter survey the Chandra the of in lected properties the present We at rdc h ubro rusta e -a sur- X-ray new that detect. we groups will regime, eROSITA, of group veys, number the the to ex- function predict By mass determined. the the is tending well how function estimate mass to cluster/group important is mass total measure the observables these how Understanding mass. properties -a bevtost eieteXryluminosity X-ray Chandra the the derive use ( We to observations members. X-ray galaxy five least at ytm eetmt eoiydsesos( dispersions velocity estimate we systems and efr iilaayi ooti h ais( radius the obtain to analysis virial a perform L avr-mtsna etrfrAstrophysics. for Center Harvard-Smithsonian bevtoi oVlno nvriaeFdrld i de Rio do Federal Universidade Valongo, Observat´orio do X ASINAAYE NPAC CMB PLANCK ON ANALYSES GAUSSIAN < z .W xmn h efrac ftegroup the of performance the examine We ). R L 500 opt 0 .Orfia apecmrss3 systems 32 comprises sample final Our ). n as( mass and ) Planck . 0 ih1 below 14 with 80, σ gr , L opt M aasrnl ii h level the limit strongly data CMB COSMOLOGY Planck and N .Bernui A. M gals MAPS 200 L aelt ofimdtecos- the confirmed satellite n h pia luminos- optical the and ) X and spoisfrtegroup the for proxies as , z 1 M 0 = 500 o ruswith groups for ) . 5 o these For 35. σ gr and ) R 199 200 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes n h 7 akapa ob qal ffiin to efficient equally be CMB to these all appear Gaussianize mask U73 the M82, and termed mask, minimum component separation nls eedn ntectsyms sd(l of (all the used by mask released cut-sky the them on depending angles, Planck rsn oeta n oiatglx,wiethe while galaxy, clusters dominant massive one More than substructure. more but a present BCM, of first-ranked CDG the not the is of structure (CDG) main Galaxy of the Dominant 20% Central about the for sample, Also, re- the and multi-modal. clusters substructured be be the to to 15% of other 50% unimodal, 35% be Only effects to vealed environment galaxies. and member evolution on cluster of study 1 foreground-cleaned sky analyze maps: full we nearly sphere, three CMB statistical the the kurtosis of patches and in- of de- skewness NG momenta on Gaussian large-angle based of directional dicators two forms be Using possible can tool all viations. one statistical identify single because to a data able that CMB expect in not signals does NG different for detections. quali- imprecise to quantitative leading and/or tative contributions primary with mixed 200 .A Caretta A. C. aeti apea seilysial eeec of (0.005 reference clusters suitable optical especially nearby an sample this substructuring, make and membership for im- analyses the masses proved beyond morphologies, properties, of medium of spectroscopic intra-cluster order range and large broad in The the galaxies content. sampling, member mass the stellar rank their al- to which us astrometry, data and lowed Near-infrared photometry for used applied. were were presence the substructures for and clus- of membership host for to tests their Strict relation of bright- state ters. their dynamical the and and structure of (BCMs) the members importance cluster the in est determine types, clusters, Bautz-Morgan to galaxy all confirmed order from spectroscopically 50 galaxies, 100 of member than sample more with a all studied have We ETA OIATGLXE N THE AND GALAXIES DOMINANT CENTRAL bevtoi ainl MCTI. Observat´orio Nacional, VLTO FTERHS CLUSTERS HOST THEIR OF EVOLUTION .d Anda-Su´arez de J. u eut hwta hs foreground-cleaned these that show results Our ait fmtosaebigue osearch to used being are methods of variety A Mu˜niz-Torres smica asehbtdffrn eeso Ga large at NG of levels different exhibit maps , 1 nilc .Andernach H. , 2 n .Hern´andez-Aguayo C. and , and , 2 .Santoyo-Ruiz H. , lnkcollaboration Planck sevem Planck 1 < z < .J Trejo-Alonso J. J. , . maps. .5)frthe for 0.150) 2 .A. M. , .The ). Planck 2 ABSTRACTS 1 , olwvr lsl oe a iha xoetof exponent an with law power − a closely The very catalogues ones. follow both oblate of are functions multiplicity 61% cumulative and ellipsoids prolate are ht3%o h ih(multiplicity rich obtaining the of on functionals, 39% Minkowski based that and superclusters, fits the ellipsoid for morpho- parameters determined We logical (25.4%). only formed A-clusters S-clusters superclusters new by between of addition S-clusters the for- and of (1.2%), the bridges (12.6%), with of cores mation superclusters A-cluster new around number SSCC): S-clusters total in ef- the superclusters of following of percentages the com- as found By (expressed we fects data. catalogues, optical both super- on paring all-sky based deepest catalogues the currently cluster 2 are from These multiplicities 39. with to con- superclusters redshifts), 1177 425 and spectroscopic taining A-clusters with 1227 (90% on S-clusters based (SSCC) alogue nlssw ple oteBlhicsooia sim- cosmological Bolshoi the similar to with applied also we significantly, is analyses less It though clusters. inconsistent, distributed randomly simulated of on based samples de- catalogues we function supercluster same for rived the with inconsistent clearly is uecutr ihmlilcte rm2t 2 the 42; ( to Southern 2 the is from other 601 multiplicities A-clusters containing with 3410 redshifts), superclusters on spectroscopic with based SuperClus- (92% Main (MSCC), all-sky the Catalogue is One ter (H.A.). us by of compilation one redshift cluster Abell/ACO the using fCG cusi rusta r omdt merge to doomed clusters. are evolution form that the groups and of in most cor- occurs that This CDGs sense of any. the if in one, goes only relation present ones massive less epeettonwctlge fsprlsesof of superclusters redshift of a catalogues within galaxies new two present We aut;Lm e oqe 0,Cl oa e Campestre, del Lomas Col. Mexico. 103, Le´on, Gto., Bosque, 37150, del Loma najuato; Valenciana, 2 (caretta,heinz,josue@as Col. ugto.mx). Mexico S/N, Gto., Guanajuato, Jalisco, 36240, Callej´on de Guanajuato; de 1 E AAOUSO UECUTR OF SUPERCLUSTERS OF CATALOGUES NEW 2 eatmnod ´sc,DICE nvria eGua- de Universidad F´ısica, DCI-CLE, de Departamento eatmnod srnmı,DN-G,Universidad DCNE-CGT, Astronom´ıa, de Departamento .Co Mart´ınez Chow M. . BL/C AAYCUTR PTO UP CLUSTERS GALAXY ABELL/ACO o SCand MSCC for 0 − 1 Caretta z .Andernach H. , 1 < δ . ∼ o SC hspwrlaw power This SSCC. for 9 0 − . 15 17 z 1 ◦ 0 = ueCutrCat- SuperCluster ) > . )superclusters 5) 5 constructed 15, 1 n .A. C. and , tro. XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes lto fteeouino h ag-cl structure large-scale the universe. of the of evolution the of ulation est fOfr,UK. 5 Oxford, of versity 4 3 Chile. tiago, 2 UK. cashire, 1 ([email protected], Gua- 36240, M´exico. Valenciana, [email protected]). [email protected], Guanajuato, S/N, Jalisco najuato, de Callej´on juato, 1 ntercneswl eg.Tersligbakhole black resulting The merge. will centers holes black their super-massive in the collide galaxies two As e.I a hrceitcsz ( Sur- size characteristic Sky has Digital It Sloan the the vey. in large of identified particularly catalogue been has of DR7QSO membership (LQG) high and group size quasar large A forcretivsiain t oaino h sky the on location Its is investigation. current our of esi,i stems xrm Q on nthe in found mem- LQG 1 and range extreme redshift size the most for both catalog the DR7QSO of is terms it In bership, z=1.27. redshift dimension longest epoch), ∼ present size, (proper Mpc h lws&CmuaoLGa h aered- same the at LQG Campusano shift, & Clowes the aa ta.(00 cl fhmgniyfrthe principle. for cosmological as- homogeneity the the of of challenges sumption scale thus and (2010) cosmology, concordance the al. with incompatibility et suggests Yadav early size the to Its in known appears Universe. currently Huge-LQG structure largest new, the be This examples. treme H IS IAERO OMCHISTORY COSMIC OF GIGAYEAR FIRST THE .G Clowes G. R. .E Forero-Romero E. J. UE-ASV LC OEGOT IN GROWTH HOLE BLACK SUPER-MASSIVE UELG H AGS TUTR IN STRUCTURE LARGEST THE HUGE-LQG- aionaIsiueo ehooy aaea CA. Pasadena, Technology, of Institute California Uni- Road, Keble Building, VA. wilkinson Blacksburg, Denys Tech, Astrophysics, Virginia Physics, of Department eatmnod srnmı,Uiesddd Guana- de Universidad Astronom´ıa, de Departamento eatmnod srnmı,Uiesddd hl,San- Chile, de Astronom´ıa, Universidad de Departamento ∼ 20Mc ebrhpo 3qaasadmean and quasars 73 of membership Mpc, 1240 eeihHrok nttt,Uiest fCnrlLan- Central of University Institute, Horrocks Jeremiah .Campusano E. 8 z . ere ot ( north degrees 8 1 = . 8 hc sisl n ftemr ex- more the of one itself is which 28, 1 .Raghunathan S. , .Velasco-Moreno S. H UNIVERSE THE .Graham J. 2 1 .K Sochting K. I. , .F Gomez-Alvarez F. M. , ∼ 1 p rjce)of projected) Mpc 615 5 2 .A Harris A. K. , volume 4 n M. and , . 0 1 / < z < 3 ) 1 ∼ and , 3 ABSTRACTS L. , 500 1 . 8 h rwho ue-asv lc oe uigthe history. during cosmic holes of black gigayear first super-massive of on growth constraints observational the the re-interpret to sults h otglx.W ou u td nbakholes black of on 10 center study range our the mass the focus at in We position until galaxy. stationary kick host a initial the the to since return BH its the we of by work amount accreted this the mass follow In to position techniques processes. initial semi-analytic use friction its well The dynamic to potential to returns galaxy’s velocity. due and the oscillates kick in it certain move while a will hole with black ejected be will o 8-0 dfii p Bogot´a, Colombia. Ip, Edificio 18A-10, No. 1 ewe h itne esrdo hyaecom- systematic the are minimize they to manage or they and measured difference patible a distances is the there between whether to on open exploration remains study further Our to supernovae. contrary of is results which the of energy approximate of group their distribution a account equitable of on taking measurements the microquasars, possi- perform this observa- we enable bility, the would the instrumentations that of and assuming tions expansion Afterwards, accelerating the universe. pos- measure is where to galaxies sible nearby to of supernovae measurement the Ia apply Type we end, gamma- this To and supernovae events. ray Ia Type between provide contrast to simulations a numerical reliable, with statistically supported is be it to supernova small actual rather is the population As microquasars. gamma-ray and from binaries events galactic gamma-ray of re- using measurement to distances, the method through alternative errors of an the present purpose duce to The is em- study method errors. this the systematic that contains found well-known was ployed on it based facts, is proven this and Although measure of universe. rate to su- expansion the candles accelerating These the standard and distances as both force. used zero repulsive are than a pernovae other Quintessence, constant of ex- cosmological and the a accepts of Relativity, General istence is to which interpretation, contrary One not rate. expanding accelerating is an universe at su- the Ia that Type -through observation- discovered pernova is it 1998, year the In UENVEADGMARYEET IN EVENTS RAY GAMMA AND SUPERNOVAE OTATN ITNE SN YEIA TYPE USING DISTANCES CONTRASTING eatmnod ´sc,Uiesddd o ne,Ca 1 Cra. Andes, los de F´ısica, Universidad de Departamento H OA UNIVERSE LOCAL THE 6 .Girola R. − 10 9 sn eueteere- these use We Msun. 1 201 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 1 1 uni- the of measurement the case expansion. calculate each verse’s we in as consistent we way, well are this as distances In the method. if supernova estimate Ia Type of error 202 htteGM eae sapwrlwgvnby given power-law obtained a We as behaves ζ masses. GCMF stellar the sample’s that this as well 5 k uvyD8ado okctlg fteDark the Digital of catalogs Sloan mock the Survey. on Energy from and DR8 data our Survey of real Sky some on present also results will cosmological I recent constrain allows time to aspects If relevant probes models. the galaxy these of of using some present abundance when will the I and clusters. galaxies cor- back- of the Universe include relations properties the These ex- of expansion. to acceleration ground attempt recent which the models al- plain investigate galaxies to of us properties lows clustering large-scale The l f55 aaisi h esitrne0 range redshift the in quan- galaxies 5558 new sam- function of survey a Field ple mass Deep FORS define cosmological the used we We galaxy evo- (GCMF). the purpose mass galactic named this Stoeger the tity For study & to (Ribeiro 1) lution. 592, surveys ApJ, galaxy 2003, from model derived data general observational semi-empirical to the a theory cosmological present uses connecting to which is approach work relativistic this of aim The asfnto atr on nteltrtr,where literature, stellar the galaxy in the found of pattern average This an function as mass interval. seen redshift be studied can result the in mass galactic . ( .R Lopes R. A. nvria ainld rsd err.Argentina. Febrero. de Tres de Nacional Universidad n t uioiyfnto nteBbn,as B-band, the in function luminosity its and 0 z nttt eFıia nvriaed S˜ao Paulo. de F´ısica, Universidade de Instituto ORLTO UCINADGALAXY AND FUNCTION CORRELATION ) H AAYCSOOIA MASS COSMOLOGICAL GALAXY THE ∝ OMLG RMTEANGULAR THE FROM COSMOLOGY .Lima M. [ M g ( 1 z 1 .Iribarrem A. , E-rzlconsortium DES-Brazil )] .Cmco .Aun,and Aguena, M. Camacho, H. , − 2 .R Stoeger R. W. . 3 FUNCTION CLUSTERS ± 0 . 4 where , 1 .B Ribeiro B. M. , 3 M g steaverage the is . 5 2 and , < z < ABSTRACTS r fsvrlnwgaiainlacssesand systems arc gravitational new more. several discov- the of data; ery spectroscopic BOSS com- with in bination measurements ob- mass and complementary models taining (HOD) distribution occupation halo constraining measure- galaxies, lensing SDSS-III/BOSS at galaxy-galaxy around ments 1; distribution order matter of dark redshifts the probing surement, aino h ag cl akmte distribution; matter dark infor- CMB-lensing scale first direct the large providing the statistics, on peak mation its to an and map measurement convergence give date lensing the contiguous will CS82 include largest the ongoing we They of and Talk, published projects. Short main scientific this the of In of overview value scientific survey. as- possi- the of the the fields enhancing many offers thereby in data, tronomy, applications spectroscopic exploring including of of and bility set UV the large Stripe- to a radio in the projects from future covering 82, and the Furthermore, existing of science. multitude cluster evo- galaxy galaxy as and such lution study addi- fields other the with in lensing, is applications gravitational focus tional Mak- strong main M. and Its weak Leauthaud, 0.6” of Waerbeke). A. mean Van a L. Kneib, mag- with ler, J.-P. to i-band down (PIs: optical area the seeing Stripe-82 in SDSS 24.1 the nitude in deg. sq. on aaaFac-rzlpoetcovering a project is Canada-France-Brazil (CS82) joint Survey Stripe-82 CFTH/MegaCam The de Rio 20080-090, ([email protected]). 43, Antˆonio, 2 Brazil Pedro RJ, Janeiro, Ladeira Janeiro, de 1 nvriyo Tokyo. of University 3 Universit´e. 2 1 nvriyo rzn,USA. Arizona, of University 3 Brazil. than earlier ones. assembled massive were less galaxies massive more Makler .Heymans C. Shan aia bevtr eerhGop twr Observatory, Steward Group, Research Observatory Vatican nttt eFıia nvriaeFdrld i eJaneir de Rio do Federal F´ısica, Universidade de Instituto H FTMGCMSRP-2SURVEY STRIPE-82 CFHT/MEGACAM THE bevtoi oVlno nvriaeFdrld Rio do Federal Universidade Valongo, do Observat´orio nttt o h hsc n ahmtc fteUniverse, the of Mathematics and Physics the for Institute CA etoBaier ePsussF´ısicas. Pesquisas de Brasileiro Centro ICRA, aoaor ’srpyiu eMrele i Marseille Aix Marseille, de d’Astrophysique Laboratoire .Moraes B. 8,9 1 .VnWaerbeke Van L. , .Woods D. , 6 1 .Hildebrandt H. , .P Kneib J.-P. , 4 .Charbonnier A. , Pereira × ha rs-orlto mea- cross-correlation shear 4 2 .Bundy K. , .Leauthaud A. , 1 4,5 .Miller L. , 1 3 n .E. M. and , .Erben T. , 7 3 .Y. H. , M. , ∼ 170 5 o, , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes hsc,Tigu University. Tsinghua physics, 9 Lausanne. de 6 5 Columbia. 4 8 Observatory. Royal Edinburgh, 7 of University omy, Colombia. 3 2 Colombia. 1 ouaino ag clsadteraiaino con- of realization simulations. the strained and galaxy scales the the large of on of population studies Applications morphological include reconstruction. method our in of sheets) and classification peaks the voids, (filaments, of environments results large-scale the and and function cells) in correlation counts distribution, char- (mean density detailed field density mass a imple- reconstructed present the the of detail method, acterization in the describe of We mentation as- explicit bias. any of of sumption independent are mass that cosmic field the of density As reconstructions the obtain from 7. we Release built result Data a al. (SDSS) Survey et Sky Yang Digital of Sloan catalogue method group the applied the We re- determined to haloes. to field of distribution density catalogue the matter halo by dark a the with construct it convolves simula- environ- and N-body its tions cosmological and from haloes computed matter ments density mass dark mass cosmic the of halo-based employs the distribution method a of The field. reconstruction of density the implementation for the method present We OPE UNESNEMDLWT A WITH MODEL QUINTESSENCE COUPLED eateto hsc n srnm,Uiest fBritish of University Astronomy, and Physics of Department AOBSDRCNTUTO FTHE OF RECONSTRUCTION HALO-BASED eatmnod iia nvria elsAds Bogota, Andes, los de Universidad Fisica, de Departamento ctihUieste hsc line nttt o Ast for Institute Alliance, Physics Universities Scottish aoaor ’srpyiu,EoePltcnqeF´ed´e Polytechnique Ecole d’astrophysique, Laboratoire readrIsiuefrAtooy nvriyo Bonn. of University Astronomy, for Institute Argelander eateto hsc,Ofr University. Oxford Physics, of Department ebi-ntttfu srpyi Potsdam. f¨ur Astrophysik Leibniz-Institut nttt eFsc,Uiesddd niqi,Medellin, Antioquia, de Universidad Fisica, de Instituto eateto hsc n snhaCne o Astro- for Center Tsinghua and Physics of Department .C Mu˜noz-Cuartas C. J. BEVTOA OSRIT NA ON CONSTRAINTS OBSERVATIONAL .C Nunes C. R. OMCMS EST FIELD DENSITY MASS COSMIC EEAIE EEOS DE GENERALIZED Forero-Romero 1 n .M abz Jr Barboza M. E. and 1 .M¨uller V. , 3 2 n .E. J. and , 1 ABSTRACTS ron- rale w ihitrcini h aksco a o eruled be data. not available can currently sector by scenarios dark out that the show in interaction we with results, good our in is with model agreement ΛCDM standard the Although ters. ()t u osrit nteESparameters EoS and the CMB BAO, on Ia, constraints SN put of to data H(z) recent most the use h akflisflosterelation the follows fluids dark the tbepaeo h oie trbnk inflation. Starobinsky the Modified the in of period, phase inflationary stable met- during of perturbations behavior the ric analyze contribu- we quantum Furthermore, the tions. on dependence essential any in term essen- Weyl-squared are the of conditions the sign stability the to the related of that tially conclusion is main work The detailed our equations. the these perform of analyt- to analysis both methods of numerical use and the ical on anomaly-induced and with corrections theory quantum the gravitational in of equations derivation wave radiation explicit considera- on the based The was to tion cosmologies. also dominated matter consideration and here the and spaces extend Sitter we de and about Minkowski taken literature of interesting effects stability an quantum is There with account. cosmological theory into classical the the in of solutions stability is purpose the first with explore Our background to perturbations. such metric of to stability respect the explore and then background, most isotropic the and equa- on homogeneous theory the general this derive in wave to gravitational is for tion purpose quantum first anomaly-induced Our with corrections. theory in gravity perturbations metric the of dynamics the consider We 1 Vit´oria. 2 Brazil. Catarina, Santa 1 e ud yasmn Emdldsrbdb the by described model DE a quintessenceparameterization mat- assuming dark a By the fluid. on with ter interacts constraints that put model energy we dark work this In RVTTOA AE N TBLT OF STABILITY AND WAVES GRAVITATIONAL .M Pelinson M. A. nvriaed saod i rned Norte. do Grande Rio do Estado do Universidade 1 eatmnod ´sc,CE nvriaeFdrlde Federal Universidade CCE/ F´ısica, de Departamento eatmnod ´sc,CMUiesdd eea de Federal CFM/Universidade F´ısica, de Departamento n Ω and classical OIIDSAOISYINFLATION STAROBINSKY MODIFIED OMLGCLSLTOSI THE IN SOLUTIONS COSMOLOGICAL m, 0 cino aumadd o manifest not do and vacuum of action o eetdvle of values selected for 1 .C Fabris C. J. , w ( .Shapiro L. a = ) w 0 2 + .O Salles O. F. , 3 w 1 β ρ ln m and β /ρ ( a x n that and ) ξ = 3 parame- n I. and , a − ξ 203 w we 0 , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 1 Brazil. Fora, de 3 204 3 2 ([email protected]). tce mgs h S2sre oee narea an covered survey (CS82) CS82 Survey of The 82 Stripe images. structural CFHT stacked galaxy the of in determination parameters the present We cp nafil eemndby determined field a in scope est(ilre l 2007). al. et code (Miller state-of-the-art lensfit the lens- with weak obtained CS82 elliptici- catalogue the ing with the comparison of a qual- determination through a ties, the on of focus assessment and ity outline above we described de work procedure the this S´ersic, 2-component In and SExtractor: Vaucouleurs+exponential. exponential in we Vaucouleurs, implemented particular de In per- models to the 4 objects. again across of use SExtractor PSF model-fitting run the the we form model finally, to and objects, PSFEx field, of use measurements we basic de- then the obtain perform and and to SExtractor features) tection use we model-fitting First, has PSFEx. (which v2.14.7 profile-fitting SExtrac- tor of a combination through a analy- with performed implemented morphological method is galaxies The of sis “forced the method. through SDSS), photometry” photome- (e.g. surveys the studies, other of in improvement evolution try the galaxy and lensing, to weak applications param- has structural galaxy eters of determination morphol- The galaxy ogy. and applications lensing for gravitational suitable involving specially CS82 makes mity − in mg ult ma eigof seeing (mean quality image .E .Pereira S. E. M. etoBaier ePsussFıia,Rod aer,Braz Janeiro, F´ısicas, de Pesquisas Rio de Brasileiro Centro eatmnod ´sc,IEUiesdd eea eJuiz de Federal F´ısica, ICE/Universidade de Departamento ntttdAtohsqed ai,Prs France. Paris, Paris, de d’Astrophysique Brazil. Institut Janeiro, de Rio Valongo, Observat´orio do ESRN AAYMRHLGE IN MORPHOLOGIES GALAXY MEASURING 1 HTMTI ESIT FQUASARS OF REDSHIFTS PHOTOMETRIC ∼ DNIIAINADETATO OF EXTRACTION AND IDENTIFICATION i bn oadphof depth a to -band E < DEC < 7 qaedgeswt h FT3 CFHT the with degrees square 170 .Makler M. IHNRO-ADFILTERS NARROW-BAND WITH H FTSRP 2SURVEY 82 STRIPE CFHT THE .Queiroz C. wti h DSsrp-2region) stripe-82 SDSS the (within 1 1 1 .Bertin E. , .Charbonnier A. , 1 n .Ru Abramo Raul L. and mag 3 AB n .Pereira R. and , − ∼ ∼ 40 1,2 4 t excellent Its 24. 0 A< RA < . )adunifor- and 6) .Moraes B. , 1 . 6 m 1 5and 45 tele- ABSTRACTS 1 , il 1 aed ˜oPuo u oMta 8,CP05800S˜ao 05508-090 CEP ([email protected]). Mat˜ao 187, Brazil do SP, Paulo, Rua S˜ao Paulo, de dade in htcnifr h aeinetmto of estimation Bayesian redshifts. the photometric inform and func- types luminosity can reliable that for need tions point-sources the and of sky, of distribution the the importance in of the modeling discuss li- good also spectral We a of inclusion stars. the codes, for include for redshift braries to need popular parallel how most the the discuss and of we some good in particular, very quasars In obtain these to for objects. redshifts how photometric de- and spectroscopic) efficient (near quasars, the of color- hamper and tection that color-color diagrams the over- to in magnitude up- how degeneracies discuss the the we as work come this such In J-PAS. surveys, with coming efficient narrow-band more or much pho- medium be accurate can with a redshifts, of quasars, tometric construction of HII the catalog and However, high-purity stars galaxies. diffi- from of quasars some regions distinguishing have in also culty surveys imaging ob- objects. these to Broad-band for unable redshifts photometric are accurate systems tain filter employing broad-band surveys optical imaging cos- many applications, for mological targets valuable are quasars Although hoydffr rmteoeepce nrelativity. in expected one the the expected to the from according that differs waves argue theory gravitational to of inter- possible of amplitude is rest the it than actions), weaker dimen- appearing theory extra (thus brane the sions to Since spread can gravity theory. that universe considers brane relativity the a general and results, distin- between of obtained observationally possibility the the guishing around With opened is discussion universe. describe brane that the equations the obtain field the to from in- analysis equation the wave the extending with later their of presented ob- on tention its is summation and consequences relativity brief servational general a on work, based rel- this construction general of In theory of the one ativity. of proofs constitute for systems searched physical most ef- different their on and waves fect gravitational of observation The O H RN NVREADPOSSIBLE AND UNIVERSE BRANE THE FOR e.d ´sc ae´tc,Isiuod F´ısica, Univers de F´ısica Matem´atica, Instituto de Dep. RVTTOA AE FORMULATION WAVES GRAVITATIONAL .D Rodr´ıguez-Camargo D. C. NUE ORCIN NAN ON CORRECTIONS INDUCED BEVTOA LEVEL OBSERVATIONAL Larra˜naga-Rubio 1 2 n .A. E. and i- XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes msin socr nbnr ytm,nest be to needs of systems, effect binary the in corrected. that occurs expect waves as gravitational to emission, involves is that it dissipation way, energy same the In OIE-N,Lpia84 ´roa Argentina. C´ordoba, 854, Laprida ([email protected]). CONICET-UNC, 1 1 aaygopctlge.Teerslswl appear will paper. forthcoming results a These in on catalogues. measured group functions galaxy correlation predictions anisotropic theoretical compare with to order simi- in a of model development lar before). the on authors working standard others are we the by Finally, noted of (as predictions model the halo %15 im- the account least into taking at halos that proves matter mass found dark prolate of have nature we more triaxial addition, and In to shape tend spherical profile. halos less massive the a most and have sense, this surrounding shapes In the with structure. halo halos matter of dark well of the alignment dependence recover mass results ob- numerical known model the fitting of by parameters in tained The particularly scales, regime. of 2-halo those range the of wide able a measurements over is numerical functions model the our cross- reproduce that shape anisotropic to found halo called have We are by correlations. functions given These directions axes. the function on cross-correlation method the depending integration of instances Carlo obtain Monte we a Using cross-correlation function. halo-matter gen- the derive the for we expressions of eral and particular, alignment In shape the structure. halo describing surrounding law the probabilistic of a distribution profiles, density probabilistic halo the a which for halo distribution model triaxial matter classic a large-scale includes the the of for version model extended an present We inld ooba apsBgta oo´,Colombia Bogot´a, Bogot´a, Campus Colombia, ([email protected]). de cional 2 co). ([email protected]. Bogot´a, Bogot´a, Colombia Campus .A Sgr´o A. M. eatmnod ´sc,UiesddNcoa eColombia de F´ısica, Nacional Universidad de Departamento bevtroAto´mc ainl nvria Na- Universidad Nacional, Astron´omico Observatorio nttt eAtoo´aT´rc Experimental, y Te´orica Astronom´ıa de Instituto NSTOI AOMODEL HALO ANISOTROPIC 1 .J Paz J. D. , Rodriguez 1 .E Merch´an E. M. , 1 1 n F. and , ABSTRACTS , 1 bl -a nra”(X)eitn lses The 50 clusters. of g emitting sample (AXN) another “normal” for X-ray found Abell re- ones colour-magnitude the their with lations of com- parameters We the systems. galaxy pared such the compose of which stages populations that evolutionary properties the unveiling elucidate underluminous at may X-ray aiming Abell clusters 54 re- of (AXU) colour-magnitude sample the a for of lation analysis an present We oteoe htwl eue yJ-PAS. by used be will similar that filters ones band the narrow of to ALHAMBRA set the a and had which Survey survey, Sky from Digital images to Sloan we pipeline the results our some applying show when we obtained Then subtraction selection. image source as such Ia and pipeline, indi- type the each of detect step describe to vidual we developing First sketch J-PAS. are a with we present supernovae we pipeline Here the optical. narrow of 56 the of in a system filters a be band with will equipped instrument telescope main m 2.5 The clusters. supernovae Ia galaxy type and oscillations, Uni- acoustic the baryonic of Spain. as expansion such observables Javalambre, the cosmological different study de through to verse is Sierra goal in main The built being fa- astronomical cility an is (J-PAS) Survey Universe Astrophysical Accelerating the of Physics Javalambre The hnANcutr,b ieec faot42% about of 0.05 of difference flatter range a redshift always surveyed by are the along clusters clusters, AXU AXN for than redshift, slopes with change the slopes but sequence red the trend: relations. colour-magnitude the constructing for v to aSler ao,19 14-7,Rod Janeiro, de Rio 21941-972, 149, ([email protected]). Ramos, Brazil Silveira da Athos Av. ls u o h X lses hsi systematically is this clusters, sam- AXU both the for for redshift but with ples, grow to found re- was colour-magnitude lation the of scatter intrinsic the Also, Lagan´a .B Siffert B. B. nttt eFıia nvriaeFdrld i eJaneir de Rio do Federal F´ısica, Universidade de Instituto H YEI UENV IEIEFOR PIPELINE SUPERNOVA IA TYPE THE and H E EUNEO X CLUSTERS AXU OF SEQUENCE RED THE efudta ohsmlsso h same the show samples both that found We .J Trejo-Alonso J. J. H AAABEPYISO THE OF PHYSICS JAVALAMBRE THE SRPYIA UVY(J-PAS) SURVEY ASTROPHYSICAL r 2,3 Neto antdsfo h DSD7wr used were SDSS-DR7 the from magnitudes .Sodr´e Jr. L. , CEEAIGUNIVERSE ACCELERATING 2 1 n .Mne eOliveira de Mendes C. and , .R .Reis R. R. R. , 1,2 2 .Cypriano E. , .A Caretta A. C. , 1 n .O Calv˜ao O. M. and , 2 .B Lima B. G. , 1 ≤ .F. T. , 2 < z 0.20. 205 1 o, XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes u,RaGl˜oBeo66 iedd,CP 10-0,S˜ao Brasil. 01506-000, SP, CEP: Paulo, Liberdade, 686, Galv˜ao Bueno Rua Sul, ais(t9 e etcndne.W ru htthe that ga- argue We passive confidence). field cent per in 95 those (at laxies than smaller average an even with the stretch Ia field, SNe host the galaxies passive than cluster’s galaxies passive of concentration optbea h urn ee,tersrthdistri- are stretch ( properties their different Ia are level, butions current SNe the cluster that, at show and compatible then field We most outliers. of possibly while exclusion detected, the be to not due can could Hub- galaxies scatter the active in residuals differences in ble Reported Ia values. SNe samples these of random reach set of our cent from per drawn 0.02 corrections. only colour that and show We stretch after luminous more 2 M´exico. ([email protected]). G najuato, Guanajuato, 36240, Valenciana, S/N, Callej´on Jalisco de 1 galaxies, of gas. nor- and groups than galaxies accreting individual systems possibly younger points clusters, being This mal clusters latter. the AXU for to those signif- than are flatter that that icantly find slopes we red-sequence substructure, shows no former the or and little significant with AXU with other the one the subdivide subsamples, we two When in clusters 31%. about by larger 206 f25(2 gis .51),adta are that and 3.35(14)], with against Ia 2.54(22) [ of SNe relation host colour–luminosity weaker galaxies stretch, smaller passive galaxies. passive that be- and confirm active differences and We in known residing samples for Ia our SNe looked tween test first To we methods, curves by technique. assessed light resampling was Their differences a sig- observed the the and field. of model nificance the SALT2 the in by parametrised Ia were properties residing SNe their Ia 1015 compare SNe and with 48 clusters identify galaxy rich to measured in project redshifts BOSS the with and by data catalogue cluster supernovae galaxy SDSS–II GMBCG the used We 3 Uni- Brasil. Cidade SP, Mat˜ao S˜ao 1226, versit´aria, Paulo, do CEP:05508-090, Rua S˜ao Paulo, de Universidade nttt eAtooi,Go´sc Ciˆencias Geof´ısica Atmosf´er e Astronomia, de Instituto eatmnod srnmı,Uiesddd Guanajuato, de Astronom´ıa, Universidad de Departamento ´ ce eAto´sc eoia nvriaeCuer d Cruzeiro Te´orica, Universidade Astrof´ısica de N´ucleo RPRISO YEI SUPERNOVAE IA TYPE OF PROPERTIES .S Xavier S. H. ’nra .A rea,L abn,P M. P. Galbany, L. Frieman, A. J. D’Andrea, anvc,J arnr .C ihl .D. M. Nichol, C. R. Marriner, J. Garnavich, lsed .P cnie,adM Smith M. and Schneider, P. D. Olmstead, NIERC AAYCLUSTERS GALAXY RICH INSIDE 1,2 .R ut,M ao .B. C. Sako, M. Gupta, R. R. , ∼ 3 σ :bsdshvn higher a having besides ): ∼ 0 . mag 1 ABSTRACTS icas, ua- β o otSeI ihsalrsrthta on passive young than galaxies stretch ( passive smaller galaxies old with show, Ia we SNe as host since, responsible is effect clusters this in for galaxies passive of age older yvna hldlha A USA. PA, Philadelphia, sylvania, 2 Brazil. SP, 1 1 eCie atao Chile. Santiago, Chile, de osrcinpaei 05ad21A ihex- with 2017A. 2016A, and and 2016B in 2015 by Commissioning followed in pected 2014, phase starting late is in construction completed Phase a be Design will The and now 2013. Agency in State Research, Chilean full of the granted CONICYT, been having from visi- and funding a 2012 as in Directors instrument of tor Board SOAR been the having by stage, approved Design in- Conceptual The at data-cubes. run is strument the will produce application and PanView instrument the open- a NOAO and run CCDs (the Torrent system) to three be controller source will The detector cameras The three efficien- the image. camera. the each optimise 2k of to x cies field coatings 2k arcmin different have 7 a will x onto and 7 view wheel a of imaging filter CCD230-42, camera, science a a nm. encompasses 550 field and arm wide 390 Each at a dychroics of two feeding consists collimator design optical Follow-Up. Ex- Microlensing BOMBOLO 3) 4) UV/Optical and Phases; Transits Near Evolutionary oplanetary Stellar 2) of Phenomena; Diagnostics Stud- Accretion Flickering of Multiband ies Simultaneous 1) science leading cases: following to minute-to- the able with the timescales, in be second events will unexplored largely BOMBOLO address events. rapid for astronomical The capability imaging independently, synchronized wavelengths. and providing simultaneously optical work arms and cov- three imager near-UV three-arms a the is ering it Chilean kind, fully its first of The instrument instru- observatory. SOAR visitor for multi-passband ment new a is BOMBOLO .Angeloni R. ERU/PIA MGRFRTESOAR THE FOR IMAGER UV/OPTICAL NEAR etod sr-neirı,PnicaUiesddCat´o Universidad Astro-Ingenier´ıa, Pontificia de Centro nttt eFsc,Uiesdd eSoPuo a Paulo, Sao Paulo, Sao de Universidade Fisica, de Instituto eateto hsc srnm,Uiest fPenn- of University Astronomy, & Physics of Department OBL:AMLIBN,WIDE-FIELD, MULTI-BAND, A BOMBOLO: ∼ 4 1,2,3 INSTRUMENTATION σ ). .Guzm´an D. , MTELESCOPE 4M Infante 1,2 1 .H Puzia H. T. , 2 n L. and , lica XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 2 3 Chile. Santiago, Chile, 7 E 8490 lra´pls at aaia Brasil Catarina, Santa Florian´opolis, Postal 88040900, ([email protected]). Caixa CEP Lima, Ferreira 476 Jo˜ao David Campus Catarina, 1 iuain n h hsclexperiments. physical numerical the per- the and between experiments simulations correlation flexible perfect more a much mitting for screens allow phase as a will benches at optical light in spatial modulators incident of phase Integration the milliseconds. to of shift resolution programmed time phase with be a screens can introduce phase that to replace modulators to phase planning spatial there- screens, are phase we with This fore do screen. to impossible phase almost our simu- is same to the patterns apply turbulence tests to lated these like make would To we realistic telescope. more the bench our on on testing algorithms before these test to like distortion.We then phase would the correct and to involves algorithms turbulence work testing of Our simulations make. numerical to computing hard and which expensive screens, are phase different pat- several turbulence needs new one terns test of To light effect the atmosphere. of simulate changing to beam a plate phase incident this move are the we screens than and Phase bigger screen. much phase a made called atmosphere, is the imi- plate by to this caused etched distortions is phase surface turbulence the whose tate beam the plate light glass experiment the a directing bench through than by the achieved rather are In elongated distortions an the circle. as see class a telescopes star 30m large artificial a such by of sodium viewed edge artifi- The when an star in telescope. observed laser effects sodium experiment the cial This reproduce effects bench. to optical the aims an recreate We on to turbulence optics. experiment of adaptive an of of reso- designing correction goal of are The the loss is telescope. distortions to these a leads in into This achievable wavefront lution plane wavefront. a distorted transforms a light stellar incom- of ing path optical the in turbulence Atmospheric TOPEI UBLNESIMULATIONS TURBULENCE ATMOSPHERIC a-lnkIsiu ¨rAtooi,Hiebr,German Heidelberg, f¨ur Astronomie, Max-Planck-Institut nttt eAto´sc,PnicaUiesddCat´oli Universidad Astrof´ısica, Pontificia de Instituto rp eAto´sc,Uiesdd eea eSanta de Federal Universidade Astrof´ısica, de Grupo IHSAILLGTMODULATORS LIGHT SPATIAL WITH .Bernardi R. 1 .Kanaan A. , 1 n .Mello A. and , 1 ade ca ABSTRACTS y. or h atsstliemsini 08 MIRAX 2018. in mission satellite Lattes the board at ri 60k liue 15 low- altitude, in km launched (650 be as- orbit X-ray will for Earth hard that a Institute experiment is (MIRAX), National tronomy Brazil, X (INPE), the Research Raios Space at de development Imageador under e Monitor The ([email protected]). 2 Braz Catarina, ([email protected]). Florian´opolis, Santa Ferrei 88040-900, CEP: Jo˜ao David Lima, Universit´ario Reitor Campus catarina, 1 iiyo u approach. feasi- our the demonstrating of masses, bility air different single co- at a the of star of monitoring values the the through obtained of extinc- efficients sigma atmospheric two the within different that is for moments show at calculated results star coefficient Our each tion for instant. mass given air a versus magnitude ap- with parent are tables multiple tables the into photometry converted using subsequently These image At PHOT. each on routine time. did all IRAF and and them positions of date star photometry any of the tables on created we falls point in star this exactly a know we pixel distortions camera. which the the we out by images, finding caused the After distortion on of the positions group determine actual can a their for with calculated stars positions CCD. the the on coordinates Comparing pixel to and them stars converts program the then for Python altitude a and azimuth developed calculates for We that masses instant. air the different same measure at the stars to several extinction method of the a brightness estimate developed To we lo- coefficients Pachon. Camera) obtained Cerro AllSky were at (SOAR used cated SASCA images camera The the by night. same the coeffi- moments various in instantaneous for extinction the site. atmospheric compute of astronomical cients to an how study show in the We to conditions alternative atmospheric great a of are cameras sky All H ADXRYTLSOE O MIRAX FOR TELESCOPES X-RAY HARD THE Rodrigues er oooItrainlOsraoy aSrn,Chile Serena, La Observatory, International Tololo Cerro eatmnod ´sc,Uiesdd eea eSanta de Federal Universidade F´ısica, de Departamento .S Bortolotto S. G. XICINCEFCET IHAN WITH COEFFICIENTS EXTINCTION .Braga J. .Barthelmy S. 1,2 1 .E Grindlay E. J. , .D’Amico F. , N PROTOMIRAX AND LSYCAMERA ALLSKY 1 .Kanaan A. , 3 n .E Rothschild E. R. and , 1 .C. M. , 2 .Allen B. , 1 n .Walker D. and , ◦ Avila ´ nlnto)on- inclination) 2 .Hong J. , 1 .H. B. , 4 207 2 2 ra , il XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ilhv 20 It a pattern. have basic will (MURA) Array Redundant formly O)ada nua eouino 1.5 of resolution angular an and FOV) akwt 0m pnnsi 13 a in openings mm 20 with mask a f13 of ray 10mm . msailrslto n nae f20cm 250 of area an a have and will resolution T2 spatial for mm Astro- 0.6 plane for detector The Center (CfA). Smithsonian physics Harvard devel- the being are at de- (T2) oped telescope CZT second imaging the The for tectors kbps acquisition. 500 op- data a real-time and for as eration attitude capability well command an as and with systems telemetry gondola pointing balloon and a control in mounted be ilpoieiae ih6 pattern with random images provide a will with mask tungsten 0.3mm-thick o etn n eosrto;ti eeomn is development the this demonstration; called and testing for 20 eut ftepooIA eetr eecp and telescope developments. present detector, gondola and protoMIRAX balloon MIRAX the of of status results current the describe aionaSnDiego. San California 4 3 2 Brazil. search, 1 devel- in been has INPE (T1) at telescope opment One semiconductor detectors. imag- room-temperature solid-state coded-aperture cadmium-zinc-telluride (CZT) with two equipped telescopes in ing essentially consists 208 yi ihattd ( altitude high a in fly t eiiisrmns eSGAIpoiea provide GeMS/GSAOI facil- complex instruments. Op- and Gemini Adaptive unique ity are South (GSAOI) Gemini Imager the tics Sys- and Optics (GeMS) Adaptive tem Multi-conjugate Gemini The .Lopez A. .Moreno C. .Araujo C. ESGAI RMCMISOIGTO COMMISSIONING FROM GEMS/GSAOI: srpyisDprmn,Ntoa nttt o pc Re- Space for Institute National Department, Astrophysics AAGdadSaeFih Center. Flight Space Goddard Astrophysics. NASA for Center Smithsonian Harvard ◦ etrfrAtohsc n pc cec,Uiest of University Science, Space and Astrophysics for Center × .Winge C. PRTOSADSINERESULTS SCIENCE AND OPERATIONS .R Carrasco R. E. .Arriagada G. .Boccas M. 20 × .Collao F. 10mm ◦ × 1 WMFV nti rsnainw will we presentation this In FOV. FWHM 3CTpaa eetr ihdimensions with detectors planar CZT 13 .Trujillo C. , 1 rtMRXproject protoMIRAX 1 .Vucina T. , .Marchant C. , 1 × ◦ .Vidal F. , m n mtikla coded lead mm-thick 1 a and 2mm × 2 1 .Dorgeville C. , .Trancho G. , ′ 20 srpyisDvso n will and Division Astrophysics s 1 .Rambold W. , 1 ◦ .Neichel B. , ul-oe edo-iw(FC- field-of-view fully-coded 3 1 .Galvez R. , 1 .Montes V. , .Pessev P. , ∼ ′ 1 nua eouinwt a with resolution angular 3k)bloni 2014 in balloon km) 43 .Collao F. , 4 n .Bec M. and , 2 .Fesquet V. , 1ue nar- an uses T1 . 1 × .Rigaut F. , 1 1 .Luhrs J. , 3MdfidUni- Modified 13 .Gausachs G. , 1 1 .Serio A. , .Urrutia C. , 1 .Diggs S. , ◦ 1will T1 . 4 1 1 2 , , , 1 , 2 ABSTRACTS A . 1 1 1 , , , eut rdcdb eSGAIdrn h sys- the process. during verification GeMS/GSAOI tem by scientific per- produced the system results present this and the In efficiency details on-sky results. formance, in science describe GeMS/GSAOI first we 2012 the presentation on-sky of produce of to end nights started the 90 at than more commissioning, and work dedicated 4 3 University. National tralian 2 1 1 ety h iso ceue ob anhdi 2020. in launched be to Cur- scheduled mission collaboration. the international rently, wide a and include mission to mm. Russian-led is a 3 as proposed to is a micron Millimetron 50 GHz, array covering mm 5000 a camera/spectrometer in and and camera/spectrometer 500 operating array from receivers submm between heterodyne to bands of is several package set and instrument a cooling passive The include by 4.5K coolers. compartment to mechanical down instrument cooled and be mi- ad- telescope 10 will be than The to less are accuracy cron. rms mirror an primary achieve the to justable space of in panels deployed the be galaxies, will and of telescope of The evolution evolution etc. systems, as- quasars, and planetary and formation and the astronomy stars as in sys- ad- such problems can VLBI trophysics that key space-earth capabilities various a scientific observa- have dress of single-dish will element It a an tem. as as operating operate or two can tory submm has one and facility far-infrared The modes: the range. for observatorywavelength optimized space is cooled that 10-meter a is Millimetron tre ttebgnigo 01 After 2011. of beginning commissioning the GeMS/GSAOI at The started sky. 85” the of on view near- 85” of x at field a quality over wavelengths (NIR) image infrared limited diffraction uniform, UFC AE UBLNEPROFILING TURBULENCE LAYER SURFACE IHTES-LDRADLSIA ESO AT LUSCI AND SL-SLODAR THE WITH eerhSho fAtooyadAtohsc,TeAus- The Astrophysics, and Astronomy of School Research eiiOsraoyAR,Nrhr prtosCenter. Operations Northern Observatory/AURA, Gemini in aelnTlsoeOrganization. Telescope Magellan Giant Center. Operations Southern Observatory/AURA, Gemini ALMA. AAA OBSERVATORYPARANAL .d Graauw de T. MMTRON 1 ∼ er of years 2 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes od uhm UK. Durham, Road, 6 Chile. Chile. ena, Serena, La 601, Casilla 5 Pino El Colina Chile. Antofagasta, 02800 4 Antofagasta de U. Germany. Muenchen, bei 3 Garching 2, Strassee 2 ([email protected]). Chile. Chile, 1 idsedi rtclprmtrt etkninto taken data. the be of to treatment parameter the the that critical before suggests a account also is m/s speed 3 wind than lower with speed connection in wind instruments dis- two the the Furthermore, of Layer. agreement pro- Surface turbulence the further of for reliable instruments analyses more both have from measurements to file allow than higher m/s m/s. speed wind 3 3 that than suggests higher result is last platform This Paranal the on (SL). only speed ground above m 20 first This the SL- in same. the also the valid much is form pretty are integrals Around LuSci low and the the SLODAR value, sample turbulence. Kolmogorov fully the to the and of short low components too is are frequency speed sets wind data this the the value) signifi- that law is indicates (Kolmogorov BETA generally 3.667 When the than whether trusted. less indicate cantly be to can intended tool profile is diagnostic Cn2 It a SL-SLODAR. as the purely by delivered trum profile. Layer the Surface Paranal finely compare the and reliability characterize to their two order enforce to the in instruments two from analysed data are Simul- profiling instruments 2008. Layer since Surface out 2012, taneous carried measurements being during (LuSci) are Paranal campaigns Scintillometer at Lunar used while been Slope instrument has Layer (SL-SLODAR) prototype Ranging Surface And at a investigation Detection Observatory, Layer Surface Paranal the ESO of context the In .Lombardi G. OT O:RVAIGTEPOLARIZED THE REVEALING POL: SOUTH uoenSuhr bevtr,Csla101 ataode Santiago 19001, Casilla Observatory, Southern European nvriyo uhm eateto hsc fI South CfAI, Physics of Department Durham, of University UACI/OO oiaE ioCsla63 aSer- La 603, Casilla Pino El Colina AURA/CTIO/NOAO, nvria eAtfgsa nddd srnma Av.. Astronomia, de Unidad Antofagasta, de Universidad a apnsOs,Crei nttto fWashington, of Institution Carnegie Obs., Campanas Las uoenSuhr bevtr,Karl-Schwarzschild- Observatory, Southern European ohisrmnsarevr elwe h wind the when well very agree instruments Both spec- power turbulence the of slope the is BETA Avila ´ 4 .Navarrete J. , Wilson 1 .Sarazin M. , OTENSKY SOUTHERN .M Magalh˜aes M. A. 6 n .Butterley T. and , 1 .Tokovinin A. , 2 .Char F. , 1 3 .Gonz´alez C. , 6 5 .W. R. , ABSTRACTS hl.Teiiilga st oe h k south sky the cover to is goal declination initial of de- The CTIO, newly at Telescope. installed a Chile. be Robotic use will 80cm polarimeter will and an Telescope sky It for Southern polarimeter the light. signed of polarized survey optical a in be will POL SOUTH lospotdb CNPq. by supported also project. describe the will of We status current assembled. the electronics and optics others. Solar Forma- and among Explosions Star System, Stellar Clouds, Envelopes, Magellanic Stellar and tion, Galaxy the Medium of Interstellar Astronomy, of Extragalactic field ogy, a covering camera degrees. a square 2.0 with about V=15, accuracy polarimetric to a down at aiming time, ing Paulo. 1 aelt iso,agon nrsrcuecompati- MIRAX INPE infrastructure the with ground ble for a pathfinder mission, Considering re- a satellite is was station. protoMIRAX ground updating that balloon software the on for quired experiment. effort astronomy significant involved X-ray A engineers protoMIRAX a system the were ground in INPE the at scientific to available challenge the facilities reusing ground for balloon requirements system The rprycngrdwt tent a xeddthe computer, extended has server Ethernet, new with configured A properly and (CRS). Control System the Reception operation, protoMIRAX de- solution for ground signed the present We frameworks. using and elements by software object-oriented satellites customized different several oper- and of particular requirements commanding with ational satellite complies SATCS for monitoring. INPE Con- at SATellite architecture software-based developed the a of (SATCS), use System flights. trol make balloon and will the control approach during This to experiment recommended the highly monitor and useful be eatmnod srnma A,Uiesdd eS˜ao de Universidade IAG, Astronomia, de Departamento MRVN INPE IMPROVING Fernandes hspoeti upre yFPS.AMis AMM FAPESP. by supported is project This its and built being currently is polarimeter The Cosmol- as such areas impact will POL SOUTH AIIISFROEAINO THE OF OPERATION FOR FACILITIES .Mattiello-Francisco F. RTMRXEXPERIMENT PROTOMIRAX 1 .Cardoso L. , ′ − aelt prto prahwould approach operation satellite s 15 ◦ naottoyaso observ- of years two about in Braga ′ ALO GROUND BALLOON S 1 1 .Cardoso P. , 1 .Rinke E. , 1 .O. J. , 1 n J. and , ≤ 0.1% 209 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes apsUiestai etrJ˜oDvdFrer ia Fl rian´opolis, Brazil. Lima, Ferreira Jo˜ao David Universit´ario Reitor Campus 1 (fatima.mattiello@inpe. Brazil br). 12201-970, CEP SP, Campos, 1 protoMIRAX the onboard balloon. the computer by provided handling services data the with compliance in tion, communica- ground-balloon for to (PUS) Utiliza- Packet Standard order the tion in address SATCS to frameworks the the in extend used widely are process- and metadata libraries telemetry component-based functions Design-patterns, and kernel ing. command the protoMIRAX for SATCS of re- the development gateways customizing CRS is the TCP/IP downlink Currently, SATCS. and to by uplink quired mapped available or- being the in channels support (OPS/SERVER) to software con- der switch, new with and facilities verters station ground existing 210 nusi mle roswt epc oohrcen- other to respect use. in with techniques errors troiding algorithm smaller new in the methods. incurs that existing on confirms than results based accuracy Simulation technique po- better new spot with the a sition measuring present for networks We neural artificial et 2008). (Thomas conditions these al. under do Gravity well Typical of perform Center not as sensor. such wavefront will algorithms star the centroiding guide in the of for elongated image return appear the photon stars, sodium as guide the laser atmosphere the of upper use the the in and layer telescope the the star to of Due guide diameter sensor. laser wavefront Shack-Hartmann a a using and wavefronts measurement scales. aberrated chal- accurate the these the of of at is number challenges system a these AO of are One an There implement to up 2006). diame- ground lenges the in al. from meter et systems AO (Nelson 30 require have than will will and more ter telescopes of of mirrors generation Optics primary Adaptive next as The nec- known is technique (AO). a it use turbulence, to atmospheric essary the tele- to ground-based due a in scopes lost resolution the recover To HC-ATANWVFOTSENSORS WAVEFRONT SHACK-HARTMANN et fPyis nvriaeFdrld at Catarina, Santa de Federal Universidade Physics, of Dept. nttt ainld eqia saii,C 1,S J. S. 515, CP Espaciais, Pesquisas de Nacional Instituto E LOIH O ETODN IN CENTROIDING FOR ALGORITHM NEW SN RIIILNUA NETWORKS NEURAL ARTIFICIAL USING .T Mello T. A. LNAE PT FOR SPOTS ELONGATED 1 .Kanaan A. , 1 n .Guzm´an D. and , 2 ABSTRACTS o- aoiad hl,Vc˜aMcen 80 atao Chile. Santiago, 4860, Vicu˜na Mackenna Chile, de Catolica 2 1 2 fezs h lwsen mg oincomponent. motion image measurements of seeing slow frequency approach the high “adiabatic” “freezes” with The Heliometer binning. Rio suggest- wider dispersions, a statistical ing than larger are heliolatitude: or they time in either between binned values differences averages the enlarge accuracy. perturbations the timing These the than from larger calculated ran- values times with expected hundreds measurements perturbations transits dom affect diameter solar they the of scales (32’): frequency to low acting Hz) are (0.01 (2013) seeing Heliometer mea- Rio refractions with each Anomalous sured of 1955). dispersions (Gething, statistical aver- value annual than between larger scatters were the ages be- data: Rio (1850-1940) as Greenwich have Campi- and Rome corrections. (1877-1937) at refraction’s doglio measured series after (1992- transits SDS remains Meridian and data equatorial (2008) an RHESSI 2011) than circles: larger solar altitude excess timing fixed by across heliolatitudes, the transits all 1998-2009 at in diameter measured As- Janeiro solar The de Rio Relativity. of trolabe General of to theories constraints alternative dynamical so- determine the to measured oblateness (1967) Dicke lar length. proportional chord’s is the 0.5” to disk, of solar reduction horizontal the the of while deformation vertical (1805) the formula computes Laplace’s S´ejour (1786). Du in ap- (0.5” diameter all pears solar at vertical of (0.5” refraction of horizontal differential and formulation altitudes) horizon) at modern 35’ to A zenithal 1600. af- law ter refraction and the Snell independently Kepler, found Harriot, Descartes altitudes. various at correct nova The forgotten. remained (984) bottle. ap- Sahl curved coin Ibn a of a in work like water horizon the under at pears (1278): bigger Alhazen supposed Witelo was (831), and Sun (1256) Farghani Sacrobosco re- Al (1020), atmospheric influencing modeled AC) fraction 150 (about Ptolemy OPTN IFRNILREFRACTION DIFFERENTIAL COMPUTING bevtoi ainl i eJnio (sigismondi@icra Janeiro. de Observat´orio Rio Nacional, ITNE:AHSOIA PERSPECTIVE HISTORICAL A DISTANCES: nentoa etrfrRltvsi srpyis Rome Astrophysics, Relativistic for Center International TALHLOAIUE N ZENITHAL AND HELIOLATITUDES ALL AT et fEetia niern,PnicaUniversidad Pontificia Engineering, Electrical of Dept. yh esrdterfato nte17 super- 1572 the on refraction the measured Tycho .Sigismondi C. 1,2 n . Boscardin S.s and 2 .it). . XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ol-ie o nyt h SadGra primary German and ob- US communitypartners. the offers astronomical to only whole it not the world-wide, observatory to international time serving how- an (DLR), as Agency Space ever German the and NASA be must CCAT and ALMA with explored. Synergies to years the many be Herschelcome. will for As SOFIA facility 2013, FIR-astronomical 2015. April premier in in cryogens implemented operations of be full out ran will of instruments time 7 the when by of potential, suite future full its the and science early SOFIA Clouds. Large Magellanic fre- the Small in THz and regions at forming hemisphere star observed including southern has quencies, the total and in a successful) targets them for of key Zealand (all New flights to 9 of deployed re- Cycle has of A, part & SOFIA as A 1, 2013, and July Letters in ApJ Meanwhile, of spectively. issues special in mid- 2012 in published were which high- spectroscopy heterodyne imaging resolution re- (THz) mid-infrared far-infrared exciting in in and of (5-40mu) both number discoveries, science a early and delivering 30 sults 2011, some in completed has flights and 2010 Dec base. to returning before flight hours observing 10 typical for lasts a in the base and in its California, from ft operates Palmdale, normally 45000 SOFIA wa- as precipitable vapor. the ter high of percent as with 99 above flying aircraft stratosphere telescope 747SP 2.7m Boeing a a In- is for Astronomy, Observatory frared Stratospheric for short SOFIA, nv fSutat Germany. Stuttgart, of Univ. 1 usto eeoe nsiniciiito rga - program initiation ac- scientific data for in software developed the quisition present to aims article This OI cec etra AAAe,UAadDIat DSI and USA NASA-Ames, at Center Science SOFIA OI samjrbltrlpoetbetween project bilateral major a is SOFIA of highlights few a present will I talk, this In in observations astronomical started has SOFIA IHIHSADFTR SCIENCE FUTURE AND HIGHLIGHTS NTUTOA SPECTROSCOPES INSTRUCTIONAL H OI IBREINFRARED AIRBORNE SOFIA THE AAAQIIINSSE FOR SYSTEM ACQUISITION DATA BEVTR IS SCIENCE FIRST OBSERVATORY - .B .B Almeida B. S. B. C. ECIG&OUTREACH & TEACHING POTENTIAL .Zinnecker H. 1 n .Hetem A. and 1 1 ABSTRACTS @aluno.ufabc.edu.br). 1 ai ae h nlrsl saone-dimensional a analyzed. is subsequently be result can final that The spectrum monochro- wave. each of matic characteristic with incidence photons the the compare spectro- of can the one which have calibrating We through for scope, tool. of method of steps type a this usual implemented of the analysis by and ac- followed reduction executes data processing, one for data acquisition, camera image the a the and side After media the quisition. in diffraction made a allow slit it, not a of through does except a that enter, box is to a light used equip- of spectra This consists of basically spectroscope. ment origin rustic of The model by today. simplified built use language spectrometer a wide C++, a in in of built was design program The the students. in use for IC, tra etutrto fteitrainlEditorial international the of ed- recent restructuration the itorial as well and as theoretical frameworks, and methodological authors Brazil than of other participation countries from arti- articles, refereeing, of of as rate writing such discussed, acceptance the also in of are submitted tradition aspects cles Important publishing education of astronomy area. ab- lack of the ongoing the mass” the and “critical papers, researchers a for of call and sence dissemination journal proper a the in Edito- of succeed nominated not initially did the Board the rial Among that articles increase mention of number can an low submitted. we relatively expect the articles to for of factors early main number too B1 is the concept it in the Qualis, lat- to the the advanced Jour- in in (current) the and journal ranking CAPES within the est Qualis B3 although scheme as Ranking - qualified nal small initially still num- been is the has that articles show of results the ber The of content. focus publication, and level, of study grade year institutions, author’s by: journal issue, classified the were the of articles analyzed The website issues. We 15 the in published on (http://www.relea.ufscar.br), present. available analysis articles the be- an 59 to its Jour- present (2004) since American (RELEA) to ginning Latin Education Astronomy the is of by work nal published this articles of of goal The .S Bretones S. P. nvriaeFdrld B,CC,Bai (cbsalmeida Brazil CECS, ABC, do Federal Universidade OTIUIN N PERSPECTIVES AND CONTRIBUTIONS H AI MRCNJUNLOF JOURNAL AMERICAN LATIN THE SRNM DCTO (RELEA): EDUCATION ASTRONOMY 1 .C Jafelice C. L. , 2 n .E Horvath E. J. and , 211 3 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 3 2 C´ordoba, Argentina. 1 3 2 1 places. and levels various educa- at astronomy tion to for aiming contribution particular, academic in gen- greater America in Latin authors from of and participation eral the increase and meth- ods and submissions, contents of of dissemination diversification number greater the the encouraging increase for to need journal the the Finally, of out desirable. pointed be is analyses would it papers additional published sense, ed- the this at of aimed In journal research. articles a of ucation in writing publication the for of quality submitted minimum commu- a the for of nity training countries, American to: Latin variety regard of greater from with field. articles advance the articles, mo- more to in publishing the necessary works to is other up it in However, field citations the through to possible ment contribution is Asso- the it of note Concluding, nomination to Brazil. the from and Editors RELEA ciate the of Board 212 6 5 USA. CA, 4 Pasadena, Technology, of tute n sbigdvlpdi yhna ato Juan of part as python thesis. in PhD Cabral’s developed Bautista supernovae being of monitoring is the classifi- and and of detection/ galaxies phase eyeball of first the cation The involves objects. project system Monitor- this solar centre; some light galactic of of the ing of Classification galaxies Monitoring them; curves; candidate within of transients and Classification and Via Iden- the tification in includes: Variables that applications Vista with L´actea the Survey community- with for projects framework science web a developing are We ia a´lc eCie atao Chile. Santiago, Chile, Cat´olica de sidad .Cabral J. AE-OC-CNCT Argentina. CONICET, - OAC - IATE A OIE,Argentina. CONICET, Brazil. - Santana, OAC de F´ısica, Feira de Departamento UEFS, eatmnoAtoo´ayAto´sc,PnicaUnive Astrof´ısica, Pontificia Astronom´ıa y Departamento acaLambas Garcia nrrdPoesn n nlssCne,Clfri Insti California Center, Analysis and Processing Infrared A,USP. IAG, F´ısica, UFRN. de Depto. UFSCar. DME, nvria enloiaNcoa-autdRegional Nacional-Facultad Tecnol´ogica Universidad OMNT CEC IHTEVVV THE WITH SCIENCE COMMUNITY 1 .Gurovich S. , 2 .Amˆores E. , Minniti 2 .Good J. , 6 4 .Clari´a J. , 3 .Medel R. , 5 n D. and , 1 D. , ABSTRACTS r- - ae e oqesn 90 aPaa retn nttt de Instituto e Argentina Plata, La 1900, s/n, Bosque del Paseo 1 lognsoeuaiopoica n21,21 y 2012 2011, en provincial 2013. educativo organismo el propuesta. esta de multiplicador efecto el garantiza docentes los did´acticos por y alcanzados conocimientos disciplinares de grado el in- que y de formaci´on confiables fuentes b´usqueda de err´oneos, que la do- para previos adquiri´o los criterios de conceptos 95% revirti´o sus el 56% centes que el mostraron Luna curso sab´ıa. del Los la resultados los a no 4% referencia un err´oneos sab´ıa; con pose´ıa y conceptos los el err´oneos y no pose´ıa conceptos Tierra, 16% 54% la el de promedio, movimientos en los a Referente men- arriba cionadas. investigaciones las a similares resultados dise˜nos mostr´o los curriculares en presencia contenidos mayor los de sobre cursantes docentes los de previos vigentes. dise˜nos curriculares los tron´omicos as- estrategias de temas diversas los comprenden utilizando contenidos did´acticas. Plata Los La distrito docentes del los los did´acticos de actualizar acad´emicos y y contenidos fortalecer de a curso capacitaci´on destinado un ofrece Geof´ısicas, UNLP, tron´omicas y (Kriner escolares textos 2004). se los que algunos astron´omicos lo en err´onea de a temas o 2010); presentaci´on confusa al la et suma Gangui de cient´ıficas 2007, Navarro no Vega o 2004, fen´omenos (Kriner alternativas astron´omicoslos cotidianos alum- concepciones los a Gan- presentan nos 1999, frecuentemente y que 2010), 1995 for- gui (Camino escasa temas una estos poseen maci´on en profesorados y de primaria de estudiantes maestros se˜nalado que han que m´ınimo, tigaciones como o, ense˜nar. cient´ıficos docentes a temas los los dominen de ciencias alfabetizaci´on adecuada en conocimiento. una del de entonces multiplicadores requiere, agentes Se de por rol clave su papel un ense˜nanza niveles juegan de los originados obligatorios de conocimiento cambios docentes el misi´on los esta sus utilizando cient´ıfico. En humana y actividad la natural por mundo el decisiones tomen los sobre y todos comprendan que de re- para alfabetizaci´onciudadanos cientfica sus la de uno alcanzar como tos tiene siglo este educaci´on de La OETSD EDUCACI DE DOCENTES EDUCACI autdd inisAto´mcsyGeof´ısicas, UNLP, Astron´omicas y Ciencias de Facultad ALFABETIZACI sacpctc´nfeardtd o utj por puntaje con acreditada capacitaci´on fue Esta conocimientos los evaluaci´on diagn´ostica de La As- Ciencias de Facultad la 2011, Desde inves- Astronom´ıa, numerosas la de campo el En .S eBiasi De S. M. NSCNAI NL PLATA LA EN SECUNDARIA ON ´ NE ASTRONOM´ıA DE EN ON ´ 1 n .B Orellana B. R. and NPIAI DE Y PRIMARIA ON ´ 1 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes srfıiad aPaa(C aPaa-CNCT UNLP). CONICET, - Plata La (CCT Plata La Astrof´ısica de n ulcshos nweed n oiasis holidays and weekends On private schools. for scheduling public Thursdays and on lessons, by possible focused used being for schools is and Andr´e municipal Tuesdays laboratory Santo On astronomic Solar (Tellurium), the Stars. Moon Wednesdays and - Astronautic Earth - System, to Sun reference make System They the disposed dome. environments planetary the apprenticeship around four con- in PhD, Calil, sists Marcos Conheci- of authorship do project, Parque this of idealization Escola Andr´e, The S˜ao - Santo Paulo. in “Sabina mento” the lo- in Kepler”, the cated Johannes of started Digital laboratory Teatro astronomic schools, the “Planet´ario e of in 2012, reception August the on relates work This Brazil. Florian´opol ([email protected]). 2 88040-900, Brazil Catarina, 5153, Santa Postal, Apartado Trindade, 1 faiain samtvtradfclttro learn- of facilitator and ing. motivator Moon’s use a of as the animations evaluate phenomenon of students the and rotation learning synchronous in anima- helps that tion indicate re- students outcomes and 77 Learning pre-test with spondents. counting a assessment from learning drawn a issues sequence. of qual- and analysis animation quantitative itative from the has obtained of are user results progress the The the which a of on in control displayed screen is interactive animation Moon dynamic introductory The and an Earth discipline. of intervention physics Sun, learning The blended hypermedia in of of use results the analyzing about evaluation by rotation learning synchronous a Moon’s poster this in report We .L Fagundes L. A. PET nvriaeFdrld at aaia Campus Catarina, Santa de Federal Universidade PPGECT, F nvriaeFdrld i eJnio i eJaneiro, de Rio Janeiro, de Rio do Federal Universidade IF, NTTTOA EAOIA PROJECT PEDAGOGICAL INSTITUTIONAL YCRNU OAINMDAE BY MEDIATED ROTATION SYNCHRONOUS .Z Faria Z. R. Kanashiro ERIGEAUTO FMOON’S OF EVALUATION LEARNING “PLANET OANSKPE”ADITS AND KEPLER” JOHANNES OPTTOA RESOURCE COMPUTATIONAL 1 1 .C .Silva P. C. L. , 1 .R Calil R. M. , ROETAR DIGITAL TEATRO E ARIO .d Silva da T. , ´ 1 1 .R Perez R. E. , 1 n .F Barroso F. M. and , n .Calipo F. and , 1 M. , 1 ABSTRACTS is, 2 ftesuet ftect fSnoAndr´e. Santo of city quotidian the and of reality students the the of of and part Astronomy the make of Astronautic divulgation and for education collaborates an team is its Teatro by “Planet´ario places e Kepler” The Johannes non-formal Digital apprenticeship. of of use ally the an that evalua- thought the is on tion presented satisfaction planetary. the the of with team Meantime the unsatisfied by 0.1% promoted reception e satis- the satisfied were partially 97.8% 2.1% teachers, fied, the 189 the by From private done network. the evaluations public the to to 5% 3% network, be- and network municipal 92% the attended, to students longed 4932 2012 the From November private to schools. and public 2012 municipal, between August attended were From and place service. the visit about the the evaluation During an stu- fulfill the discussed. teachers with the subject done the is feedback about a dents lab- end session astronomic the planetary the At on oratory. a seen watch contents After the students supporting classroom. the in course developed group the curriculum age the the Astronomy considering and of always contents Astronautic, the explain and environ- to On the used of are students. ment resources the laboratory of survey astronomic knowledge a the do previous visit. monitors the better the a about course for the on starting Before passed the reception are the reception, rules During acquaintance ses- are: closure. activities dome which and laboratory, sion stages, astronomic the four trough in service. course schools done the is execute Astron- This to of Aeronautic contents on and trained omy to and inauguration guided monitor was the the team students, Since with activities of beginning visitors. the the for opened hi eut.Atr hycluaea vrg radius average an communicate calculate they and After, shadow results. Two sticks their homepage: theme a measure the the schools with in 2010 http://sites.google.com/site/projetoerato. Brasil” since Erat´ostenes project Brazil but “Projeto this America, in South co- in works Argentina project the Education. con- ordinates Astronomy autonomy” basic “docent to the train- cept according teaching is actions of ing application Project and Eratosthenes development Brazilian the of objective The 1 har iia n lntru oansKepler. Johannes Planetarium and Digital Theatre RZLA RTSHNSPROJECT ERATOSTHENES BRAZILIAN .Langhi R. 1,2 n .Vila¸ca J. and 3,4 213 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes T/R o oIu¸u rzl([email protected]). Igua¸cu, Brazil 4 do Foz PTI/BR, 3 ([email protected]). Igua¸cu, Brazil 2 do Foz PTI/BR, about 1 investigations to divulgation. scientific data and of formation source teaching rich a action be national can this learn that Furthermore, to students Astronomy. believe the We more motivate could this Education. with like Science compare actions we in when areas Brazil, in other rare extreme Education still Astronomy - in project researches This about discusses 2012). Editora, Escrituras forma¸c˜aoS˜ao Paulo: professores. a de repensando (Educa¸c˜aoAstronomia: Nardi & em Langhi according forma- model” “activist tive called is au- formation docent continued modifications con- during the responsible and to respect autonomy to realities This intents tonomy. their project of This teach- depends text. the what in work, modifications see ers we and change practice the could professional and useful Teaching interviews area are Formation. Education data use Teaching Science These will about col- researches teachers. we to the To research, with Skype our via experiments. for the data lect elaborate to itinerary some pre-ready show doesn’t site our au- because with tonomy, with the constructed were schools 2010, that Brazilian Since experiments different of verti- ground. hundreds in leveled received stay the project should in (gnomon) position stick cal The Earth. of 214 fa nta usinar;ii rprto fthe of preparation iii) application questionnaire; the initial by an and identified of astronomy technologies, about analysis IFNMG, digital preconceptions Janu´aria; ii) the students’ Campus at its of licenciates of the locus pedagogical research of the of (PPC) analysis i) projects taken: following be The to were steps Science. was Physics, Biological astronomy in and students Mathematics of Licenciate thirty-two concepts to offered basic learning about involved with activities course training astronomy. advanced of teaching An use the the in of materials interactive potentialities of the (IFNMG), investigate Gerais to aimed Minas and of and conducted North Science the survey Education, in of Technology a Institution of Federal the results at presents study This oetto:PTIC&T/FPTI-BR. Fomentation: PROEX-UNESP. and PTIC&T/FPTI-BR Fomentation: ooAtoˆmc aiioMneer ih,Funda¸c˜ao Filho, Montenegro Astronˆomico Casimiro Polo Funda¸c˜ao Filho, Montenegro Astronˆomico Casimiro Polo NEATV AEIL NTHE IN MATERIALS INTERACTIVE .A Macˆedo A. J. ECIGO ASTRONOMY OF TEACHING 1,2 n .R Voelzke R. M. and 2 ABSTRACTS ecesadme hi riigneeds. training future their of to meet options and contribute methodological teachers the may of in broadening which the technologies astronomy, of digital viability of of Teaching involving the and use of astronomy, learning resource to meaningful related of astronomy of evidence concepts to rates an relation the low; in was curriculum; knowledge the prior of students licenciate- results subjects the various diluted The content only in astronomy IFNMG includes physics the in analysis. course in content that a indicated methodology, conducted with quantitative was combined and test qualitative The the questionnaire. with final analysis the and of application v) tools; using interactive modality, various presence previous part-time proposal under education students’ developed the the of application account iv) knowledge; into taking course 1 un tet88 10-0,Sa al,S,Brazil. SP, Paulo, S˜ao 01506-000, 868, ([email protected]). Street Brazil. Bueno MG, Janu´aria, 39480-000, 2 6, ([email protected]). km Road, Janu´aria lntos fe h ciiis oedevelopment ex- some incomplete activities, had the After responses zenith. the by planations. general, daily in passes Sun And, How- the the time. first, that at measure misconception expressed, participants using to the of of objects 53.8% possibility ever, the the of shadows objects; in the the changes of relations and shadows of movements the existence apparent the day year; such the the between throughout during both as sky well po- the as the in Sun in variations the almost of of because sition existence the treated, recognized: themes all the had about already participants notions the after Initially, and activities. before participants the ques- the open to five applied to with was sundials used tions test of was A model types phenomena. concrete the Two A simulate tested. and objects. with built the relation were its apparent if and shadows the sky the the addressed in 2012, Sun module the in of The movement course, education described. continuing is last a the of of at conceptions developed module teachers, astronomical school the elementary 65 about research A rziod u nvriy apsLbrae Galv˜ao Liberdade, Campus University, Sul do Cruzeiro FM,Cmu auai.Sa ead am S/N Farm, Geraldo S˜ao Janu´aria. Campus IFNMG, OCPIN BU H APPARENT THE ABOUT CONCEPTIONS OEETO H U N THE AND SUN THE OF MOVEMENT LMNAYSHO TEACHERS’ SCHOOL ELEMENTARY HDW FTEOBJECTS THE OF SHADOWS .I Machado I. D. 1,2 o , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes sntdiyb eih(rm3.%t 95.4%). to 36.9% (from shadows sun zenith the the by that of daily opinion not the behavior with is the 29.3%); the to of of 3.1% basis reading (from considering the the on permits Sun; that hours the 29.2%), devices of to as position 6.1% sundials the (from on year to the the depending 18.4% during of (from and length day 41.6%) the the percent- throughout that varies the indicating shadows in responses: increase of an age was observed. there was phenomena example, the For of explanations the in (FPTI/BR). 2 ([email protected]). 1 uso bu o orlt srnm ihother with astronomy relate to how con- dis- to about the through is cussion transposition program didactic the the the to of in tribute use objective direct The for dif- classroom. designed different considering levels, motivate learning, learning and to ferent teaching focus of central processes the As- is where tronomy sequences didactic de- transdiciplinary ele- communities vulnerable velop and social high-school of of school undergrad- mentary teachers Adventurers professors, and called University students 2012 uates Universe. in ini- the program we of new activities, a these into tiated supplement methodologies To learned the the classroom. Teachers bring Galileo who and teachers workshops world- training a promoters the the create of Ambassadors to Galileo aims of IYA2009, network of program, wide legacy The a classes. is tools science that education their astronomy in of resources use teach-and effective train the to in ers developed program is international This the (GTTP). an Program project: we Training of extension Teacher funds, other committee Galileo federal with with efforts local 2014, uniting a are In by nearby city. and requesting organized Sul the are do Grande and Rio states of requested cities are different courses by training The multimedia. of audiovisuals, and re- observations, teachers telescopic attractive as to using such Astronomy sources levels, lecture middle to and fundamental aims It since Astronomy of 1999. Department perma- our a of program is nent (OEI) Observatory Educative Itinerant ISMNTN CEC NTESUHOF SOUTH THE IN SCIENCE DISSEMINATING .B Pavani B. D. etr aa´ tt nvriy o oIu¸u Brazil Igua¸cu, do Foz University, Paran´a State Western Support: E,GT N DETRR FTHE OF ADVENTURERS AND GTTP OEI, NVRE RIIGTAHR AND TEACHERS TRAINING UNIVERSE: aiioMneer ih srnm Center Astronomy Filho Montenegro Casimiro 1 .F .Saraiva O. F. M. , BRAZIL 1 n .Dottori H. and , ABSTRACTS 1 oicuetahr n tdnso te schools. other 3 of students 900 and and expanded teachers were school, include collaborations to one the 2013, of In col- teachers we students. 20 2012 with In laborated disciplines. non-science and science Dprmn fAtooy hsc nttt,URS Brazil UFRGS, Institute, Physics Astronomy, of 1Department 3 2 1 mrc eadn osuet u,tann n re- and Latin training in flux, search. astronomy students of to it development regarding what America the and years to next give the the can for emphasize has we RECA collabo- Finally, that that possible. vision people it that make the to and activities rated made and has Colom- achievements that, network the III After the all the today. review in until history we proposed the Congress was of Astronomy review it bian quick since a main RECA is 3 one in of divided first student is The work activities, parts. This outreach resources. as and that community links, such bigger a that benefits of individuals part gives compiles make and to It groups willing university are the astrophysics. their of and by most connected astronomy be for to love needed As- Colom- that by de students created bian Colombianos network national Estudiantes a tronom´ıa) de is (Red RECA eod.Temtoooycnit nteaayi of analysis the in consists As- methodology Ob- The Hazardous monitor- Earth Potentially teroids. Near the especially and in (NEOs), asteroids jects of enroll students discovery to college and is ing and objective re- school main and Its high observatories institutions. be- schools, search project educational universities, international tween Collaboration an is Search (IASC) Astronomical International .C eoiaGutierrez Remolina C. M. .A Rojas A. G. NENTOA SRNMCLSEARCH ASTRONOMICAL INTERNATIONAL nvria ainld Colombia. Colombia. de Caldas, Nacional de Universidad Jose Francisco Distrital Colombia. Universidad Andes, los de Universidad .Koh .F ao,A .Sla .G Silva G. G. Silva, L. A. Matos, F. M. Kroth, C. EA EWR YSUET,FOR STUDENTS, BY NETWORK A RECA: oo Restrepo Hoyos RZLA ATCPTOSI THE IN PARTICIPATIONS BRAZILIAN Ramos 1 .J al-ot,A .Klu,E. Kalmus, T. A. Dalla-Costa, J. L. , 3 COLLABORATION n .C utaoCasas Buitrago C. J. and , 1 STUDENTS .D iee Nieto Jimenez D. J. , 1 .VlsoMoreno Velasco S. , 2 .F. A. , 3 . 1 P. , 215 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes 1 choose to students careers. the the future helped their after has the and it how before and as campaigns, changed such astronomy events, im- in past the interest the discuss by latest will promoted the We as pact campaigns. a well 2013 present as from results, will news overall We the of Hawaii. PS1 summary Haleakala, the uses in which institution telescope the campaign, Brazilian Pan-STARRS a the milestone: of in important appearance participa- one straight Brazilian with third of IASC, year in fourth tions the marks 2012. September 2013 in conducted was Search which Asteroid Campaign, All-Brazil in event the was major measure- collaboration A this of asteroids. hundreds known and already for NEOs), ments asteroids them new of dozen have (3 a schools found over timeframe. in and resulting 72-hour IASC, universities a joined Brazilian in 2010 delivered the Since be and are must network images school The results the Hawaii. throughout and distributed America observato- North several in in ries obtained images astronomical 216 o ats .P .Crah,&R .d Moraes de V. R. & Carvalho, S. P. J. ORBIT Santos, CIRCULAR dos DISTURBING A IN A BODY AROUND CONSIDERING ORBITS GANYMEDE LOW-ALTITUDE Nesvorn´y D. STABLE & Gomes, S. PRODUCE R. TO TNOS MECHANISM HIGH-INCLINATIONS DYNAMICAL Michtchenko A. A T. & Aguero F. DYNAMICS PLANETARY N. OF STUDY THE IN SOFTWARE MATHEMATICA THE OF USE THE XHNEATVT HOG COSTLESS THROUGH ACTIVITY EXCHANGE RMWR FTEE NW PROJECT UNAWE EU THE OF FRAMEWORK .Zanazzi A. OT FIACLSIAY EFFECTIVE ITALY: CALLS AFRICA SOUTH nvriaeFdrld ˜oCro,Brazil. S˜ao Carlos, de Federal Universidade SYELK)CNETOSI THE IN CONNECTIONS LIKE) (SKYPE 1 .Albanese L. , 1 n rsiiNaidoo Troshini and , .I .Brasil, O. I. P. .Cardoso J. ITO ABSTRACTS OF LIST ABSTRACTS 130 129 129 2 aeTw,SuhAfrica. South Town, Cape iea nrosrsuc e ob ul exploited. fully be to yet resource enormous appears teachers an and like children communi- between simple model this coun- cation and World, between the are exchanges around all LARIM create tries as to such chances Interna- conferences perfect and Regional project or EU-UNAWE tional The lan- etc. astronomy, guages of uses whole interdisciplinary the year, during school story background a teachers with The working such as methodologies countries. didactic two curricula, the shadows on in confronted different time cast same gnomon the at equal an under- why to stand order in researches, their science shared actual prepared They learned curiosities. and experiences, shared with - methods, - participation have and children interest directly, huge talking seeing and of Zanemfundo chance other in this each to those Thanks and Town). the (Cape school chil- School of Italian the the between one of later in dren and Sicily participated sessions in training also teachers Italian the that and par- Italy) project teachers (South the town Skype to in Cape organized ticipating also the we but children, between experts the connections ex- and project’s the teachers the in the involve the only to at not event order change training In teachers’ Observatory. a activities SAAO also organizing and work- schools Town, school township at Cape the in with team ing African South the joined team with EU-UNAWE Italian the 2012 summer In ML SEODFAMNSI EARTH- IN ORBITS CROSSING FRAGMENTS ASTEROID Assafin SMALL M. J. & Vieira-Martins, Camargo, R. B. Braga-Ribas, I. F. IN Desmars, OCCULTATIONSJ. EPHEMERIS STELLAR OF CONTEXT TNO’S THE OF IMPROVEMENT Hoyos, Sucerquia J. M. Zuluaga, & J. Melita, STARS M. DWARF Cuartas-Restrepo, OF ZONE HABITABLE THE EVOLU- IN EXOPLANETS TERRESTRIAL MAGNETIC OF TION AND THERMAL TIDAL, 02 iez,Italy. Firenze, 2 50125 - 5 1 ot fia srnmclOsraoy bevtr 7935 Observatory Observatory, Astronomical African South NF-Osraoi srfiiod rer,LroE Fermi E. Largo Arcetri, di Astrofisico Osservatorio - INAF .Dh .B Afonso B. G. & Duha J. 130 130 P. , XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes UGOPO ATROTATORS FAST OF SUBGROUP PLANETS THE OF HABITABLE CHARACTERIZATION ATMOSPHERIC COMMON MOST THE Brasser R. PLANETARY & Gomes, MODEL’S ENCOUNTERS NICE CLOSE SATELLITES THE REGULAR DURING OF BEHAVIOR THE Sfair RADIATION RESONANCE R. SOLAR THE THE FORCE AND OF UN- MIMAS ARC EFFECTS WITH RING THE G THE DER Roig OF F. EVOLUTION & THE Mothe-Diniz, T. Carvano, J. Filho, DIFFERENTI- FAMILIES ASTEROID OF ATED EVOLUTION DYNAMICAL NTESLRSYSTEM RESONANCES SOLAR BODY THE THREE IN THE OF ATLAS H N METEORITES SNC THE COM- Jr. MEAN-MOTION TO MENSURABILITIES CLOSE SUPER-EARTH SYSTEMS IN RESONANCES SPIN-ORBIT DMDLN FTEBPLRNEBULA BIPOLAR THE 2346 OF NGC MODELING 3D THE Izaguirre ON EFFECTS S. STRATIFICATION DENSITY L. & Voelzke R. II M. TAIL 1910 1P/HALLEY THE COMET OF STRUCTURES OF ANALYSIS MORPHOLOGICAL MB H EIA ILO MODELS MILLION MEXICAN DATABASE Costa THE D. D. 3MDB: R. & Lago A. SPECTRA J. DISPERSION HIGH FORM NGC 6302 AND 3918 NGC OF PROFILES KINEMATIC Yuan J. & N10 Suad BUBBLE A. L. THE & Arnal M. E. RE- Ortega, E. M. SHELL Gamen, R. MOLECULAR SH2-187 A TO LATED 126.1–0.8–14: G OARMAT NTELREMAGEL- LARGE THE CLOUD LANIC IN SUPER- REMNANTS TWO NOVA OF STUDIES SPECTROSCOPIC Goldes V. G. & LeCoarer, SOUTH- MAGELLANIC LARGE CLOUD THE THE OF IN REGION EAST BUBBLES OF STRUCTURE .C ora,S .GuitiWne,& Winter, Giuliatti M. Mour˜ao, S. C. D. .A doe .Aboi-rz E. Ambrocio-Cruz, P. Oddone, A. M. .Mrse .Delgado-Inglada G. & Morisset C. .M anio&D .Gon¸calves R. D. & Carneiro M. C. .Puet .V .Copetti F. V. M. & Pauletti D. .Gm,J eie .Wu, Y. Lepine, J. Gama, D. .B ier .Callegari N. & Ribeiro B. F. .Ccoosi .Pineault, S. Cichowolski, S. .E Varela E. M. .Gallardo T. .C ouia R.S. Nogueira, C. E. .S Martins- S. W. .Pinotti R. ABSTRACTS 131 132 132 131 131 133 133 134 134 135 135 135 134 136 136 136 P. .H eqer,&M .Vasconcelos J. M. & Cerqueira, H. A. TAYSAEACEINDS MODELS VARIABLE WITH DISK M. & ACCRETION Dougados, STEADY-STATE C. Perraut, K. Lima, H Benisty A. THE R. USING H. AUR G. AB OF MENT ENVIRON- CIRCUMSTELLAR THE Lazarian MODELING A. & Santos-Lima, R. Pino, Dal Gouveia CORES CLOUD LENT TURBU- OF COLLAPSE GRAVITATIONAL THE IN DIFFUSION RECONNECTION OF ROLE THE Pereira YDMIGO ALFV OF OF DAMPING BY DISKS FRACTION ACCRETION PROTO-STELLAR IONIZATION DUSTY OF T. INCREASE & Fernandes, B. Gregorio-Hetem, Santos-Silva J. Hetem, STAR ANALYSIS A. FRACTAL YOUNG STATISTICAL CLOUDS: PARENTAL A OF THEIR AND ASSOCIATION CLUSTERS THE ON SH2- Montmerle AROUND CLUSTERS ASSOCI- 296 YOUNG SOURCES TO X-RAY ATED OF NATURE THE Cerqueira H. A. & Vasconcelos, J. M. Feitosa, A. PROPLYDJ. BEEHIVE THE Arrieta OF SIMULATIONS A. 3D & Georgiev, ION- L. OF Richer, R. FUNCTION A AS STRUCTURE IZATION 7009 EXCITED NGC IN COLLISIONALLY LINES AND RECOM- BINATION OF KINEMATICS DISCREPANT THE Lopes SOUTHERN VVV EXTINCTION THE RAYLEIGH-JEANS MAP FROM THE A SEEN SURVEY: AS ON DISK GALACTIC EXTINCTION OF THE Cambresy L. STRUCTURE & Pereyra, Magalh˜aes, A. CLOUD FIELD DARK MUSCA Krabbe MAGNETIC C. A. THE & Copetti, F. V. M. Rauber, PLANE- 2440 NGC B. AND A. THE 6302 NGC AND OF NEBULAE TARY PHYSICAL PROPERTIES OF CHEMICAL VARIATIONS SPATIAL AND imbert REGIONS II IMPLICATIONS H THEIR RE- IN II LINES O COMBINATION FROM DERIVED PRESSURES, ABUNDANCES AND TEMPERATURES, DENSITIES, .St,R aba .Fro .Roman- A. & Firpo, Barb´a, V. R. Soto, M. .Geoi-ee,B enne,&T. & Fernandes, B. Gregorio-Hetem, J. α NWAVES EN .R .L˜o .M de M. Le˜ao, E. M. R. M. ´ .R .O Magalh˜aes, O. S. R. E. .Tre-emet M. Torres-Peimbert, S. .Pibr .Pe- A. & Peimbert M. .L ier,A M. A. Ribeiro, L. N. α .Jatenco- V. LINE 217 137 141 141 140 140 140 139 139 138 138 137 137 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes UT-PC NRRDSPECTROSCOPY D. OF Ribas, INFRARED Mello I. de MULTI-EPOCH Porto Horvath, F. E. G. J. & Galante, Odert, P. Leitzinger, OF ORIGIN THE LIFE STUDY TO ASTROBIOLOGI- APPROACH AN CAL PROJECT: BIOSUN THE CRTO ICMP FV01OPH INSTA- MASS-TRANSFER MODEL V2051 THE BILITY OF FAVOR OF IN EVIDENCE MAPS ADDITIONAL OUTBURST: ALONG DISC ACCRETION Luz la de V. OA YESASO INTERMEDIATE OF Hernandez- IN STARS ABUNDANCE BRIGHTNESS TYPE LI SOLAR OF DETERMINATION Granada A. & Otero, S. Mennickent, E. R. Aguayo, FTESBILMTROBSERVATORIES SUBMILLIMETER SMA/ALMA THE ERA THE OF IN FORMATION PLANET AND Gameiro STAR F. J. & Sterzik, M. Figueira, P. Santos, UCHUS OIISO RTSASIN PROTOSTARS 7 VE- OF RADIAL BINA- MULTI-EPOCH LOCITIES PRECISE PROTO-SPECTROSCOPIC RIES: FINDING Rubio M. & Romero, G. G341.24-0.27 IRDC THE J. OBSERVATIONS OF FAR-IR & AND Teixeira, MILLIMETER P. Bouvier, J. Alencar, Stauffer P. TAURI H. S. T nis, CLASSICAL 2264 NGC OF IN STARS DISKS Min- D. INNER & THE Soto, M. Nilo, L. J. niti Firpo, V. Jaque, M. ULES CLUSTER GLOB- STAR DUSTY TO NEW ASSOCIATED CANDIDATES OF STUDY Petriella INFRARED A. & Giacani, E. Paron, CLOUD BRIGHT-RIMMED A IN FORMATION D. STAR TRIGGERED R. OF & STUDY Barbosa, L. C. Blum Damineli, YSOS A. MASSIVE Navarete, OF F. SAMPLE A WARDS UVYO XEDDH EXTENDED OF SURVEY A Ray, P. Tamura T. M. Dawson, P. & Geers, C. V. COM- Jayawardhana, A STAR REGIONS IN FORMING DWARFS TOWARDS BROWN OF SURVEY: CENSUS PLETE SONYC THE 218 ETUIPIRT OUTBURST TO PRIOR CENTAURI .St ig .Br´,A Roman-Lopes, Barb´a, A. R. King, Soto P. gia .C aotn,E etn,& Bertone, E. Dagostino, C. M. Aguila, ´ .C beaa .Hnlee,M. Hanslmeier, A. Abrevaya, C. X. .VaaAmia .Ml,N C. N. Melo, C. Almeida, Viana P. .Zapata L. .L nrd .Baptista R. & Andrade L. E. .P os,P .McGin- T. P. Sousa, P. A. .M mz-´mz B. Amazo-G´omez, M. E. .Mzc .Shl,R. Scholz, A. Muzic, K. .Vsuz .Cappa, C. Vasquez, J. 2 .E rea S. Ortega, E. M. MSINTO- EMISSION ρ OPHI- ABSTRACTS 144 144 145 145 144 143 143 143 142 142 141 G. OLSOSBTENGOUA CLUS- GLOBULAR TERS BETWEEN COLLISIONS Alfaro E. Ma´ız Sota, Apell´aniz, J. & A. Walborn, R. N. Morrell, AND SPECTRO- SEVEN STARS O WN SOUTHERN HIGH-RESOLUTION OF AFTER MONITORING SCOPIC OF RESULTS YEARS SURVEY: OWN BAROTROPIC Marchant IN P. & FIELDS STARS MAGNETIC Haucke M. & ON Cidale, S. STARS L. SGS Kanaan, Cur´e, B S. OF STUDY WIND Zuber LOW- K. & OF Jack, D. EVOLUTION STARS THE NEUTRINO MASS ON NON-STANDARD EMISSION OF EFFECTS Santill´an A. & ud-Doula, Cur´e, A. ZEUS-3D USING WIND SOLUTIONS RADIATION-DRIVEN & SLOW Jr., AND Santos FAST C. F. Maia J. S. Corradi, F. B. F. J. CLUSTER W. Angelo, S. OPEN ESO429-SC02 CANDIDATE THE REMNANT OF SPECTROSCOPY A PCR O TLA POPULATION STEL- STELLAR APPLICATIONS THEORETICAL FOR OF SPECTRA LIBRARY LAR NEW A Pereira S. E. & OCCUR- CME SERIES THE RENCE OF Mel´endez ANALYSIS J. SPECTRAL & Milone, A.C. EVI- Carlos, C. NEW C. STAR: G. FORMATION M. POOR PLANET METAL ABOUT DENCES A OF YSIS ANAL- CHEMICAL Gib- DIFFERENTIAL Assmann DETAILED K. P. B. & Fellhauer, Kroupa, M. P. Smith, son, R. Candlish, CLUSTERS N. STAR G. POPPED OF MIXING PHASE STAR Bufano SUPERGIANT F. A FROM 2011HS SN TORS: PROGENI- SUPERNOVA IIB TYPE UNVEILING Kurtev R. Chen´e, & N. Alegr´ıa, SURVEY A. VVV CLUSTERS THE OPEN IN Oliveira OLD S. DISCOVERED A. NEWLY & Baptista R. Borges, B. STARS VARIABLE CATACLYSMIC VARIA- IN TIONS PERIOD CYCLICAL FOR SEARCHING .Amz,A esnge,J .Valdivia, A. J. Reisenegger, A. Armaza, C. .T eln .J Rocha-Pinto J. H. & Belloni T. D. .Br´,R ae,J .Ais N. Arias, I. J. Gamen, Barb´a, R. R. .R eat,M .G Guedes, G. R. M. Cecatto, R. J. .Coelho P. .AcoDız -.Schr¨oder, Arceo-D´ıaz, K-P. S. .Brsoa .Ram´ırez S. Borissova, J. .Aaa M. Araya, I. .Acs M. Arcos, C. 146 146 150 148 147 147 147 145 151 150 149 149 148 148 151 M. XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes ra,R ae,&E endzLajus Fernadez J. E. Ferrero, & G. Tor- Gamen, Soto, S. R. Lopes, M. Arias, Roman Gunthardt, A. G. Robledo, Morrell, res N. Barba, NEW H. AND R. RESULTS BINARIES EARLY ECLIPSING STARS: & OF Nickeler, NIP H. D. Cidale, Cur´e S. M. L. Tomic, S. Venero, CYG VARIABILITY WIND 55 THE OF OF ORIGIN THE ON Calder´on Espinoza D. & D´ek´any, Catelan, I. M. STRIP INSTABILITY IN CEPHEID VARIABLES THE PULSATING LIGHT-CURVE OF PROPERTIES Gomes R. A. & OPTICAL/NEAR-INFRARED Jr, Ferreira M. M. Casana, COHERENCE AND AM- PLITUDE THEIR FROM CLUES BINARIES: X-RAY IN OSCILLATIONS QUASI-PERIODIC TWIN-PEAK LONG- Breitfelder J. M´erand, & BINARITY ENVELOPES FROM AND CIRCUMSTELLAR DISTANCES, DIAMETERS, CEPHEIDS INTERFEROMETRY: & BASELINE Campion, Le F. CLASSICAL J. Galli, Fidˆencio B. M. A. P. Ducourant, SEQUENCE STARS PRE-MAIN OF MOTIONS PROPER Bonatto 24 PISMIS CLUSTER THE STAR VVV-ESO: FOR PIPELINE PSF-FITTING A FROM CLUSTERS MODELING SMC CMD FOR Catelan PARAMETERS M. & Minniti, VARI- LACTEA D. VIA VISTA Pullen, THE OF IN CATALOG ABLES GENERAL Christen A. THE & Cassetti, J. Rial, F. Cur´e, STARS D. M. FIELD MAIN–SEQUENCE TO TION APPLICA- STARS: RO- OF THE DISENTANGLE VELOCITIES TATIONAL TO METHOD Marchiano NEW E. A P. & Rocco, Di H. O. Cruzado, A. APPLICATIONS ASTROPHYSICS FOR USE- FUL STRENGTHS OSCILLATOR OF LATIONS Templates CALCU- MULTICONFIGURATION VVV EXTENSIVE The & Borissova, J. Team Saito, K. D´ek´any, Jord´an, Alonso-Garc´ıa,R. A. I. J. Gran, Angeloni, F. Navarrete, R. C. Catelan, M. Ramos, PROJECT treras TEMPLATES VVV THE .C .Frer,R exia C. Teixeira, R. Ferreira, S. C. A. .Huk,M ru,R .J. O. R. Kraus, M. Haucke, M. .Da tal. et Dias B. .Glen,P evla A. Kervella, P. Gallenne, A. .JqeArancibia, Jaque M. .A .Da C. & Dias G. A. R. .German`a, R. C. .Dkn,J. Dekany, I. .Hajdu, G. .Con- R. ABSTRACTS 155 155 155 154 153 153 153 152 152 151 151 154 O AIBESASIN STARS VARIABLE RELATIONS FOR PERIOD-LUMINOSITY NEAR-IR NCMATBNR ADDTSFROM OBSERVATIONS CANDIDATES TELESCOPE BINARY SOAR COMPACT IN SIGNATURES ACCRETION HIGH-IONIZATION F. D´ek´any Ramos, I. Contreras Alonso-Garc´ıa, & R. J. Gran, Catelan, M. Navarrete, C. NRYINTERACTIONS LOW- ENERGY TO HIGH- WITH FROM CLOUDS: MOLECULAR COLLIDING M´endez, REMNANTS A. SUPERNOVA R. Carraro, Moyano G. M. Smith, & R. Bidin, DENSITY MATTER Moni DARK Silva LOCAL da THE Pereira ON R. J. & Soares, B. B. PLEIADES Miranda, OF THE D. OF INCLINATION AXES MEAN ROTATIONAL Vaz THE R. ESTIMATING P. L. & Landin, R. FIELDS MAGNETIC WITH STARS PMS ROTATING, OF MODELS STELLAR Levato H. CEN A TOPEI TAIIAINSGSIN OF SIGNS NON-LTE STRATIFICATION S. Geisler, ATMOSPHERIC Chen´e D. N. Cohen, A. E. & R. Villanova, Bidin, Moni SURVEY GALACTIC C. VVV Mauro, IN OF CLUSTERS STELLAR & ANALYSIS Nelson, T. PHOTOMETRIC Mukai, K. Nu˜nez Sokoloski, E. L. N. J. Luna, UV M. AND X-RAYS Mello IN de STARS Porto SYMBIOTIC F. G. & Lorenzo-Oliveira D. APPROACH BAYESIAN AND AGES: CARLO ISOCHRONAL MONTE PRECISE OF SEARCH BINARY IN Placco X-RAY M. MASS V. & HIGH THE J054134.7-682550 XMMU PROPER- OF X-RAY TIES AND Vaz R. OPTICAL COLOR- P. UNVEILING L. & IN Mendes, S. T. EVOLUTIONARY ISOCHRONES DIAGRAMS MAGNITUDE AND SEQUENCE TRACKS PRE-MAIN IEIETFCTO NTESNSSPEC- SUN’S THE TRUM IN IDENTIFICATION LINE HT WR STARS DWARF WHITE al. DETERMINATION TEM- PERATURE - DETERMINATION SURVEY MASS JPAS - THE DETECTION IN STARS DWARF WHITE .L aa .F iv,N ryil,& Przybilla, N. Nieva, F. M. Maza, L. N. .R Kitamura R. J. 3 HE AND 4 1 .O Kepler O. S. HE n .P Martins P. L. and .Lpsd Oliveira de Lopes R. .Montmerle T. ω .T .Mne,N. Mendes, S. T. L. NTEB STAR BP THE IN CENTAURI .R adn L. Landin, R. N. .Kna et Kanaan A. .J. G. 159 159 160 160 160 159 158 158 158 157 157 156 156 161 219 1 A. C. F. XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes AATCDNMC:OII,HISTORY, PROSPECT AND ORIGIN, PRESENT DYNAMICS: Bonatto C. GALACTIC & Bica, E. Araujo, De P. WITH P. Pavani, PHOTOMETRY CLUSTERS INFRARED Pintado 2MASS I. EMBEDDED O. & GALACTIC Illiev, K. 7099 I. NGC Paunzen, AND E. 6205, NGC 104, NGC CLUSTERS: ∆ Orellana ETERS PARAM- ASTROMETRIC EXTENSIVE USING REGIONS Almeida IN J. SKY A. DETECTION F. L. CLUSTER & Cieslinski, OPEN Silva, D. G. Rodrigues, M. K. V. Jablonski, C. Oliveira, S. 220 OEIGBU OIOTLBRANCH HORIZONTAL STARS BLUE MODELING 1 MEN- ZEL NEBULA PLANETARY THE OF CON- DITIONS PHYSICOCHEMICAL THE Grosbøl OF P. MAPPING & Dottori, H. Jr., Santos INDEXES USING PHOTOMETRIC ONES NEAR-IR OLDER FROM CLUSTERS STAR EMBEDDED GROUP LOCAL DISCRIMINATING Pereira B. C. 2360 & NGC IN STARS GIANTS HIGH- RED OF SPECTROSCOPIC HIGH-RESOLUTION THE al. et Rodrigues J1007.5-2017 V. ON C. RX POLAR ACCRETION MAGNETIZED LIGHT PROBING OF Rivinius ANALYSIS T. & THE BY OF CURVES STARS DISKS OF BE PARAMETER VISCOSITY THE INVESTIGATING SEMI- FOR A PIPELINE OF AUTOMATIC DEVELOPMENT THE TOWARDS Beers C. T. & LYRAE STARS RR CEMP K. FOR SEARCH R. CONTINUED A & Lorenzo-Oliveira, D. L´epine, Siqueira J. Dias, S. SUN: CONNECTION? THE A AND IN NEIGHBORHOOD ORBITS SOLAR THE GALACTIC EXTINCTIONS, Minniti, MASS D. Larsen, S. Lucas Kurtev, S. P. R. Catelan, & Borissova, M. Ivanov, J. D. Hanson, V. M. SURVEY M. (VVV) Popescu, LACTEA VIA THE VARIABLES VISTA IN THE IN STELLAR FOUND DESCRIBE CLUSTERS TO MASSCLEAN USING A BEVTOSO HE GLOBULAR THREE OF OBSERVATIONS .Sno .Monteiro H. & Santos P. .G ats&L .Martins P. L. & Santos G. R. .M egai .R end,S Rossi, S. Kennedy, R. C. Reggiani, M. H. .R ´ml,A .Crifi .Haubois, X. Carciofi, C. R´ımulo, A. R. L. .G aı,M .D is,&R B. R. & Biasi, De S. Pa´ız, M. G. L. .F ot eMlo W. Mello, de Porto F. G. .V ae Silva Sales V. J. .Pichardo B. .F C. F. J. Bogdan .B. D. ABSTRACTS 162 162 161 161 166 165 165 164 164 164 163 163 162 166 H OMLADSBUIOSTP II-P TYPE SNE SUBLUMINOUS AND NORMAL BETWEEN SUPERNOVA THE Fran¸ca ANOTHER A. 2009N: V. & SN Silva, P. M. Silva, STARS FIELD EVOLVED .d ot,&M .G Maia REDSHIFT G. HIGH A. AT M. GALAXIES & Costa, da ENERGY N. DARK THE POPULA- OF SURVEY LIGHT STELLAR THE DISK IN TION OUTER LMC THE Pellizza J. GALAXY L. & Tissera, IN BINARIES MODELS BLACK-HOLE FORMATION X-RAY FROM HIGH-MASS FEEDBACK STELLAR OEFITTING MORE Emilio M. & DIS- Pacheco, STARS VELOCITY BE ROTATIONAL OF TRIBUTION OF STUDY A ASSGEAINO ON TRCLUS- TERS STAR YOUNG OF SEGREGATION MASS Baptista R. & QUIESCENCE OUT- IN IN AND OPHIUCHI BURST OF V2051 NOVA MAPPING DWARF THE DISC ACCRETION & INFRARED Raga, Vel´azquez, A. P. Esquivel Costa, A A. A. 209458B Schneiter, EXTRASOLAR M. HD OF STUDY RANGES: CASE SENSITIVITY RATE MASS-LOSS THE ON Melendez J. & Maia TWINS SOLAR IN ELEMENTS HEAVY OF ABUNDANCES A. CHEMICAL DIFFERENTIAL Chauvin, Campion, G. Le Song Zuckerman, F. I. B. & J. Krone-Martins, Galli, O. B. G. A. P. Ducourant, NEW OF DATA LIGHT ASTROMETRIC IN HYDRAE TW REVISITING CRTO ICMPIGO THE BINARY OF ECLIPSING MAPPING J0926+36 SDSS PERIOD DISC SHORTEST ACCRETION ICAUDNE NGLCI BULGE GALACTIC IN STARS ABUNDANCES & Soares, ZINC B. Freitas B. Nepomuceno, de F. B. M. D. M. ROTATION Silva, P. STELLAR R. THE FROM ING ARIS- NONEXTENSIVITY TIME-DEPENDENT Leister SPECTROSCOPIC V. N. OF K¨unzel, & ANALYSIS FEATURES 2883: ALS .Tak´atsK. .Yu J. .R ivia&B Barbuy B. & Silveira R. C. .Blio,B atao .Grri L. Girardi, L. Santiago, B. Balbinot, E. .R iv,R .Lvnae,R. Levenhagen, S. R. Silva, R. A. .Shiden&R Baptista R. & Schlindwein W. V .S ilrelDAgl,E. D’Angelo, Villarreal S. C. SIN I ITIUINFOR DISTRIBUTION .B ors .R P. R. J. Soares, B. B. .C rae .B. P. Artale, C. M. .Sto .Janot- E. Sitko, C. .Tier,C. Teixeira, R. .Wojcikiewicz E. .E Bauer E. F. .Tucci M. 168 169 167 172 171 171 168 170 170 170 169 167 166 171 168 J. XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes VAT OBSER- AT OBSERVATIONS DETER- FROM VELOCITY MINATION RADIAL CLUSTER OPEN Mast D. & Walcher, P. Falc´on Barroso, J. S´anchez J. Bl´azquez, C. Husemann, S´anchez, B. F. Gonz´alez Delgado, S. M. DATA R. Garc´ıa Benito, CALIFA P´erez, R. TO CUBES STARLIGHT SPACE: AND APPLYING TIME IN GALAXIES RESOLVING Sodr´e Jr. L. VISIBLE EMISSION & UV THE Dantas THEIR IN AND GALAXIES REGION SPECTRAL OF THE SYNTHESIS BETWEEN Alonso RELATION V. M. THE Castell´on, & Nilo L. J. Cuevas, CLUSTERS GALAXY LUMINOSITY RAY X- LOW IN INDEX CONCENTRATION L. GALAXY & Fernandes, Cid R. AS Sodr´e Jr. Asari, 0.5 V. Stasi´nska, N. = DATAG. SDSS Z BY SINCE TOLD EVOLUTION PHASES GALAXY PASSIVE OF AND AGN Foster FORMING, Brodie, C. J. STAR J. & Coccato, Romanowsky, Strader, L. J. A. Forbes, Usher, D. C. Merrifield, Pota, M. V. Arnold, , Chies-Santos, A. Bamford Oliveira, de S. Mendes GALAXY C. THE Cortesi, HOST A. AND THEIR (GCS) OF EVOLUTION CLUSTERS ORIGINS GLOBULAR THE OF BETWEEN CONNECTION Makler THE M. & Caminha, G. Cypriano, SURVEY GRAV- ARCS SOAR ITATIONAL THE FROM CLUSTERS GALAXY .Garc´ıa-RojasJ. 6822 NGC Hern´andez-Mart´ınez, Pe˜na, GALAXY L. Flores-Dur´an, & M. THE POPU- IN DIFFERENT LATIONS OF Wilkinson STUDY I. KINEMATIC M. A & Assmann, P. GALAXIES Fellhauer, DSPH L´epineM. D. OF R. FORMATION J. THE & Dias, S. W. Monteiro, YAIA NLSSO =0 Z= OF ANALYSES Arag´on- Gray DYNAMICAL A. M. & Pino, Bamford, del S. Salamanca, Rodriguez B. THE SUPERCLUSTER Chies-Santos, OF 901/902 SURVEY ABELL IMAGING LINE Plana EMISSION H. & Carvalho S. M. H OF KINEMATICS INTERNAL E A562 CLUS- TER OF DATA VELOCITY THE Telles OF ANALYSIS E. & Bicalho C. I. NUCLEI GALACTIC ACTIVE METAL-POOR ROPC O DIAS DOS PICO ORIO ´ .L eAoi,R i enne,E. Fernandes, Cid R. Amorim, de L. A. .Cle´nEpnz .G´omez P. & Calder´on Espinoza D. .V Costa-Duarte, V. M. .A .Fra H. Faria, F. A. M. II .Cbra E. Cibirka, N. GALAXIES .L. M. . 3 ABSTRACTS , 175 175 174 174 174 173 176 176 175 172 173 173 172 0 H. A. S. . 5 H MATO A UKRTTO ON ROTATION BULK LYMAN- GAS THE OF IMPACT THE Fa´undez-Abans THE 2229- AM ON 735 OF INTERACTION ABUNDANCE AND OF KINEMATICS EFFECTS THE Dors O. Fa´undez-Abans, & M. UNDER GALAXY RING CONSTRUCTION POLAR A 2217-490: AM .Mateus STATISTICS A. MARKED BY PROBED GA- LAXIES OF PROPERTIES ENVIRONMENTAL THE al. et Makler M. SURVEY ARC GRAVITATIONAL SOAR THE Garc´ıa Benito R. P´erez, & E. des, Fernan- Cid UV R. Gonz´alez AND Delgado, Fern´andez, M. OPTICAL R. THE GA- IN CALIFA LAXIES OF HISTORY Junqueira, Andrievsky FORMATION C. STAR S. T. & Barros, Dias, A. S. D. W. Jr., OF Scarano S. RESO- EVOLUTION GALAXIES ine, COROTATION SPIRAL SECULAR OF THE THE DISKS IN OF NANCE ROLE THE Galaz POP- MORPHOLOGY STELLAR AND SDSS. ULATION THE IN GALAXIES E+A Z-SSFR team THE GAMA GALAXIES: IN GAS RELATION I H AND SFR SPECIFIC METALS, BETWEEN THE CONNECTION (GAMA): ASSEMBLY MASS AND Caproni GALAXY A. & Falceta-Goncalves, D. GA- Ruiz, DWARF HYDRODYNAM- SIMULATIONS IN 3D ICAL FROM PROCESS RESULTS LOSS ON LAXIES: HALO MASS MATTER DARK THE OF EFFECTS A. THE M. & Vega-Acevedo, Maga˜na-Serrano I. Hidalgo-G´amez, M. A. GALAXIES B. Braz DS V. J. OF Cendron, RATES F. FORMATION M. A. STAR & M. Lacerda, Parize, Rossi, M. D. M. L. A. Klein, L. DE- E. Amorim, de Fernandes, SURVEY L. Cid R. SKY Mateus, INFRARED DIGITAL IN IN TECTED GALAXIES SLOAN OF THE PROPERTIES PHYSICAL & Cl´audia Winge, Krabbe, C. Bonatto GEMINI C. A. Rodrigues, I. WITH iza, 1219-430 AM GMOS-S MI- MERGER THE OF NOR DYNAMICS AND PHOTOMETRY Dijkstra M. & Forero-Romero, J.E. .FetsLms .Rdius .Dr,&M. & Dors, O. Rodrigues, I. Freitas-Lemes, P. .A enne-iee,M .Pastor- G. M. Hernandez-Jimenez, A. J. .A aaLpz .M okn,& Hopkins, M. A. Lara-Lopez, A. M. α LINE .FetsLms .Rodrigues, I. Freitas-Lemes, P. .A afaci .O. L. Lanfranchi, A. G. ..Garavito-Camargo, J.N. .R epc,A. Herpich, R. F. .Lia&G. & Leiva R. .R .Lep- D. R. J. .L´opez-R. 176 177 181 180 180 180 179 179 179 178 178 178 177 221 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes RPRISO AAISADGOP AT Cora, Z GROUPS Ruiz AND A. N. GALAXIES S. A. OF PROPERTIES Padilla, & Kurczynski, D. P. N. Gawiser, Navarrete, E. P. F. cibia, “COUNT THE APPROACH MODEL: MATCHING” SEMI-ANALYTIC A ULTRA- IN COUNTS NUMBER (?): GALAXY SUBMILLIMETER GALAXIES OF DWARFS CLASS COMPACT NEW A 222 i enne,&G Stasi´nska G. & Fernandes, Cid CROSCOPE MI- STARLIGHT THE UNDER RELATION RATE FORMATION MASS–METALLICITY–STAR THE Fria¸ca GALAXY S. AS REDSHIFT MARKER EVOLUTION HIGH AT LINES Herrera-Camus PAH R. & Bolatto, A. M82 Salter, IN GAS DENSE THE Merch´an OCCUPATIONM. HALO DISTRIBUTION OF DETERMINATION Gabbasov F. Mart´ınez-Garc´ıa, R. 5278 Eric & THROUGH DARK NGC Rosado, M. OF CONTENT SYNTHESIS: MATTER RATIO POPULATION STELLAR MASS-TO-LIGHT S. & DISK Higuera-G. A. M. Quintero Mart´ınez-Galarza, R. MID- GALAXIES J. THROUGH MODELS SED FORMATION INFRARED OF STAR PARAMETERS WITH PHYSICAL NU- IN drigues DYNAMICS SIMULATIONS ARMS MERICAL SPIRAL AND BAR Jablonski F. INFRARED IN MODEL GALAXY Andernach H. & Torres-Papaqui, OTHER WITH MEASUREMENTS COMPARISONS GALAXIES: DEN- AND OF RESULTS ENVIRONMENT THE THE MEASURING OF SITY TO S. APPROACH T. AN & Men´endez-Delmestre, K. Gon¸calves Oliveira, UNDERSTAND S. C. TO GALAXIES DOOR LYMAN-BREAK LUMINOUS HIGH-REDSHIFT A UV STARBURSTS: COMPACT LOW-REDSHIFT Sodr´e Jr. L. POPULA- GALAXIES STELLAR WITHIN TIONS OF DISTRIBUTION THE Ribeiro B. L. < 1.4 .S acmno .A .Lps A. & Lopes, A. A. P. Nascimento, S. R. .Shikan .Vl sr,R. Asari, Vale N. Schlickmann, M. .Rdiuz .A Sgr´o, & A. M. Rodriguez, F. .A reaMnkt,J P. J. Ortega-Minakata, A. R. .Mieske S. .H .Sno .C. A. & Santos B. H. J. .Sls .Glz D. Galaz, G. Salas, P. .M Mu˜noz Aran- M. A. .Peai&I Ro- I. & Puerari I. .F ao P., Ramos F. A. .M oas& Novais M. P. .Pld & Polido P. .Repetto, P. ABSTRACTS 182 181 186 185 185 185 184 184 184 183 183 182 182 186 INLN RPRISO STAR-FORMING OF GALAXIES EMIS- PROPERTIES THE LINE TO SION APPROACH DATA-DRIVEN GA- A Fernandes ANALYSE Cid R. TO Ben´ıtez, & N. TOOL DATA PHOTOMETRIC NEW LAXIES A MAGAL: H NRMD AAYM1I H ERA COSMOLOGY THE PRECISION IN OF M31 GALAXY ANDROMEDA THE de Amram, P. Mendes Carrasco, Plana R. C. H. E. Alfaro, & Mello, M. de F. Olave, D. Oliveira, D. Jr, Scarano S. TAILS SYSTEMS MERGING TIDAL AND IN GRADIENTS METALLICITY Scannapieco SCE- C. HIERARCHICAL IN OF NARIO HALOES SPIRALS STELLAR MASSIVE OF FORMATION THE Carrasco R. E. GALAXY MRK996 HII NUCLEUS: DENSE A EXTRAORDINARILY WITH OF CONDITIONS PHYSICAL Morisset C. & COOKBOOK NEBULATOM THE CIEGLCI NUCLEI GALACTIC ACTIVE OF Mateus A. PROPERTIES GALAXIES POST-STARBURST POPULATION STELLAR COMPACT Valotto C. & IN GALAXIES OF GROUPS CORRELATION FIR/RADIO .A ie,adT Storchi-Bergmann T. and Riffel, A. R. 2110 THE NGC OF OF REGION CENTRAL Riffel A. KINEMATICS R. TWO-DIMENSIONAL & Kharb, P. Robinson, GALAXY A. Axon, ACTIVE J. D. THE IN 102B ARP SPIRAL NU- THE CLEAR OF EXCITATION AND KINEMATICS Ant´on MAGNI- S. & QSOs Andrei, DR7 H. ABSOLUTE SDSS THE OF TUDES AND Robinson A. SPEC- & MORPHOLOGY FROM Muller, S. A. FIELD NGC4501 Bergmann, INTEGRAL OF TROSCOPY REGION GMOS/GEMINI THE Sales OF A. CENTRAL D. KINEMATICS & Pastoriza, TWO-DIMENSIONAL G. M. Riffel, AGN R. OF FOR ert, PROPERTIES MODEL UNIFIED PHYSICAL THE THE TESTING .B isr,T .Bes .Crlo & Carollo, D. Beers, C. T. Tissera, B. P. .Tle,T .Tun .I ztv & Izotov, I. Y. Thuan, X. T. Telles, E. .Sd´ r .Albernaz-Sirico A. & Sodr´e Jr. L. .S ot,T Storchi-Bergmann, T. Couto, S. G. .Bu,R .Rffl .Storchi- T. Riffel, A. R. Brum, C. .R eaValdarenas Vena R. R. .Torres-Flores, S. .Ar´evaloP. .Valls-Gabaud D. .Schoenell, W. .Ceh,A. Coelho, B. .R Diniz, R. M. .Stasi´nskaG. .Wre& Werle A. .Audib- A. 190 188 188 187 187 187 189 189 189 192 191 191 190 190 186 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes .I .Dnz .G atrz,R ie,R A. AGN R. CIRCUMBINARY Riffel, DISKS IN R. Storchi-Bergmann FORMATION Pastoriza, T. GAP & G. Diniz, M. R. M. Diniz, Riffel, F. I. NGC1052 S. OF NATURE LINER THE UNVEILING euo .A eVt,&J .Horvath E. J. & BLACK Vito, De IN A. M. FIELD venuto, MAGNETIC PULSARS WIDOW OF DECAY Portilla G. J. & OP- THE IN SPECTRA LINERS TICAL AND SEYFERTS Andruchow IN I. FHILS & Scellone, A. S. Zafra, BANDS Torres G’ J. AND I’ THE FROM IN DATA 3C66A GEMINI-GMOS AND PG1553+113 OF BLAZARS ENVIRONMENT THE Mu˜noz THE A. CHARACTERIZING J. & Falco, E. Mediavilla, SDSS1155+6346 HE0047-1756 AND IN MICROLENSING CHROMATIC Riffel 2 R. & SEYFERT Bergmann, 5929 THE NGC IN GALAXY Dors OUTFLOWS O. & NUCLEAR Bonatto, C. Pastoriza, G. IN M. Broth- erton, S. II] M. Rodr´ıguez-Ardila, Aleman, GALAXIES A. I. [FE Riffel, FORMING STAR AND AND AGNS HYDROGEN MOLECULAR J.R. & Higuera-G., Mart´ınez-Galarza Mario-A. P., Ramos Andr´es F. GALAXIES OF TYPES DIFFERENT IN POLYCYCLIC HYDROCARBONS AROMATIC WITH Ferreiro D. DIAGRAM & DIAGNOSTIC Schmidt, E. Neme, Vega GALAXIES L. 1 SEYFERT LINE ROW NAR- IN Floyd CONTINUUM D. THE CHARACTERIZING & Webster, R. Neri-Larios, QSOS D. OF MICROLENSINGS ITATIONAL Davies GRAV- R. THROUGH ACCRETION & AGN Hicks, PROBING E. Malkan, M. EVO- Sanchez, GALAXIES THE SEYFERT IN OF Ricci FEEDBACK LUTION V. AGN ACTIVE T. OF & ROLE Menezes, THE THE B. R. Steiner, 1068 J. OF NGC OF NUCLEUS GALACTIC ARCHITECTURE Garcia- THE A. Rodr´ıguez-Ardila, & Rissmann A. Marinello, NUCLEI EMISSION O. GALACTIC FEII ACTIVE IN OF Storchi-Bergmann PROPERTIES T. PHYSICAL & Riffel, A. R. TOMOGRAPHY Hennig, MRK1066 PCA IN BY RING REVEALED MOLECULAR NUCLEAR A .Ecl .DlValle Del L. & Escala A. .J .Vr,A .Rodriguez, M. A. Vera, C. J. R. .M atlo .G Ben- G. O. Castilho, M. C. eisr .Qitr V., Quintero A. Seditsira .A ie,T Storchi- T. Riffel, A. R. .Rjs .Mta E. Motta, V. Rojas, K. .Mueller- F. .A Oio, A. G. .May, D. .A. M. .G. M. ABSTRACTS 192 197 196 196 196 195 195 195 194 194 194 193 193 193 192 R. .Kil,E .d ovi a io .V del V. M. Pino, ON Dal HIGHLIGHTS Gouveia Sol H. de & M. Valle, E. Khiali, B. FOR RADIATION MICROQUASARS MODEL EXPLAINING RECONNECTION MAGNETIC A H AATCDSRBTO FFERMI OF SOURCES DISTRIBUTION POINT GALACTIC Romero THE E. G. & Valle del SOURCES GAMMA-RAY CLASS GALACTIC NEW OF A AS STARS RUNAWAY MASSIVE Hadrava P. & AITO-YRDNMCMDLOF BINARIES X-RAY HIGH-MASS MODEL RADIATION-HYDRODYNAMIC ASINAAYE NPAC CMB PLANCK ON S. S. MAPS ANALYSES & Forman, R. GAUSSIAN W. Jones, C. Lopes, Murray A. A. P. RPRISO AAYGOP SE- BO THE GROUPS OBSERVA- OF X-RAY TIONS GALAXY CHANDRA FROM LECTED OF Dupke R. & PROPERTIES Oliveira, de Lopes R. Ribeiro, BL/C AAYCUTR PTO UP CLUSTERS GALAXY OF ABELL/ACO SUPERCLUSTERS OF CATALOGUES NEW Trejo-Alonso, Hern´andez-Aguayo Mu˜niz- C. J. A. & M. Torres, J. Santoyo-Ruiz, Anda-Su´arez, Andernach, H. de H. J. Caretta, A. CLUSTERS HOST C. THE THEIR AND OF EVOLUTION GALAXIES DOMINANT CENTRAL .Mre tal. et Moraes B. SURVEY STRIPE-82 CFHT/MEGACAM THE Stoeger R. W. & FUNC- MASS TION COSMOLOGICAL DES-Brazil GALAXY & THE Aguena, M. Camacho, consortium H. Lima, M. CLUSTERS GALAXY AND CORRE- FUNCTION ANGULAR LATION THE FROM COSMOLOGY 0 H OA UNIVERSE IN LOCAL EVENTS THE RAY IA GAMMA TYPE AND SUPERNOVAE USING S. DISTANCES & CONTRASTING Gomez-Alvarez F. M. Velasco-Moreno Forero-Romero, E. J. HISTORY COSMIC IN OF GIGAYEAR GROWTH FIRST THE HOLE & Sochting, BLACK K. SUPER-MASSIVE I. Campusano, Graham E. J. L. M. Harris, A. K. IN STRUCTURE UNIVERSE LARGEST THE THE HUGE-LQG- Caretta . 15 .Co atıe,H nenc,&C A. C. & Andernach, Mart´ınez, H. Chow M. .Bernui A. .R oe,A rbre,M .Ribeiro, B. M. Iribarrem, A. Lopes, R. A. γCAS .G lws .Raghunathan, S. Clowes, G. R. TSFIELD OTES ¨ .Jbosi&P Polido P. & Jablonski F. LK STARS -LIKE .Girola R. J. .Vajgel, B. Cechura ˇ .M. E. .V. M. z 198 198 198 197 199 199 200 199 223 202 202 202 201 201 201 200 ∼ XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes H ADXRYTLSOE O MIRAX PROTOMIRAX FOR AND TELESCOPES X-RAY HARD THE Walker D. ALL- CAMERA AN SKY WITH COEFFICIENTS Mello EXTINCTION A. & Kanaan, A. MODULATORSBernardi, LIGHT SPATIAL WITH SIMULATIONS TURBULENCE ATMOSPHERIC Infante L. & Puzia, SOAR WIDE-FIELD, TELESCOPE THE 4M FOR MULTI-BAND, IMAGER UV/OPTICAL NEAR A BOMBOLO: al. et CLUSTERS IN- GALAXY SUPERNOVAE RICH IA SIDE TYPE C. & OF Lagan´a,PROPERTIES Neto, Lima F. Oliveira B. T. de G. Mendes Caretta, Cypriano, A. E. Sodr´e Jr., C. L. Trejo-Alonso, CLUSTERS J. AXU J. OF SEQUENCE RED THE Calv˜ao O. M. (J-PAS) SUR- VEY ASTROPHYSICAL FOR UNIVERSE ACCEL- PIPELINE THE ERATING OF SUPERNOVA PHYSICS JAVALAMBRE IA THE TYPE Rodriguez F. THE Merch´an, & E. M. Paz, J. MODEL HALO ANISOTROPIC OBSERVA- Larra˜naga-Rubio A. AN E. IN- ON LEVEL TIONAL POSSIBLE CORRECTIONS AND DUCED UNIVERSE BRANE THE FOR GRAVITATIONAL FORMULATION WAVES Abramo QUASARS Raul L. OF OF FILTERS NARROW-BAND WITH EXTRACTION REDSHIFTS PHOTOMETRIC AND IDENTIFICATION E. Pereira Makler, R. M. & Moraes, Bertin, B. SURVEY Charbonnier, 82 A. IN Pereira, STRIPE Shapiro CFHT MORPHOLOGIES L. THE I. GALAXY & Salles, MEASURING O. F. Fabris, C. J. son, MODI- INFLATION STAROBINSKY THE FIED IN SOLUTIONS COSMOLOGICAL OF STABILITY AND WAVES GRAVITATIONAL Jr GEN- EOS A DE WITH ERALIZED MODEL QUINTESSENCE COU- PLED A ON Forero-Romero CONSTRAINTS OBSERVATIONAL E. J. M¨uller, & V. THE Cuartas, FIELD DENSITY OF MASS COSMIC RECONSTRUCTION HALO-BASED 224 .B iet .R .Ri,& Reis, R. R. R. Siffert, B. B. .S otlto .Kna,& Kanaan, A. Bortolotto, S. G. .Agln,D uma,T H. Guzm´an, T. D. Angeloni, R. .C ue .M Barbosa M. E. & Nunes C. R. .D Rodr´ıguez-Camargo & D. C. .Baae al. et Braga J. .A Sgr´o, D. A. M. .C Mu˜noz- C. J. .Qerz& Queiroz C. .S Xavier S. H. .M Pelin- M. A. .E S. E. M. ABSTRACTS 207 207 207 206 206 205 205 205 204 204 204 203 203 203 R. MMTRON al. et Carrasco R. RESULTS TO E. SCIENCE COMMISSIONING AND OPERATIONS FROM GEMS/GSAOI: ETSD EDUCACI DE CENTES aSla .F Barroso “PLANET F. M. & Silva, da COM- RESOURCE SYN- PUTATIONAL BY MEDIATED MOON’S ROTATION CHRONOUS OF EVALUATION Orellana LEARNING B. R. & Biasi De OT O:RVAIGTEPOLARIZED THE SKY REVEALING SOUTHERN Butterley POL: T. & SOUTH Wilson, W. R. Tokovinin, A. ANSKPE”ADISINSTITUTIONAL ITS AND KEPLER” HANNES ALFABETIZACI Minniti Gar- D. D. Clari´a, & Medel, Amˆores, J. R. E. Good, Lambas, J. cia Gurovich, S. VVV Cabral, THE J. WITH SCIENCE Horvath COMMUNITY E. J. & Jafelice, AS- C. PERSPECTIVES OF AND TIONS JOURNAL CONTRIBU- (RELEA): AMERICAN EDUCATION TRONOMY LATIN THE Hetem A. & INSTRUC- SPECTROSCOPES TIONAL FOR SYSTEM ACQUISITION DATA aai,F hr .Gonz´alez C. ESO Char, F. AT Sarazin, LUSCI AND OBSERVATORYPARANAL SL-SLODAR THE PROFILING WITH TURBULENCE LAYER SURFACE UCACI MRVN INPE IMPROVING UESINEPOTENTIAL SCIENCE FU- TURE AND HIGHLIGHTS SCIENCE FIRST OBSERVA- - TORY INFRARED AIRBORNE SOFIA THE Boscardin S. & Sigismondi ZENITHAL C. PERSPECTIVE AND HISTORICAL A HELIOLATITUDES DISTANCES: ALL REFRACTION AT DIFFERENTIAL COMPUTING Guzm´an D. & ARTIFICIAL NETWORKS USING NEURAL IN SENSORS WAVEFRONT CENTROIDING SHACK-HARTMANN FOR FOR SPOTS ELONGATED ALGORITHM NEW & Cardoso, P. Cardoso, Braga L. J. Fernandes, O. J. Rinke, EXPERIMENT RAX PROTOMI- THE OF OPERATION FOR CILITIES NSCNAI NL PLATA LA EN SECUNDARIA ON ´ ROETAR IIA JO- DIGITAL TEATRO E ARIO ´ .d Graauw de T. NE SRNMı EDO- ASTRONOM´ıA DE EN ON ´ ′ .M Magalh˜aes M. A. ALO RUDFA- GROUND BALLOON S NPIAI EED- DE Y PRIMARIA ON ´ .MtiloFacso E. Mattiello-Francisco, F. .T el,A Kanaan, A. Mello, T. A. vl,J Navarrete, J. Avila, ´ .B .BAlmeida B S. B. C. .L auds T. Fagundes, L. A. .S rtns L. Bretones, S. P. .Lmad,M. Lombardi, G. .Zinnecker H. .S. M. 208 213 212 208 212 211 211 211 208 209 210 210 209 XIV Latin American Regional IAU Meeting (Florianópolis/SC, Brazil, 25-30 November 2013) Editors: A. Mateus, J. Gregorio-Hetem & R. Cid Fernandes EAOIA PROJECT PEDAGOGICAL FTESNADTESAOSO H OB- THE OF SHADOWS JECTS THE AND MOVEMENT SUN THE APPARENT OF THE ABOUT TIONS CONCEP- TEACHERS’ SCHOOL ELEMENTARY Voelzke R. TEACH- ASTRONOMY OF THE ING IN MATERIALS INTERACTIVE Vila¸ca J. & Langhi PROJECT ERATOSTHENES BRAZILIAN AIGSINEI H OT FBRAZIL OF SOUTH THE IN DISSEMI- SCIENCE NATING AND TEACHERS UNI- TRAINING THE VERSE: OF ADVENTURERS AND GTTP OEI, .I Machado I. D. .A aˆd M. Macˆedo & A. J. .Z ai tal. et Faria Z. R. ABSTRACTS 213 214 213 214 R. AINLATOOIA ERHCOL- SEARCH LABORATION ASTRONOMICAL INTER- NATIONAL THE IN PARTICIPATIONS Buitrago-Casas Nieto, BRAZILIAN C. Jimenez J. & D. Ramos, J. F. Restrepo, A. Hoyos P. Moreno, STU- FOR DENTS Dottori STUDENTS, BY H. NETWORK & A Saraiva, RECA: O. F. M. Pavani, B. D. aaz,L laee .Naidoo T. & PROJECT Albanese, UNAWE L. EU Zanazzi, THE OF WORK FRAME- THE IN CONNECTIONS LIKE) EFFECTIVE COSTLESS (SKYPE THROUGH ITALY: ACTIVITY CALLS EXCHANGE AFRICA SOUTH .C eoiaGterz .Velasco S. Gutierrez, Remolina C. M. .A oa tal. et Rojas A. G. 216 215 215 215 225 A.