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Oral Programme Abstracts Monday, 18th July 2011

13 Formation, Durham, Monday, 18th July 2011 Institute of Astronomy, University of Cambridge 14 Prof Robert Kennicutt [email protected] Notes Abstract Thanks to an infusion of multi-wavelengthsystematic observations patterns of and -forming scaling laws near governingreveal and large-scale deeper far, star insights we formation into are in the now unprecedented physical regulation able detail.challenge of to These the star study new formation, simple the observations as empirical well prescriptions asstar-forming new and galaxies. complications theoretical and inconsistencies descriptions This which talk whichaddressed will underlie with review most ALMA the models and current and other new state simulations facilities. of of this rapidly evolving subject, and identify key issues to be Galaxy-wide processes Galaxy Formation, Durham, Monday, 18th July 2011 MPA [email protected] Prof Simon White 15 Notes Abstract The current and past systematic properties ofcharacteristic the velocity, galaxy morphology, population – star-formation abundances rate andties and clustering – as , a provide as function our of well mass, principal asTechniques size, source scaling for of relations simulating information between the about these global the proper- propertiesof one of processes or large regulating a populations few the systems, of formation began galaxies,It and to rather be is evolution than developed now of in the the possible galaxies. detailed late to internal 1990’sto follow and structure giant have the made cluster formation dramatic cD’s progress and in within evolution thelations a subsequent of constrain single decade. the the simulation, full efficiency and galaxy so andgalaxy population to parameter merging, from the investigate dependences growth Local how of of Group central observed processes black dwarf abundances, such holes,largest spheroidals clustering and simulations as the and to ejection the date scaling of sequestration follow mass, re- energy of thethose and formation baryons planned heavy and for elements in next evolution in generation galaxies, galactic of cosmological winds. hundreds surveys. The ofplementation Recent millions technical of advances of MCMC of galaxies importance techniques within in for this volumes area theof similar include systematic the to a im- exploration scaling of scheme high-dimensional which parameterin allows spaces, any the a other development dark cosmology matter consistent simulationtelescopes with carried which current out allow CMB in and past one large-scale light-conesHST cosmology structure in or to constraints, ground-based the represent and surveys. simulations structure the These to construction developments formation uncertainties be open of in rendered up galaxy virtual the as formation possibility physics images of will directly investigating affect directly comparable the and precision to systematically of those how cosmological of inferences deep from future surveys. The formation and evolution of the galaxy population Galaxy Formation, Durham, Monday, 18th July 2011 MPA Dr Guinevere Kauffmann [email protected] 16 Notes Abstract I will discuss whatphysical the properties past of generation galaxies, of asand large well dark as spectroscopic matter the galaxy halo relations masses. surveys between have the taught physicalI properties us will of then about focus galaxies relations on and the between their so-calledfundamental “galaxy environments the relation. bi-modality”, reviewing I the will physical attempt processesproduces that to might two elucidate be such the at different kinds work classes in of of shaping observations galaxy. this that may finally clarify why the LCDM Universe Clues to galaxy formation from local populations Galaxy Formation, Durham, Monday, 18th July 2011 ETH Zurich Prof Simon Lilly [email protected] 17 ) 2 z < Notes Abstract I will briefly review some ofz the main 2 observational and results later. concerningwill I the mostly will evolution focus introduce on of the those the broad underlying galaxy range simplicitiesbe population, of of used phenomena especially the to concerned, galaxy at derive including population the flows that analytic of have form(s) gas emerged for onto from the and large dominant off surveys. evolutionary of These processes galaxies, can concerned. but Late galaxy evolution ( Galaxy Formation, Durham, Monday, 18th July 2011 CEA – Saclay Dr David Elbaz [email protected] –2.5. This is also the epoch when the cosmic 5 . = 0 z 18 Notes star formation history peaked andof started debate to and decline various until physicalthe present-day. mechanisms quenching have The of been star cause invoked formation of toHST from this of explain AGN decline the feedback it dominant has or ranging galaxy been population simply from a atthat the a these major the exhaustion redshifts drop theme of gas revealed of the the reservoirs the presence gas participating of rateThese content to large of instabilities of clumps these could of mergers galaxies. major either star to events formation result Imaging suggesting of from with filaments, major star the mergers formation of so-called were galaxies cold subject or flows. to berelating driven strong The star by dynamical formation recent intergalactic in instabilities. finding infall galaxies that of with star material theirredshifts, through formation stellar has mass obeyed been and invoked some gas to simple content, favor scaling extending the the laws cold Schmidt-Kennicutt atHowever, flow relation all the scenario. to determination redshifts high of the starWith formation rate Herschel, of it galaxies suffers is from nowa strong possible uncertainties major due to step to determine dust forward with obscuration. inWe unprecedented the will accuracy review understanding the some of actual of the the SFRforming dominant recent of galaxies. factors results distant obtained playing galaxies in a and this role context make in and the present evidence building for of an present-day infrared galaxies. scaling law for star- Abstract Most present-day were formed at intermediate redshifts, i.e. Star formation at intermediate redshift Galaxy Formation, Durham, Monday, 18th July 2011 Leiden University Dr Joop Schaye [email protected] 19 Notes Abstract I will review methods and recentI developments in will large also volume present SPH some simulations recent of results the from formation the and OWLS evolution project. of galaxies. SPH simulations of the formation and evolution of galaxies Galaxy Formation, Durham, Monday, 18th July 2011 University of Victoria Dr Sara Ellison [email protected] 20 Notes Abstract Bars and galaxy-galaxy mergers represent themation two in main galaxies. mechanisms for I triggeringgas-phase gas will inflows present measured that in a lead SDSS comparative to galaxiescontributions central study to of star of probe bars for- the these and efficiency merger-induced two of gas mechanisms gas inflows which flows. in contributing uses These to results the the will star build-up reveal of formation the the rates relative stellar and bulge. Gas flows in galaxies: mergers versus bars Galaxy Formation, Durham, Monday, 18th July 2011 Universidad Autonoma de Madrid 21 Dr Patricia Sanchez-Blazquez [email protected] Notes Abstract We will present star formation histories and thespiral stellar galaxies and with gaseous metallicity and gradients without in barsgalactic the disk with disks of the due a aim sample to of of bars 50 quantifying bynon-barred face-on the comparying galaxies. redistribution both Numerical of the simulations mass have gas-phase and shown andinduce that angular star-phase evolutionary strong momentum metallicity processes gravitational in gradients such torque the as on by redistribution the non-axisymmetricney of components disk mass 2002) of and and barred angular consequent and momentum change in ofand the chemical their galactic abundance disks evolution (Sellwood profiles. we & must If Bin- ponents understand we and the hope vice-versa. to secular understand processes Furthermore, chemical andcritical the evolution re-arrangement observed gradients re-arrangement of metrics of material of stellar by Galaxy disk non-axisymmetric evolution,G-dwarf com- including metallicity material distribution. the influences Perhaps age-metallicity the the relation most interpretation in obvious- of of the these at various solar aforementioned least neighborhood non-axisymmetric 2/3 components and are of the bars While spiral local observationally galaxies it host has been a found bar, thatgalaxies, and barred galaxies a possibly have complementary all shallower gas-phase analysis disk metallicity galaxies of gradientscause have the than non-barred the hosted stellar a study abundance bar profiles of at has bothsuffer some not gas from) point yet very and in been different stars their evolutionary undertaken. is evolution. process. This important is in unfortunate providing be- a complete picture, as the two components undergo (and Quantifying the mixing due to bars Galaxy Formation, Durham, Monday, 18th July 2011 University of Nottingham 0.5) we have concentrated on the putative ∼ 22 [email protected] Prof Alfonso Aragon-Salamanca Notes progenitors - spiral galaxies -interesting and results. the Although there galaxies are caught still in some the loose ends, act a of coherent transforming. picture may In be emerging. this talk I present some of our more Abstract Evidence is mounting indicating that S0s weremorphology. once spiral Studying galaxies the that timing, ceased location forming and stars physicalin and mechanism(s) subsequently involved itself, changed in but their this transformation it is can notthe only also interesting last provide few very years we useful have clues beenfind on following out several how where lines galaxies of it evolve research happens, to andof and test the the whether look possible transformation this for role transformation - the is of the indeed physics the S0s taking driving environment. themselves place, it. - During while At at low intermediate redshift redshifts we (z have studied in detail the final products Transforming spirals into S0s Galaxy Formation, Durham, Monday, 18th July 2011 Kavli Institute for Cosmology, Cambridge 23 Dr Andrew Pontzen [email protected] Notes Abstract Recent simulation work (Governato et al.tionally 2010) consistent has ’cored’ produced dark dwarf matter galaxies central which profilegas. are (Oh both et bulgeless While al. and adiabatic have 2010). expansion an Both observa- wasflows, effects previously it are thought known was to to not be be the clearNavarro result capable et whether of of al outflowing the modifying 1996, effects Gnedin dark & could matterthe Zhao be profiles detailed 2002, physical in large Read mechanism response & enough at Gilmore to to work 2005).and out- in resolve a It flattening physical the is model cusps aimed therefore observational into at imperative cores cusp/core doing to in justfor discrepancy that. reach Governato a (e.g. a et In much full the al’s new understanding more work. picture of I pronounced Itests present, present effect the of new ’burstiness’ than the of simulations scenario. generally the outflows supposed is crucial, from allowing adiabatic calculations. I outline possible observational Flattening cusps with supernova feedback: a physical model Galaxy Formation, Durham, Monday, 18th July 2011 24 Dunlap Institute for Astronomy & Astrophysics, University of Toronto effective radii in a number of early-type galaxies, over the full galaxy field. We not only obtain 5 - 3 Dr Anne-Marie Weijmans [email protected] Notes stellar and gas kinematics, which areinfer the used properties to of construct the mass stellar halo modelsdark population. of halo that I the will we dark show can halo, our obtain be recent with we results, these and also measurements. discuss measure the line properties strengths of the to stellar and Abstract From galaxy formation theories, we expect galaxiesthese to be haloes embedded are in not massive haloes always of straightforward darkgravitationally matter. to potential detect: For in early-type they spiral galaxies often galaxies lackonly and the a we large handful are cold of therefore gas forced early-type discstheoretical that to galaxies predictions are use the of used other, dark as galaxy less haloes tracers formationthe accessible of have models tracers. Atlas3D the been against Survey mapped. As to observations. a increase This result,obtained We this poses spectra for have number. a out therefore to problem Using started for integral-field a direct spectrographs programme comparisons such within of as SAURON and VIRUS-P, we have Mapping dark and stellar haloes with integral-field spectrography Galaxy Formation, Durham, Monday, 18th July 2011 University of California, Santa Cruz [email protected] Prof Joel Primack 25 Notes Abstract The highest resolution cosmological simulationsimulation based has on been the current basis cosmological for a parameterson series is of semi-analytic the papers modeling. based Bolshoi There on simulation. halo are abundance alsosummarize matching, This larger the and and new key smaller papers results simulations in both in preparation from based the the Bolshoi/MultiDark Bolshoi series. simulation In suite this and talk the I research will based on it. The Bolshoi Cosmological Simulations and Their Implications Galaxy Formation, Durham, Monday, 18th July 2011 University of Waterloo Prof Mike Hudson [email protected] 26 Notes Abstract Halo masses are a key ingredient forthis understanding galaxy problem. evolution. Galaxy-galaxy The lensing CFHT providesshapes a Legacy new and way Survey 5-band to Wide photometric approach component redshiftsdetermination over has of 170 been galaxy-scale sq analyzed halo degrees. masses by as I the a will CFHTLenS function present of team, results galaxy providing from , accurate this colour unique and redshift. dataset, allowing the Galaxy evolution from weak lensing with CFHTLenS Galaxy Formation, Durham, Monday, 18th July 2011 Universidad Católica de Chile mergers with little star formation 4 − 1 ∼ sample. Applying this method to ETG galaxies Galaxy Descendants z z Dr Nelson Padilla [email protected] 27 , these galaxies undergo 0 and = 1 z in the MUSYC survey, we findactivity. that between Notes Abstract We will present a method toIf select the descendants number of density high and redshiftdark-matter clustering haloes galaxies, amplitude at motivated the of same in redshift a results in sample EPS fromwhere theory of numerical the or galaxies numerical simulations. properties simulations. is of The known, the latter descendant can thesethis be population can new followed can redshift to be lower be can matched redshifts, inferred. be to considered The a as observational statistical population sample descendants of that of shares the this higher properties at Clustering and Number Density Selection of High- Galaxy Formation, Durham, Monday, 18th July 2011 Instituto de Astrofísica de Canarias 28 [email protected] Dr Alexandre Vazdekis Notes Abstract Massive galaxies are known to show stellarformation populations timescales. that We are present enhanced a in new alpha-elements, generationately high which of resolution. stellar may population indicate These models predictions very predicting are short based alpha-enhancedmospheres. on SEDs the at We empirical moder- show stellar that library these MILES, models with provide theand significantly aid colours. of better theoretical fits We stellar to also at- observed introduce galaxy spectra, web-basedclude absorption tools these line-strengths for alpha-enhanced building-up predictions. model SEDs for varying star formation histories, which in- Alpha-enhanced stellar populations models for studying massive galaxies Galaxy Formation, Durham, Monday, 18th July 2011 17 10 to 10 10 University of Sussex Dr Jon Loveday [email protected] 29 . I will present measurements of the galaxy luminosity function 4 . 0 ∼ z Solar masses over 150 square(LF) degrees in to the redshift ugriz bands for these groups, highlighting the evolving dependence of LF on halo mass. Notes Abstract The Galaxy and Mass Assembly (GAMA) survey has determined dynamical masses for 14,000 galaxy groups of Galaxy luminosity function: dependence on halo mass Galaxy Formation, Durham, Monday, 18th July 2011 Institute of Astronomy, ETH Zurich , indicating that two distinct physical pro- 1 ∼ z Mr Yingjie Peng [email protected] 30 cesses are operating, namely theenvironment “mass quenching” quenching, and we “environment then quenching”. suspectthe Considering star that the formation the unique of environment features the quenching ofSDSS star the DR7 forming is group galaxies actually catalogues are satellite quenched are quenching,pecially as employed the through they to distinction fall investigate which of into the environment larger dependencethe haloes quenching of observations and effect various and become on galaxy satellites. the centrals properties and predictions on Thealmost satellites. environment, from perfectly new with es- Peng We the et find predictions al. of excellentenvironments our agreements from (2010) model. between high model. I to will low also The redshifts, discuss with mass the some functions global other of evolution interesting of centrals implications the from and mass this satellites functions model. in follow different Notes Abstract The galaxy population appears towhen be large composed samples of of infinitely galaxies complex areand different similar studied, types evolutional it and modes appears while properties that the at theships outliers first vast among represent sight, majority stellar some mass, of however, minority. star galaxies The formation justdifferential underlying rate follow effects simplicities and simple of of environment scaling mass the are relations and interrelation- seen environment in are SDSS completely and separable zCOSMOS. We to demonstrate that the The Simplicity of Galaxy Evolution and Environment Quenching in SDSS Galaxy Formation, Durham, Monday, 18th July 2011 . Possible resolutions New York University gal M galaxies move back and forth between at their centers, a quarter of which are 5 ⋆ . L 10 Dr Jeremy Tinker [email protected] 10 < gal M 31 red galaxies. Dark matter halos exhibit a similar effect, known as assembly bias; ⋆ L , the types of halos that house galaxies with ⊙ M 12 10 < halo M Notes at fixed halo mass, old,mass slow-growing halos form preferentiallyquenched of dense their environments. star formation. This Usingthe a effect galaxy galaxy is population group strongest catalog into to for centralthese determine and halos low-mass the satellite of halo galaxies. masses galaxies, ofI I galaxies, willany explore and scale demonstrate the to larger that decompose environmental than the dependence the fraction of halotrack of the scale) galaxy red-and-dead growth at properties galaxies of fixed halos. for is stellar The independent andexcluded ansatz of halo by that environment mass. the quenched (at field data, I and implying will thata compare galaxies conundrum halo live these for in growth results the halos and to subhalo that galaxy N-body abundance have growthsame matching simulations stopped dark are paradigm, growing that in mass, uncorrelated is which clearly regardless for galaxies of low-mass of whether objects.normal the the rates same This galaxies for stellar represents are mass their forming occupy mass, stars halos redare or of galaxies that not. the should these If live galaxies quenched in galaxies only different live recently halos in quenched that halos blue their that galaxies star grow at formation, at fixed or that sub- Abstract It is well known that galaxy bimodalityregions. depends on This environment; is red, dead, especially early-type true galaxies for primarily live sub- in high-density Are Galaxy Growth and Halo Growth Correlated? the blue cloud and red sequence. Galaxy Formation, Durham, Monday, 18th July 2011 130K redshifts. This ∼ University of St Andrews solar masses. As well as offering a 12 10 [email protected] Dr Aaron Robotham 32 catalogue allows us to observationally probenew the constraint halo to mass the function temperature (HMF) of down dark-not to matter, density- this a also much means more we fundamental discriminator canhave when now attempting on probe to environment the pick as fate apart a of the function galaxies. roles of stellar halo mass mass and environment Notes Abstract We present the GAMA Cataloguethe (G3C). GAMA This redshift is survey the being highest nearly fidelity 100% group complete catalogue over ever 144 constructed, sq. virtue deg. of of the sky- containing in total The GAMA Galaxy Group Catalogue: Probing the Universe One Halo at a Time Galaxy Formation, Durham, Monday, 18th July 2011 33 National Astronomical Observatories, Chinese Academy of Sciences Dr Qi Guo [email protected] 0.5) far-infrared selected galaxies in the PhaseI field of the Herschel-ATLAS (H-ATLAS) survey, < optically selected galaxies from the Galaxy and Massgalaxies Assembly to (GAMA) investigate redshift how survey and the group distribution cataloguehalo and based mass. formation on GAMA of FIR galaxies depend on environmental effect, e.g. dark matter Notes Abstract We us low-redshift (z Environmental dependence on Herschel-ATLAS galaxies Galaxy Formation, Durham, Monday, 18th July 2011 INAF - Padova observatory Miss Benedetta Vulcani [email protected] 34 Notes Abstract The properties of galaxies change in awhich systematic factor way with is galaxy the mass, most with redshift importantthat and in several with driving galaxy environment. galaxy properties Understanding evolution are isfunction largely one of determined of galaxies by the in the main clusters, stellar goal asA mass. of a results I the that function will astrophysics. has of present several the It the far galaxymorphological is first reaching morphological evolution well determination implications type, known of of for and the galaxies. the how mass mass itfunction assembly, evolves I of the between EACH can mass z=0.8 morphological show segregation and types with how z=0. cause (ellipticals, environment strong this. and S0s is the and the I late-types) evolution will inthe of clusters, also morphological and fractions. the show discuss total how Then, the mass fixing muchenvironments possible a function, the (clusters, processes redshift, morphology-mass and that groups, I relation of field). will depends the presentformation Moreover, how on mass rate much I relation redshift, the can between according mass clusters, present to distributionexplain groups the varies the and the first among evolution field quenching study different at of of of high-z, star thearXiv:1010.4442 and formation ) difference what (Vulcani this of et means the al. for stellar the mass 2010 mechanisms – ApJLetter proposed 710 star to L1, and Vulcani et al. 2010 MNRAS in press, z=0 as a function of environment The evolution of the galaxy mass assembly and star formation activity from z=1 to Galaxy Formation, Durham, Monday, 18th July 2011 < z < 3 . 0 Yale University Mr Tomer Tal [email protected] 35 despite only moderate growth in mass. 2 ∼ z 7 . 0 and discuss the implications of our findings to show that stellar mass growth in massive ellipticals is heavily ∼ 1 . 0 z ∼ using SDSS imaging data. We select objects that are identified as Luminous Red Galaxies from SDSS-III BOSS spectra z 7 . influenced by minor mergers. Thismassive is galaxies especially since relevant in light of recent observations that show significant sizeNotes growth in 0 and associate their group members statisticallyluminosity function using therefore randomly represents the selected group regions mass within over-densityluminosity in function the respect around same to the its SDSS most surroundings. massive fields. We redmass show The galaxies that has contribution derived the evolved group of significantly in satellite theat last accretion six to Gyrs and the estimate the central total galaxy. We also compare our results with a study of local groups Abstract We present an empirical study of the group luminosity function around massive red galaxies in the redshift range since Direct observations of the evolving group luminosity function of massive red galaxies Galaxy Formation, Durham, Monday, 18th July 2011 Leiden University 1.5, and their remarkably > Prof Marijn Franx [email protected] 36 high density and small size.deep photometry, leaving I no review doubt the thatbeyond new they three, are results but truely remakably which compact enough, have and theirbe very come star easier massive. forming out, to These progenitors including find. galaxies have kinematic Comparisons can not of be been measurements the found identified and evolution to yet very of - redshifts the even mass though size theyNotes relation should with theoretical predictions are presented. Abstract One of the surprising results of the last decade is the discovery of quiescent galaxies at redshifts The emergence of the red sequence Galaxy Formation, Durham, Monday, 18th July 2011 9.5) 1. By < ∼ SAAO log Ms < Dr David Gilbank [email protected] 1 ∼ 37 1. I will present results from ROLES (the Redshift One LDSS-3 Emission line Survey) which, combined with other ∼ Notes comparison with a local samplewe drawn can from the measure SDSS the (which mass-dependentobserved is timescales star-formation also for history used star-formation of compare to the with assess the Universe the predictions calibration over of of half the our Durham its semi-analytic SFR age. model, indicators), Galform. I will also discuss how the Abstract Motivated by suggestions of ‘cosmic downsizing’ in which the(SFRD) dominant proceeds contribution from to higher the to cosmic lower star mass formation galaxies rateat density with increasing directly cosmic exploring time, we for have recently the completed first a survey time aimed the spectroscopic star-formation activity in low mass galaxies (8.5 From dwarfs to giants: the history of star formation since z higher mass surveys, has measured the cosmic star-formation rate density (SFRD) as a function of stellar mass at z at z 38 Oral Programme Abstracts Tuesday, 19th July 2011

39 Galaxy Formation, Durham, Tuesday, 19th July 2011 University of Groningen Prof Amina Helmi [email protected] 40 Notes Abstract I will review our current understandingpopulations and of their the internal dynamics. Milky These Way systems and arethe unique its kinematics, since satellites, we ages can and with study abundances them emphasis in of on incredibleto individual detail the put by stars. properties strong measuring Together of and with very their the complementary stellar many constraints ongoing on large cosmological surveys models this of has galaxy allowed evolution. us Clues to galaxy formation from the and Local Group perspective Galaxy Formation, Durham, Tuesday, 19th July 2011 Durham University [email protected] Prof Carlos Frenk 41 Kev) only a few because of the cutoff in the power spectrum due to free streaming. Characterising the 4 ∼ CDM model accounts suprisingly well for an impressive amount of data on the cosmic large-scale structure, ranging in Λ Notes scale from a few gigaparsecs toof a rigour few as megaparsecs. on On larger megaparsecand scales scales well-understood where the diagnostics. model microwave Yet, cannot it background is be radiation preciselyclearly. tested on data with small For and the scales example, measures where same the N-body degree of nature simulations galaxylook of the of completely clustering dark galactic different: provide matter dark manifests clean the itself matter former most halosparticle produce of made a mass very of large cold number (CDM) of or substructures, warm the (WDM) latter dark (in matter the case of a dark matter Abstract The nature of structure on subgalactic scales is thereforeIn a this key talk to I understanding will the review nature howthree we of aspects can the learn which dark about are matter. dark particularly matterand informative: from (iii) the (i) the properties combination of the the of luminosity satellites (i) function of andgalaxy the of (ii). formation Milky satellites, I Way. is will (ii) There strongly show the are that suppressed dynamicscomes CDM by of has at no the reionization the difficulty satellites and in expense supernova explainingresolution of the feedback luminosity CDM a in function simulations because large small whose subhalos, population potentialWay although of wells this satellites. barren are success or consistent There dark withcorrect is subhalos. the satellite a available Similarly, in problem, spectro-kinematic subhalos it however, data thatmatch is are for when much the possible the too (i) dynamical to massive Milky data, and compared find require with (ii)whose subhalos the observations. are dark brightest in Equivalently, matter considered models satellites distribution high that to is together: much formto too current in concentrated this medium CDM to discrepancy: sized be models compatible halos, (i) place with rathercomplex the the the than feedback data. Milky in processes There the satellite are not most system three includedsimulations massive possible is in to solutions not illustrate current possibilities typical; models. (i) (ii) and I (ii). the will dark use matter both is semi-analytical not techniques cold and but cosmological warm; (iii) there are The satellites of the Milky Way as a probe of the nature of dark matter Galaxy Formation, Durham, Tuesday, 19th July 2011 Max Planck Institute for Astronomy 42 Prof Hans-Walter Rix [email protected] Notes Abstract The stellar-population-dependent structure and kinematics offor our shaping our Galaxy’s thinking disk about has disk galaxy historicallydances formation been for and large an evolution. stellar important samples New beyond testbed data the sets, solarnew neighborhood providing in ways detailed the kinematics to Milky and Way, test abun- have internal great potential andbased to external on provide disk qualitatively SDSS/SEGUE. evolution mechanism. I’ll discuss recent results and insights, in particular ones Dissecting the Milky Way’s Stellar Disks Galaxy Formation, Durham, Tuesday, 19th July 2011 Observatoire de Paris Prof Francoise Combes [email protected] 43 Notes Abstract In galaxy formation scenarios, slowously dynamical accreting processes, matter where from the cosmicmergers. galaxies filaments, Galaxy remain disks compete in develop with non-axisymmetric quasi-equilibrium, waves, more whiletum such violent as outwards, continu- bars and evolution, and concentrate spirals, triggered the to mass. by transferin Perpendicular efficiently galaxy bar particular the resonances interactions angular in form momen- and late-type pseudo-bulges, galaxies. which arebe The frequently discussed. observed relative importance Secular of evolution theThe two may observed formation/evolution bar alleviate scenarios frequency the can to also problem assemble quantify ofwould mass the double amount will too its of massive slow mass gas bulge in accretion about formation all 10 along in Gyr. a the galaxy Cosmological life-time. standard simulations Typically LCDM confirm a the theory. galaxy importance of accretion. Secular evolution of galaxies Galaxy Formation, Durham, Tuesday, 19th July 2011 200pc, ∼ Max Planck Institute for Astrophysics Dr Andrew Cooper [email protected] 44 Notes these are currently the onlygalaxies. fully cosmological I will models focus of on galactic resultsgalaxy that stellar compare formation haloes the models. that latest I resolve Milky will Way the then andon cold present M31 a a streams observations phase-space method with of correlation explicit for function. faint predictions quantifying dwarf I from theissue will CDM degree of use of ‘in this substructure situ’ method in to halo halo compare star star our formation.theoretical surveys, simulations basis Finally based to for I data will the from describe systematic SDSS ongoing study andexample). work address of with the By diffuse the combining light Millennium such around II surveys large simulation. with samplesevolution. This HI of provides observations galaxies a we (from aim SDSS learn and more PanSTARRS, about for the role of satellite accretion in galaxy Abstract I will present simulations of thenew formation and technique destruction for of these satellites simulations, in combining Milky Way-like N-body dark and haloes. semi-analytic We methods. have With developed a a spatial resolution of Galactic Stellar Haloes in the CDM model Galaxy Formation, Durham, Tuesday, 19th July 2011 Max-Planck Institut fur Astronomy 45 [email protected] Dr David Martinez-Delgado Notes Abstract Within the hierarchical framework forgalaxies galaxy formation, to minor this merging day. andgalaxies tidal As in interactions the part are local of expected universe a to withsurface shape pilot data brightness large taken survey, sensitivity. at we Our small observational have (0.1 efforttures to carried has in 0.5-meter out led the diameter), to ultra-deep, halos robotic the of telescopes wide-field discovery that thesepresents imaging of provide galaxies, an previously of exquisite likely undetected assortment some associated giant with of isolated stellar debriswith tidal struc- spiral from available phenomena tidally stellar exhibiting disrupted halo satellites. strikingly simulations Ourety diverse set of collection in morphological morphological of a characteristics. specimens galaxies Lambda-Cold detected Dark in Oursupport Matter our that comparison survey cosmology the could suggests hierarchical represent that formation one thisto of scenarios extraordinary the the predicted vari- Milky first by Way comprehensive these in pieces theoretical the of models Local evidence apply Volume. to I generally will to also galaxies present similar the discoveryup of observations a with tidal stream Subaru around telescopeof a show nearby a this dwarf minuscule irregular stream merger galaxy completely in withimportant resolved a our role LMC-type into small in system telescopes. stars, the in providing Follow- star the formation observational local history evidence and universe. evolution This of result nearby dwarf suggests galaxies. that dwarf accretion could play an Universe with small telescopes Stellar tidal streams in nearby galaxies: mapping the minor merger rate in the local Galaxy Formation, Durham, Tuesday, 19th July 2011 Harvard University Dr Elena D’Onghia [email protected] 46 Notes Abstract We employ numerical simulations andinner simple regions analytical estimates of to the arguestar Galaxy that clusters. can dark We be matter carry substructures efficiently outallowing orbiting destroyed a in us set by the of to disk fiducial examine shocking, high-resolutionsatellites the collisionless a in simulations impact dynamical high-resolution in of process Aquarius which the simulations we knownOur adiabatically disk and to calculations grow analytically on indicate affect a estimate that the globular disk, the the substructuremass presence cumulative function abundance. of halo of substructures a and in disk We disk-shocking the with innercalls also effect. only parts into track of 10% question halos. whether the of these This the orbits suggests substructures total that can of Milky there produce dark is Way transient no matter features mass inner in can missing disks, satellite significantly like problem alter multi-armed and the spiral patterns. Substructure Depletion in the Milky Way Halo by the Disk Galaxy Formation, Durham, Tuesday, 19th July 2011 Leibniz-Institute for Astrophysics Potsdam (AIP) 47 [email protected] Prof Matthias Steinmetz Notes Abstract Large spectroscopic surveys of theproperties Milky of Way the allow Milky us Way. to Themillion take Radial Milky Velocity Way a stars. Experiment systematic RAVE Beside view has radial at velocities, meanwhileof stellar the spectroscopically the parameters observed combined and RAVE about chemical abundance stars. half rations and a could dynamical Amonglocal be resonances derived many for and possibilities, the the majority general RAVE velocity thus andresults provides abundance investigating distribution means these of to phenomena the extended study and the trends the solar with remnants suburb. RAVE of I data. will past describe accretion recent events, The Chemodynamical Disection of the Galactic Thin and Thick Disks with RAVE Galaxy Formation, Durham, Tuesday, 19th July 2011 Harvard University 6 Gyr) orbit about the Milky > Ms Gurtina Besla [email protected] 48 2 Gyr). Without a short period orbit about the MW, gravitational interactions between the Clouds and the ∼ Notes Way (MW). This differs markedly fromMW the (period canonical of picture in whichMW the can Clouds no travel longer on be a considered quasi-periodicpropose as orbit that the tidal about interactions main the between driver the for LMChistories the and and morphological SMC kinematic are evolution sufficient properties of to of the explain the Magellanicfurthermore the discuss Clouds, System. observed the morphology, without Instead, broader star relying we implications formation on of athe this previous star dwarf-dwarf pericentric formation tidal histories interaction passage and scenario about to evolution the our of MW. general dwarf We understanding galaxies will of in our local volume. Abstract Recent high precision proper motions from the(LMC Hubble and Space SMC, Telescope respectively) suggest are that either the Large on and their Small first Magellanic passage Clouds or on an eccentric long period ( Kinematics of the Magellanic Clouds The Implications of a First Infall Scenario on the Star Formation Histories and Galaxy Formation, Durham, Tuesday, 19th July 2011 Peking University [email protected] Dr Sakurako Okamoto 49 ratio. The number of Galactic satellites is doubled in recent years thanks to systematic surveys in L / M Notes Abstract There are many dwarf galaxies aroundsimple, the with the Milky high Way, most of them are considered to be both dynamically and chemically The Stellar Populations of Ultra Faint Dwarf Galaxies the SDSS data archive. These newlywell-known discovered ”classical” ultra dSphs, having faint amorphous dwarf morphology (UFD) and too galaxiesplate. low are surface roughly brightness to Because 10 be to of found 100 by their the timesformation photographic fainter faint history than luminosities the (SFH) and and apparently detaileddiagrams large structural (CMDs) sizes properties of in are Galactic the still dSphs, sky, unclear.enough including the to six Here, derive general UFD the we natures galaxies. stellar present of ages Thestars the UFDs, based images in deep on such taken each colour-magnitude the as by galaxy. main star Subaru/Suprime-Cam sequencedSphs, The are turn-off, the brighter sensitive and younger wide galaxies populations enough have are to relatively moreformation study younger spatially the in concentrated populations spatial the to than distribution central the of these galaxy regionblue of center continued HB fainter than stars. at ones. old On least stars, the In a indicating otherGalactic the few that hands, globular the brighter Gyr, the cluster. star CMDs consistent of This with the result the faintestthose indicates satellites of different that show brighter spatial the a dSphs distributions at single gas an epoch in of occurrenceto of the red of belong star progenitors their and formation to of initial as the star UFDs a less formation. were metal-poor massive This removed halos is more than reasonable those effectively if of than the brighter UFD dSphs. progenitors were likely Galaxy Formation, Durham, Tuesday, 19th July 2011 MPIA, Heidelberg Dr Nicolas Martin [email protected] 50 Notes Abstract Recent discoveries of faint dwarf galaxies around bothsystems the that Milky are Way and 100 Andromeda to have 1,000 expandedized the times our realm fainter view of than of galaxies known the to Andromeda only satellite 10I system. years will Based ago. present on the In both detailed particular, the properties panoramic the survey ofthey PAndAS data, individual, relate survey and faint to has deep Andromeda their revolution- photometric satellite environment follow-up, galaxies, (luminosity asof function, well the sizes, as Andromeda 3D their galaxy. distribution, global etc) properties, and how can help us understand the formation and what they can tell us about their host Insights on the Andromeda Satellite System: A deep view of the faintest of galaxies Galaxy Formation, Durham, Tuesday, 19th July 2011 IoA, University of Cambridge Dr Jorge Penarrubia [email protected] 51 Notes Abstract Dwarf spheroidal galaxies (dSphs) are therole smallest in and faintest constraining galaxies galaxy in formation theof models known dark within Universe, a and matter as cosmological enclosed such context.of they within play individual Several the a stars. authors key luminous have Unfortunately, radius shown thehindered that of thus strong the a far degeneracy amount any dSph that meaningful exists can derivationshow between be of that dynamical how strongly for mass dark constrained and dSphs matter velocity by that isallowing anisotropy us spatially contain modelling to has distributed spatially/kinematic the measure in for distinct kinematics these the stellar first galaxies.Early time components results In the found this density this for profile talk degeneracy of the I dark can Fornax will matter and be haloes Sculptor on broken, dwarf galactic thereby spheroidals scales will of a be few shown hundred and parsecs. discussed. Measuring the Distribution of Dark Matter in Dwarf Spheroidal Galaxies Galaxy Formation, Durham, Tuesday, 19th July 2011 Royal Military College of Canada . If cuspy halos are not present, the observations 8 σ 52 Dr Rachel Kuzio de Naray [email protected] will provide useful constraints onkinematic theory/simulations and of baryonic photometric physics data (e.g.halos for than feedback). LSB the galaxies A predicted shows growing triaxialstar body that formation cuspy of they to CDM high-quality are remove halos. baryons moreconfront and consistent Sophisticated the low feedback low with angular scenario mass momentum spherical with gas the galaxy coredLSB star to simulations galaxies dark formation change to have histories matter an determine and used initially the merging feedback cuspy applicability histories of halo from of these seemingly into models. undisturbed, a quiescent cored halo. We Notes Abstract Dark matter-dominated galaxies like low surfaceCDM model brightness on (LSB) galaxy galaxies scales. provide If powerfulhalo LSBs tests concentrations are of and found the to on predictions reside the of in values the cuspy NFW-like of CDM cosmic halos, parameters constraints such can be as placed on CDM LSB Galaxies and their Dark Matter Halos Galaxy Formation, Durham, Tuesday, 19th July 2011 Kapteyn Astronomical Institute, University of Groningen 53 Prof Marc Verheijen [email protected] cm line of atomic hydrogen provide a unique perspective as they reveal environment-dependent physi- 21 Notes Abstract The processes of accretion and depletionobservations of in the gas in galaxies playscal an processes important like minor role mergers, in ram-pressure their strippingnumerical formation and tidal simulations and interactions evolution. have that remain now Radio unnoticed reached otherwise.vations a Moreover, at level of the sophistication scales thatopportunities of allows for galaxies. large for scale meaningful HI I comparisons surveys with will with the SKA present pathfinders obser- a like ASKAP, brief MeerKAT overview and Apertif of on the the WSRT. current state of HI affairs and discuss the future Gas in Galaxies - an HI perspective Galaxy Formation, Durham, Tuesday, 19th July 2011 MPA Garching Dr Barbara Catinella [email protected] ), covered by both SDSS spectroscopic and GALEX imaging 05 54 . 0 < z < 025 . 0 ) and redshift ( ⊙ M 10 10 > ∗ M Notes Abstract The main obstacle to understanding the formation and evolutionIn of particular galaxies we is still our lack limited knowledge measurements of of thesamples the role for HI played which gas, by ancillary gas. which data is on stellar the and reservoir starGALEX for formation Arecibo future properties SDSS star are Survey formation, also (GASS), available. for an large To ambitious and thisin programme unbiased end to massive we assemble are galaxies. the carrying out first Using the unbiased the inventorystellar of Arecibo atomic mass radio hydrogen ( telescope, we are acquiring HI spectra for 1000 galaxies selected uniquely by Cold Gas in Massive Galaxies: Results from the GALEX Arecibo SDSS Survey surveys. Our selected stellar massstar-forming range to allows red us and to passively probetheir evolving. the structural interesting and In region star this where formation talkthe galaxies properties. I transition average I will from gas will discuss blue properties argue how and that oftransitioning the gas between the gas scaling blue, local content relations star-forming galaxy of cloud are and population, massive notfor red only systems but systems sequence. necessary depends that are In to might on also particular, characterize have objects a recentlynature with very of accreted HI the gas useful excess GASS from are tool sample, the good I to candidates surroundinginvolve will identify medium. morphological illustrate objects pruning, a Lastly, and relation that taking between thus might advantage baryonic is of mass be more the and suited velocity unbiased to for comparison massive with systems theoretical that models. does not Galaxy Formation, Durham, Tuesday, 19th July 2011 MPE 6 with ∼ ). The sample is purely mass Dr Amelie Saintonge [email protected] 0 . 10 > ⊙ M / ∗ M and 2 star-forming and sub-millimeter galaxies. The position 55 = 1 z Notes selected, and therefore provides an unbiasedand view molecular gas of phases. the In distribution these offrom massive condensed galaxies, the baryons while between atomic MH2 the is gas a stellar,of constant mass. atomic fraction galaxies, gas of stellar Contrary we mass, to find it ismost the that mostly global scenario the decoupled galaxy established molecular properties by gas (stellarcorrelation and resolved depletion is dynamical in CO timescale the masses, maps is depletion concentration time-specific of not index, starstar-forming formation mass a universal, rate galaxies surface plane, significantly but and where density,...). extreme smaller a rather cohesive ULIRGs, The number varies picture as strongest of emerges, by well a linking local as galaxy a normal in factor this of plane is determined solely by its gas fraction and the importance of dynamical effects affecting it. Abstract We are conducting COLD GASS, a legacylink survey between for atomic molecular gas gas, in molecular massive gas,30m galaxies. star telescope, The formation survey’s we aim and is measure global to the galaxy understand properties the CO(1-0) in line the in local 350 universe. massive Using galaxies the (log IRAM The non-universality of the Molecular Gas Depletion Timescale in Massive Galaxies Galaxy Formation, Durham, Tuesday, 19th July 2011 CDM Λ m-selected µ . We show that the McGill University 5 . 0 ± 2 ) luminosities imply that ∼ 0 ) z → –2. We reveal evidence that the 5 . (1 + ) emission from a 24 = 1 1 0 ∝ Dr Jim Geach [email protected] J ∼ → z gas f = 1 . The CO ( , with J 2 2 ∼ 20% of the baryonic mass, but have star-formation ∼ ∼ z z gas-dominated disks at 56 . We have used the new gas mass estimates to piece together the z and . These relatively ’normal’ star forming galaxies bridge the gap between local ’quiescent’ 4 . = 0 z latest predictions for the evolution of the molecular gas fraction in semi-analytic models of galaxy formation within a the disks still contain a large’efficiencies’ similar reservoir to of the molecular local gas gas, poor contributing quiescent disks Universe are supported by thesedepletion new in data, galaxies and over cosmic discuss time. how the observations fit into our overall picture of gas accretion / Notes sample of galaxies at star forming discs and moreevolution active of disc the galaxies molecular at gas high- fraction of star-forming galaxies since average molecular gas fraction has undergone strong evolution since Abstract We present new IRAM Plateau de Bure interferometric detections of CO ( The evolution of the molecular gas fraction of star-forming galaxies Galaxy Formation, Durham, Tuesday, 19th July 2011 Durham University [email protected] Miss Claudia Lagos . We also find that the ratio H2/HI is strongly 2 ∼ z 57 systems, and is always dominated by the HI content of low and intermediate α dependent on stellar and cold gasobserved mass, evolution and inferred from also damped-Ly on redshift.mass halos. The predicted We predict cosmic that density the star evolutiongalaxies, formation of rate in vs. HI agreement agrees stellar with mass with local plane the should observations,law. have and two sequences show of that ”active” the and ”passive” evolution of this plane offers a means to constrain the SF Notes Abstract We investigate the star formationmolecular and hydrogen the components, gas using content theratio of galaxy of galaxies formation molecular by model to GALFORM splitting atomic in theon hydrogen, the the interstellar H2/HI, CDM H2 medium in content. framework. into each We galaxy its WeH2/HI are self-consistently atomic calculate and able and and the to stellar calculate predict and the the cold star HI gasand formation high mass mass, redshift rate function, and observations. based the the We CO(1-0) far-infrared-CO also luminosity predict luminosityby the function, radically relation, HI different the and which evolution: correlations H2 are for mass between HI functions in the up goodfor number to density agreement z=8 H2 of and with the massive find objects local maximum that decreases these number slowly are with density characterised increasing of redshift, while massive objects is reached at Cosmic evolution of star formation and the gas content of galaxies Galaxy Formation, Durham, Tuesday, 19th July 2011 European Southern Observatory [email protected] Dr Luca Cortese 58 Notes Abstract Even though it has been known forwe decades still that the miss properties a of coherent galaxiesone are picture tightly of about linked the the to main the role problems environment played has theygas, been inhabit, by stars, the the dust lack cluster and of environment information metals) onwide-area about taking galaxy the multi-wavelength part properties evolution. in surveys of the Until the are star different veryenvironment finally baryonic formation recently, on under components cycle the (e.g., way, of different constituents galaxies making of andUV, it galaxies. their SDSS-optical, possible variation In Arecibo-HI, to this with Herschel-FIR/submm) talk, investigate local Isample for density. separately will of the the combine Now, nearby Herschel new effects galaxies multiwavelength Reference in of datadensity different Survey, the (e.g., regions. environments, a GALEX- to volume-, I investigate will magnitude-limited howmoving explore the from how star the the formation field cold cycle to gas, the changes center from dust of high and Virgo to metal and low content discuss the and implications star of formation these activity results of for galaxy galaxies evolution vary models. when The role of the cluster environment on the star formation cycle of galaxies Galaxy Formation, Durham, Tuesday, 19th July 2011 : the famous 3 . 0 ∼ z University of Arizona Dr Tim Rawle [email protected] 59 ), Herschel photometry spans the peak of the dust component, 4 . 0 − 2 . 0 ∼ z merging system known as the Bulletmembers Cluster, and and characterize their a dust relatively component, undisturbed allowing us clustera to MS2137. function study of the We distribution morphology locate of and the star formation FIR-bright localgalaxies in cluster environment. with the dust two In component systems SEDs addition, as that we do investigateany not sources an conform to observed intriguing the at subpopulation templates higher of derived redshift. from FIR-luminous local field galaxies, yet are also unlike Notes allowing us to constrain therate. dust Although properties, a measure large fraction total ofHerschel, infrared galaxies the luminosity far-infrared in highlights and massive regions clusters hence of are derive activityof quiescent within obscured cluster early-types the galaxy star system. and evolution, therefore formation The exposing remain FIR starburst effectively undetectedof probes mechanisms by the the such as-yet transitional as un-quenched phases tidal in-fall interactions population. and Here mergers, we as focus well on as two the particular, remnants contrasting clusters at Abstract Nominally designed to locate high-redshiftSurvey” galaxies (HLS; magnified PI: by Egami) 44clusters. also massive provides foreground For deep clusters, sources 5-band, the at far-infrared “Herschel these (FIR) Lensing redshifts imaging ( of the galaxies contained within those Exploring Star Formation in Clusters with the Herschel Space Observatory Galaxy Formation, Durham, Tuesday, 19th July 2011 Texas A&M University ) and 2) the astoundingly 1 < z < 0 ). Prof Kim-Vy Tran [email protected] 62 . = 1 z 60 high star formation rates and reversal ofgalaxy the clusters star-formation known density at relation a discovered in look-back the time core of of nearly one 10 of billion the years most distant ( Notes Abstract Understanding how galaxies form and evolve inhistories clusters continues of to galaxies be in a key rich question clustersformation in constrains in astronomy. cluster both The galaxies stellar ages simply and population accelerated assembly relative modelsassemble to and their their hierarchical counterparts stars formation in in the scenarios. a lower Is density fundamentallymembers field, star different and or manner? active do galactic cluster To nuclei galaxies answer from this our Spitzer/MIPS question, Infra-Red I Cluster summarize Survey results at on ( 1) star-forming Star Formation in Galaxy Clusters Over the Past 10 Billion Years Galaxy Formation, Durham, Tuesday, 19th July 2011 . Using STScI 62 . = 1 z are not entirely con- 62 . 1 z < = 1 Dr Jennifer Lotz [email protected] z 61 . However, the observations of massive cluster galaxies at 2 z > in over-dense regions – i.e. at the time and place of intense star-formation and merger activity. 5 . 1 z > . Half of these mergers are dissipationless, as indicated by their red rest-frame optical colors and low 24 6 . 1 ∼ z Notes sistent with this picture. Themassive best galaxies way at to disentangle the mergerWe and present star-formation the recent histories merger is history to of study massive the galaxies progenitors in of a spectroscopically-confirmed proto-cluster at Abstract The assembly of the most massivechical galaxies galaxy in the formation universe models is invoke a lateformed classic assembly the problem times bulk for for of galaxy very their formation massive stars models. galaxies at Current via hierar- the merger of smaller galaxies that Caught in the Act - The Assembly of Massive Cluster Galaxies at HST WFC3 near-infrared imaging from the Cosmicwe Assembly find Near-infrared that Deep the Extragalactic merger Legacy Survey rategalaxies (CANDELS), of at the massive proto-cluster galaxiesmicron is and 5-10 UV times emission. higher than We the discuss merger the rate implications of for massive massive galaxy field assembly in proto-cluster environments. 62 Oral Programme Abstracts Wednesday, 20th July 2011

63 Galaxy Formation, Durham, Wednesday, 20th July 2011 . 10 z < ETH Zurich form from direct collapse of ⊙ M 5 Prof Lucio Mayer [email protected] 10 > yr) at the center of gas-rich major mergers at 6 10 < 64 supermassive gas clouds assembled on very short timescales ( Notes Abstract The formation of realistic galaxiestrophysics for in nearly the two Cold decades. Darkstar A Matter formation combination and model of feedback has increased processes been resolutioneither has in a SPH allowed simulations or major to AMR and open grid produce improved based problem disk sub-gridlations codes, of recipes galaxies were alleviating still of with cosmology the suffering realistic angular and from momentum sizes as- other ”catastrophe”.in in issues, However, bulge-to-disk notably the until ratios an past now excesse much few all of higher years, these lowinconsistent than simu- with angular with those momentum several of material observational typical in constraints. the spirals, center, and resulting anIn excesse this stellar mass talk rendering I simulated willactual galaxies star show forming how gas a phase majorresolution in to step the resolve forward at ISM, least is namely the made molecularformation giant molecular becomes clouds. once complexes. more stars This In clustered are this and can new formed supernovaesurrounding be regime explosions gas, at achieved an driving become inhomegenous densities with spontaneously an ISM sufficient comparable outflows naturally order hydrodynamical arises, without to ofstructural star ad magnitude properties, those hoc more from of momentum efficent low the deposition. in mass heating Asto dwarfs the a the the result, size Milky galaxies of Way, with the can realistic In LMC be with addition, finally slowly these rising produced galaxies rotation within doshows curves the not to remarkable CDM suffer late-type agreement. model, spirals from without akin an Iellipticals fine and excesse will tuning SO stellar galaxies also of in mass. the parameters discuss same framework in pastblack Comparisons and conclude sub-grid holes and with with outlining recipes. in new galaxies a new massive in preliminary model galaxies. for the results the formation THINGS concerning In of supermassive survey the the latter formation model of black massive hole seeds with masses SPH simulations of the formation of individual galaxies Galaxy Formation, Durham, Wednesday, 20th July 2011 Max Planck Institute for Extraterrestrial Physics ) 3 - 65 = 2 z Prof Dr Reinhard Genzel [email protected] Notes The middle ages of galaxy evolution ( Galaxy Formation, Durham, Wednesday, 20th July 2011 Max-Planck-Inst. fuer extraterrestrische Physik 66 Dr Linda Tacconi [email protected] Notes Atomic and molecular gas in galaxies Galaxy Formation, Durham, Wednesday, 20th July 2011 relative 8 σ and m Ω Ohio State University [email protected] Prof David Weinberg gap between the minimum halo mass required to 20 − 10 67 ∼ halos are similar in high density environments and in large scale voids. HOD models naturally explain ⊙ over a wide range of redshift, (b) that the observed luminosity dependence of galaxy clustering is driven M ⊙ 12 M 10 12 − 10 11 ∼ 10 Notes observed features of the galaxy correlation function, pairwiseallow velocity dispersion, new and cosmological void tests probability distribution. by providing Theyover also a when flexible model fitting of observations. non-linear galaxy These bias approaches whose provided parameters early can evidence be for marginalized a downward revision of host a central galaxy andof the halo mass needed to host a satellite of the same luminosity, and (f) that the central galaxies to WMAP1 values, and they areaccurate now modeling enabling precise of new redshift-space constraints distortions onhalo these occupations. and parameters. galaxy-galaxy Environmental Frontiers dependence lensing of is and thea a subject probing source source include of the of potentially systematic environmental powerful uncertainty dependence insights for into of cosmological galaxy analyses, formation but physics. it is also Abstract Twenty-first century galaxy surveys inspiredfunctions an and array clustering of new of interpretiveThe galaxies methods key to that assumption the connect of theoretically the these(conditional observed predicted luminosity modeling distribution function), population techniques and of SHAM — (subhalo dark commonlymatter abundance halo matter acronymed matching) depends — on as halos is its HOD in mass that but the (haloto which has average emerge no occupation they galaxy from direct distribution), applying content knowledge reside. these of of CLF methods the a to halo’s dark M observations larger are: scale environment. (a) that Some galaxies of form the withprimarily key maximum insights by efficiency the in halos increase of of mass primarily central by galaxy the luminosity large with fraction halo ofhas mass, red large (c) galaxies that that scatter are the at satellites color the in dependence massive high of halos, clustering end, (d) is that (e) driven the that luminosity-halo there mass relation is a factor Connecting Galaxies to Dark Matter Halos: HOD, CLF, SHAM, and All That Galaxy Formation, Durham, Wednesday, 20th July 2011 University of Waterloo Prof Brian McNamara [email protected] 68 solar masses. No known population of galaxies exists in clusters that could have donated molecular gas at these 10 10 0.5 Gyr, directly linking cooling atmospheres to star formation. Furthermore, the molecular gas masses in many BCGs Notes Abstract Recent X-ray and radio observationsbeing have quenched shown by that mechanical heating cooling by hotwas outflows atmospheres associated discovered with in when nuclear clusters radio high and jets. giantatmospheres resolution This of elliptical so-called X-ray dozens galaxies “radio observations of mode” are galaxy feedback revealed clusters.emission giant While emanating cavities from largely the devoid in nuclei of of the thermal BCGs.required gas, central The the to cooling mechanical cavities inflate power regions are released them filled by of radio with againstradio the AGN, radio the synchrotron estimated synchrotron hot through surrounding power. the atmospheric pV work This pressure,through is is a enough generally finely-tuned power feedback a loop. to fewcluster suppress hundred galaxies. I radiative times will I will cooling present larger show evidence and than that∼ from to the star the formation regulate far is star triggered UV formation, when toexceed the apparently the central far cooling time IR of for the starlevels. hot formation atmosphere I in falls will below brightest discuss thefrom evidence the favouring hot and atmosphere, against and fuelling I will AGNshowing briefly though AGN touch cold outflows on molecular dispersing the accretion metal-enriched role of and gas black Bondi throughout hole the accretion spin ICM. in powering AGN. I will present new evidence Supermassive black holes and mechanical feedback Galaxy Formation, Durham, Wednesday, 20th July 2011 Kavli Institute for Cosmology, Cambridge 69 [email protected] Dr Ian McCarthy Notes Abstract Traditionally, studies of galaxy formationfraction of have the focused baryonic mass on of the normalthat and observable massive regulate galaxies stellar is the properties believed to formation of beformation of galaxies. in a necessarily stars hot However, diffuse incorporates do form a both and so large many thephases by of the interact. stars influencing processes At and the present, the properties galaxy hot groupsmeasure of and the gas this clusters properties and hot represent of an the both gas. only the understandingto systems stellar of a Thus, in and significant the the gaseous a fraction universe baryonic processes of complete for (i.e., by the which the view halo which it intragroup/intracluster of viral is medium) these In radius. galaxy possible components this to out talk I willthermodynamic review and what chemical has properties been (and ofand potentially the distribution can intracluster of be) the medium. hot learnt gas In about asmassive particular, galaxy a galaxies I formation function at of will from the system discuss detailed mass present-day studies what tellsgas and of us the can in about the overall tell the the us content efficiency past. about of feedback feedback I and processes will the in also efficiency normal and discuss of environmental what processes the such metallicity as and tidal abundance stripping patterns and strangulation. of the The intracluster/intragroup medium Galaxy Formation, Durham, Wednesday, 20th July 2011 Australian Astronomical Observatory 70 Prof Matthew Colless [email protected] Notes Abstract The Fundamental Plane relates dynamical and structurallicity properties cause of scatter early-type galaxies, about but the differencesearly-type plane. in galaxies age However and form metal- such and stellar evolve.Galaxy population Survey, variation and We also for obtained reveal 7,000 information theLick of about Fundamental index these the analysis. Plane galaxies way for We we that then a alsovelocity measured derived sample dispersion, the age, of and trends metallicity 10,000 of also and these galaxies withfind alpha-element stellar stellar from the over-abundance population population the principal from trends parameters not components a 6dF with just of size, withradius surface the velocity and dispersion surface brightness Fundamental brightness. and and Plane. the The residuals most about remarkable Inand the finding across contrast is Fundamental the that, Plane, plane, to although but they the previous also show stellar with no work, populationsity. variation parameters we A at vary all galaxy’s through along position the along long thisdensity axis axis of more is the likely closely plane, to related roughly have to corresponding its undergone to merger major luminosity history, den- mergers. with early-type galaxies with lower luminosity Structure, dynamics and stellar populations in early-type galaxies Galaxy Formation, Durham, Wednesday, 20th July 2011 ESO Prof Eric Emsellem [email protected] 71 Notes Abstract We provide a census oflimited the Atlas3D apparent sample, stellar thus angular revealingvast momentum the majority of (86%) distributions all of and ETGs 260 properties are early-typeRotators of Fast only galaxies Rotators the represent (ETGs) with Fast about regular within 14% and rotation, of the Slow and theseDistinct volume- spread ETGs, Rotators. Cores. over are In a rather We round large this show (E4 range context, or thatassociated of we rounder) flattening, the with probe with while various most these Slow of parameters. two them including having familiespropose the Kinematically of a mass galaxies. trend revision within of We thethen the red further find sequence tuning-fork show that of how such diagram galaxies a the to classificationmagnitude E better leads in and to represent surface S0 a density. the log-linear classification We clean large mayshaping discuss morphology-density variation of be the relation galactic in impact holding misleading. systems. of for bulge such nearly We sizes four results of orders on of our fast understanding rotators. of the processes We involved in the The stellar angular momentum of nearby early-type galaxies: a paradigm shift Galaxy Formation, Durham, Wednesday, 20th July 2011 University of Oxford Dr Michele Cappellari [email protected] 72 Notes Abstract Galaxies satisfy tight scaling relations (e.g.global observables Faber-Jackson, like Tully-Fisher, luminosity, Kormendy size relation,to Fundamental and models Plane) kinematics. of between galaxy The formation, physical has interpretationobserved for of long or the been (ii) complicated relations, the by and samples the theircomplications, are fact comparison too that by (i) small deriving either and masses only biased luminosities forthe for and the statistical not consequences studies. masses volume-limited of are Atlas3D Here our sample weformation findings illustrate of models. for the 260 power the nearby of interpretation early-type removing of galaxies. both local We and discuss high-redshift galaxy scaling relations and for galaxy A new look at galaxy scaling relations Galaxy Formation, Durham, Wednesday, 20th July 2011 substructures are 4 10 73 Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology Dr Simona Vegetti [email protected] Notes Abstract The cold dark matter (CDM) paradigm predicts that atowards significant number lower of substructures, masses, with a populates steeply rising the mass function dark halo of galaxies. In the Milky Way, however, of order Quantifying mass substructure in early-type galaxies predicted inside the virial radius, whereas onlyparadigm. few New tens and have independent been so methods far are,Local observed. therefore, Universe required This and to poses beyond. a assess One major the such challenge level methoda to of will novel the mass be method, CDM discussed substructure based in in this on galaxies talk, strong inbeyond which gravitational the consists the lensing, of local to three Universe parts. uniquely and address First,that in I this will uses massive problem, discuss allowing all early-type us galaxies. the to information Ito probe contained will substructure detect in briefly and the present precisely surface aSecond, quantify brightness fully I Bayesian distribution mass will adaptive-grid of discuss substructure how method, highly in to magnified combine,to single in Einstein constrain a lens rings the statistical galaxies, substructure sense, and mass the even arcs, fraction detectionsof of in and mass mass the case substructures slope substructure from of of in multiple the very lens the mass galaxies galaxy high sample function. formation of mass-to-light Third, models. SLACS I ratios. If lenses, will time present as is new well left, results a I on will several the discuss level other possible systems, future and applications discuss of possible the method. implications for Galaxy Formation, Durham, Wednesday, 20th July 2011 MPA [email protected] Dr Laura V Sales galaxies. We find that the existance of extended = 0 z 74 is naturally reproduced in the LCDM, albeit not the norm. The representative 2 − 3 ∼ and characterize the morphological changes undergone by these extreme objects. z 2 ∼ z Notes disks galaxies as early as redshift volumes simulated in GIMIC provideearly then an disks avenue in to the trackextended Local down disk the Universe. population properties at of Our the results present day suggest descendants that of low such to moderate mass groups are the current habitat of the Abstract Understanding the origin of galaxythe morphologies main is morphological one components of (disks,observation, it the spheroids) has become leading of apparent challenges over galaxies the ofindividual seem past galaxies decade galaxy to evolves that continuously. formation the be We available studies. use present data the point suite atassembly to of Although of a all high disks scenario resolution redshifts at hydrodynamical where simulations high the surveyed GIMIC morphology redshifts to of so and study the their far posterior by evolution onto The rise and fall of disks in cosmological simulations Galaxy Formation, Durham, Wednesday, 20th July 2011 National Research Council, Canada Dr Lauren MacArthur [email protected] 75 Notes Abstract I discuss current notions of spiral galaxyof formation galaxy based bulges on and disks. detailed studies Current of studiesformation, the show thus stellar that the populations representative SPs (SPs) SPs of and must spiral kinematics galaxies involveSpiral are average not bulges SP well follow matched values the by integrated single same over episodesas correlations of the star those of star of formation increasing elliptical history light-weighted of galaxies. ageBulge the and formation In galaxy. metallicity appears a to with mass-weighted be central dominated context, by velocityin bulges early dispersion processes are disks that predominantly or are composed common not. to of allgradients While old spheroids, in whether monolithic and most they collapse metal-rich bulges. currently SPs. cannot reside Further bulge beminimally growth ruled via to out secular the processes, in or stellar some “rejuvenated”high-quality cases, star mass formation, merging optical budget. generally must spectra contributes be of I invoked integrated alsodetermine to the SPs demonstrate explain reliability along how of the with the the SP inferred optical-NIR combination SFHs. imaging of can full single population out synthesis model modeling weaknesses of and help Formation based on Detailed Spectroscopic Studies Galaxy Formation, Durham, Wednesday, 20th July 2011 ), based on Keck DEIMOS 3 . 1 University of Oxford/Caltech < z < -band magnitude Tully-Fisher relation 2 . B 0 Ms Sarah Miller [email protected] 76 90% of our sample, and we model the HST resolved bulge and disk components of each galaxy in order ∼ 3 . 1 ∼ consistent with a decline in diskthe luminosity likely of contributions at of fixed baryons velocity andevolution. dark over matter the When within same accounting various redshift for disk interval. the radiitrend We within resolved to our use gain bulge sample our a and and data better the disk to understanding likely componentsassembly driving of evaluate history of force the behind of each observed our disk galaxy, tightly galaxies. constrained we evolution observe of a the Tully-Fisher striking relation maturation and Notes spectra, multi-color HST ACS imaging,tended and spectroscopic ground-based integration Ks-band times, which photometry. hasvelocities led A for to unique each significant galaxy feature improvements and of in athey our determining rigorous flatten survey characteristic appraisal for is rotational of their the accuracy. ex- to Rotation de-project curves measured are velocities reliably while traced accountingstrate to for the the emission merit radius asymmetry, of where seeing, these advances dispersionprevious by and recovering studies slit an at effects. intrinsic intermediate We scatter redshift, on demon- comparablewe the to Tully-Fisher show that relations of evidence of locally for a determined modest factor relations.hydrodynamical 2 evolution With - and in this 3 the semi-analytic less increased stellar than precision, predictions. in mass Tully-Fisher Greater relation evolution at is a seen growth in rate the in agreement with recent Abstract We present new measures of the evolving scalingmass relations between estimates stellar for mass, rotational a velocity, morphologically magnitude, and inclusive baryonic sample of 129 disk-like galaxies ( z The Assembly History of Disk Galaxies: Evolution in the Tully-Fisher Relation to Galaxy Formation, Durham, Wednesday, 20th July 2011 ) is flat in projection. 1/3 Max Planck Institute for Astronomy are generally much smaller and denser 2 ∼ z are Disk Dominated 2 ∼ z 77 Dr Arjen van der Wel [email protected] Notes Abstract Over the past few years, it has become clear that massive, quiescent galaxies at The Majority of Compact Massive Galaxies at than they are today.dominated. Based This result on is foremost HST/WFC3 based on imagingViewing the simple angle we observation statistics that immediately now a imply significant that present fraction it (about is strongdimensional likely surface-brightness evidence that fits. the that majority The is such immediate disk-like, which implicationto galaxies is settle is further are into that corroborated mostly a by the two- disk. majority disk- of Theseit stars dense, is disk-like formed likely systems from that are gas all the that massive progenitorsrelatively had galaxies, of gas-poor time including massive, merging, their bulge-dominated can present-day galaxies destroy bulges, today. thinmass. first Hence, disks form and as cause disks. the Subsequent galaxies evolution, to driven gradually by grow in size and, to lesser extent, in 78 Oral Programme Abstracts Thursday, 21st July 2011

79 Galaxy Formation, Durham, Thursday, 21st July 2011 UC Santa Barbara with outflows (and inflows) of 5 . 1 250 galaxies. Analysis of the interstellar ∼ < z < [email protected] Prof Crystal Martin 6 . 0 80 Galaxies 5 . 1 z < absorption lines quantifies the fractionlow-ionization of gas. galaxies And over we the discussthe redshift the prevalence range correlation of of both outflow scattered speed emissionthat and and give fluorescent strength rise emission with to from galaxy these it. properties.that galaxies could If and We enable discuss time also large the permits, describe surveys physical I for conditions will outflows also across much discuss of nebular cosmic emission-line time diagnostics withNotes of JWST. galactic outflows – a technique Abstract Using new, deep spectra, we measure the near-ultraviolet spectral features of of Gas Outflow and Inflow in Galaxy Formation, Durham, Thursday, 21st July 2011 1 co- ∼ Caltech . At present, there exist 2 z > Prof Charles Steidel [email protected] 81 2–3)) is a crucial, but poorly understood, aspect of the galaxy formation process. ∼ z 300 physical kpc at ∼ Notes Abstract During the peak epoch offormation, galaxy as formation, well the as intergalactic the mediumgalaxies. is waste both dump The the for exchange source the of of products baryons gas of between responsible star forming for formation galaxies fueling and and star black their hole ”Circum-Galactic accretion Medium” that (regions are within not retained by Gas-phase Outflows and Accretion During the Peak Epoch of Galaxy Formation moving Mpc ( By applying a combination ofthe more faint traditional galaxy QSO surveys sightlines) andpresent to an absorption the overview line same of studies survey recent (usingin- observations volumes, and background and a -out) their galaxies picture on implications in of forming for addition galaxies thepuzzling understanding and galaxy/IGM to discrepancies the and system between influence on is observations of the emerging. baryonic and physicsunderstanding flows and of theoretical I chemistry (both the expectations will behavior of whose and the distribution resolution CGM/IGM of at may baryonic be material over key cosmic to time. advancing our Galaxy Formation, Durham, Thursday, 21st July 2011 UCO/Lick Observatory [email protected] Prof Xavier Prochaska 82 Notes Abstract I will review observations on the relationship between theon intergalactic low medium redshift. (IGM) and This galaxies, includes with new particular results emphasis (or from lack the Cosmic thereof) Origins of Spectrometer the on the galaxy-IGM HST. connection I with will also redshift. explore the evolution The IGM-galaxy connection Galaxy Formation, Durham, Thursday, 21st July 2011 University of Arizona Prof Rameel Davé [email protected] 83 Notes Abstract I will discuss observations andtime. theoretical Observations insights of into CIV the and chemical otherhave metal enrichment distributed absorption of at metals diffuse high over intergalactic redshifts a suggest gassmall, significant that early across strong galaxies volume cosmic and are of generally ubiquitous more the galactic successful outflows universecapable at of matching at providing observations. sufficient early IGM Outflows epochs. enrichment observed without in any redshifts Outflowslower contribution 2–4 from that redshifts galaxies very are is early eject non-standard characterized more sources. by material Evolution athat to from general star-forming migration galaxy of halos metals have backescape towards velocity, an galaxies. suggesting oxygen that New content “halo HST/COS exceedingsubstantial fountains” observations component that show are of of common infall the today. into star-forming galaxy’s Such galaxies ISM, reaccretion today. with of ejected velocities material below may the represent halo a The metal enrichment of the intergalactic medium Galaxy Formation, Durham, Thursday, 21st July 2011 Durham University –3, and from observations of = 0 z Dr Cedric Lacey [email protected] 84 –10. I will discuss how these new comparisons test our ideas about star = 3 z Notes Abstract A key goal of theoreticalrequires models models that, of as galaxy well formationfeedback as is etc, incorporating to can all also understand of be the themm, compared physics history directly radio). of of to dark star Since observational matter formation data each halohave on in star assembly, a different the formation gas theoretical star universe. tracer cooling, approach formation star offers tracers thatunified This formation, only (UV, allows approach, a optical, a which IR/sub- partial unified combines view comparison a andCDM with sophisticated has with all model important of a of uncertainties, these radiative galaxy it tracers.optical, transfer formation is IR, model I in essential sub-mm for will the to and the describe framework radiodetailed results emission wavelengths. of comparisons from from of structure I the such stars formation combined will a model and of focus with dust in far-IR data this in from talk galaxies, Herschel on at and redshifts what predicts we SEDs have learned spanning about UV, galaxy evolution from A unified model of galaxy evolution in the IR and UV Lyman-break galaxies in the rest-frame UV at formation and feedback, and whether they supportin the idea order of to a explain top-heavy the IMF observed in starbursts, sub-mm which galaxy was population. previously proposed Galaxy Formation, Durham, Thursday, 21st July 2011 ? 2 Leiden Observatory . Using large, cosmological simulations, I will = 2 [email protected] Ms Freeke van de Voort z 85 Notes discuss how this decline isWhen related gas to accretes the along evolution filaments of ofthe gas the central cosmic accretion web, galaxy and it to quickly is outflows (cold generallycooling driven time relatively mode). is by dense, long active cold, for More massive metal-poor, galactic diffuse haloes and nuclei (hot gasrate flowing mode). (AGN). onto towards shock By haloes. the heats present Star time, at formation the does the hotof not mode virial the track strongly hot dominates hot-mode radius the halo halo to global gas accretion, accretion the never northe does reaches virial it global the temperature track cold-mode central total galaxies. accretion and halo rate its The accretion, density drop becauseby onto in most preferentially haloes, the preventing but gas star that with formation entered a rate haloes delay. in followsin the a I the hot corresponding will mode absence decline from show of accreting in that AGN onto AGN their feedback, central feedbackand gas galaxies. plays the accreted Consequently, a drop in crucial off the role in hot the mode cosmic would star become formation the rate dominant would source be of much fuel less for steep. star formation Abstract The cosmic star formation rate is observed to drop sharply after redshift What’s causing the drop in the cosmic star formation rate below redshift Galaxy Formation, Durham, Thursday, 21st July 2011 University of Sussex Prof Peter Thomas [email protected] 86 Notes Abstract We present results from aand AGN. hydrodynamical Subgrid version physics of is the handledsimulation Millennium using to-date, the Simulation is latest with able version energy to ofR500, injection resolve with the the halos from L-Galaxies largest of semi-analytic supernovae clusters having model. virial inpopulation temperature excess This, in of 1 the 500,000 clusters, keV largest paricles. and SPH and the For the above entropybased first and with time, on metallicity at we jet profiles are least heating of able 15,000 to the is match X-ray gascool-core crucial both gas. and for particles the non-cool-core galactic A this within clusters, physical success. without model over-cooling With for of AGN the gas energy addition in injection of cluster radiative cores. cooling, we are able to reproduce both X-ray The Millennium Gas Simulation Galaxy Formation, Durham, Thursday, 21st July 2011 University of California, Irvine SPIRE catalogs of three independent wide- Herschel Dr Julie Wardlow [email protected] 87 gravitationally lensed infrared galaxies in 30 ∼ area HerMES fields. Thanks to the boostus from gravitational to lensing, perform these galaxies extensive have extremely follow-uphigh-resolution high observations. fluxes, submillimeter, which optical enables Our and suite near-infrared of imagingwe for follow-up present a a data significant thorough includes fraction investigation spectroscopic ofpopulations of CO-line the the of redshifts sample. observed high-redshift and and Using galaxies, intrinsic these particularlyinto properties data the intrinsically of physical bright the differences lensed submillimeter-selected of SMGs. the sources, populations. provides Comparisons with an other insight Notes Abstract We select a sample of A detailed study of infrared-luminous galaxies at high redshift Galaxy Formation, Durham, Thursday, 21st July 2011 (of 5 . 2 < z < 4 . 0 National Astronomical Observatory of Japan 88 and [OII] emission lines from our targets. These targets will be α Dr Tadayuki Kodama [email protected] ), and two general fields (GOODS-N and SXDF) with Suprime-Cam and MOIRCS and their 5 . 1 z > Notes which 8 are located at Abstract MAHALO-Subaru (MApping HAlpha and Linesvestigate of how Oxygen) the is an star on-going formingcores, Subaru activities cluster intensive in outskirts, programme galaxies groups, which and are aims the propagated to general as in- field). a We function are of targetingunique time, 13 sets clusters mass, of and and narrow-band proto-clusters filters environment at (many (cluster can of map them out are star custom-made forming for this galaxies particular with purpose). the The redshifted narrow-band H imaging MAHALO-Subaru: Mapping Star-Formation at the Peak Epoch of Galaxy Formation (have been) extensively followed-up by NIRsuch spectroscopy as with FMOS dust-corrected and star MOIRCS formation totargets rates, quantify for the AGN ALMA nature contribution as of and these well.results gaseous emitters obtained metallicities. In so this far. This presentation, The project I individual will studies will serve will give be excellent an presented introduction by of Hayashi, Koyama, this Tadaki, programme, and and I. some Tanaka. highlights of our Galaxy Formation, Durham, Thursday, 21st July 2011 Swinburne University Prof Karl Glazebrook [email protected] 89 Notes Abstract Observations of the high-redshift Universethat have suggested are a energised picture and of fedabout massive this by star-formation picture. in cosmic We gas-rich, have cold found turbulent flows. turbulentmodern disks disk Universe. galaxies However in Despite the recent SDSS their catalog, IFSNew turbulence a data Keck population they AO previously taken assisted kinematically thought observations at extinct resemble of in lower-redshift these disks, the in galaxies have and size have strengthening revealed fall raised they their on questions also similarity a contain with giantturbulence regular their star-forming is high-redshift Tully-Fisher clumps up counterparts. with relation. to Across star-formation 1-2 all kpc rate,formation redshifts and and the turbulent strongest not gas correlations disk of within stellar galaxiesof nor is the very gas gas suggestive masses. rather of than a Thewhether direct the detailed the feedback other turbulence mapping of way is star-formation of around. a driving the fundamental the More location driver kinematics detailed of of and disk star- higher formation SNR or a AO natural mapping consequence. at high-redshift is needed to see Turbulence and star-formation - chicken or egg? Galaxy Formation, Durham, Thursday, 21st July 2011 Max-Planck-Institut fur extraterrestrische Physik 90 2: Insights from resolved kinematics, morphologies, ∼ Dr Natascha M. Forster Schreiber [email protected] 2 galaxies are gained from studies of the spatially-resolved dynamics, star formation, and physical prop- 2. The survey is complemented with detailed rest-frame optical morphologies and resolved metallicities. I ∼ ∼ Notes Abstract Key insights on z erties from near-IR integral field spectroscopy,from with high-resolution instruments mapping such of as the SINFONI stellar at componentmechanisms of the driving galaxies, VLT. the this build-up Together provides of with a massive morphologies galaxies. powerful combination Imapping to will of study present Halpha recent in-situ results kinematics the from and ”SINS”, distribution the withpopulation largest survey SINFONI, at with for z full now 2D over 100 galaxieswill discuss probing the the implications massive of star-forming key results onspheroids some and of the disks, most including fundamental the open issues role concerning of the disk formation of instabilities massive and minor/major merger events in the formation of bulges. The growth of galaxies at z star formation, and metallicities. Galaxy Formation, Durham, Thursday, 21st July 2011 Yale Prof Pieter van Dokkum [email protected] 1-3 Universe with HST 1-3, what we can expect from 3D-HST, and show some = = z z 91 s of galaxies at high redshift. The talk will cover what we have recently 1000 -orbit HST Treasury program. The program uses the WFC3 grism, providing 2484 redshifts and stellar population diagnostics for Notes Abstract I will describe the 3D-HST survey, a 3D-HST: a large spectroscopic survey of the learned from ground- and space-based near-IR spectroscopy at first results from WFC3 spectroscopy and imaging of distant galaxies. Galaxy Formation, Durham, Thursday, 21st July 2011 3, 2.5; > < INAF z < Dr Giovanni Cresci [email protected] 3.3 have regular rotation, though highly turbulent, > 92 3. > 3, when the Universe was less than 15% of its current age. We report on our metallicity > 3 using near-IR spectroscopy with SINFONI at VLT and LUCIFER at LBT. We find that at z > 3 massive galaxies deviate from this relation, being more metal-poor. In some of these massive galaxies > Notes survey of galaxies at z low-mass galaxies obey the same fundamental relation between metallicity, mass and star formation rate as at 0 Abstract The metal content in galaxiesbut provides little important was known information for galaxies on at the z physical processes responsible for galaxy formation, AMAZE and LSD: Metallicity Evolution of Galaxies in the Early Universe however, at z we can even map the gasand inverted metallicity. abundance We gradients find relative that toregions local three galaxies, of galaxies with at star lower z formation. abundances nearchemical the evolution Overall centre, observed the close in to results galaxies the at suggest most z active that prominent inflow of pristine gas is responsible for the strong Galaxy Formation, Durham, Thursday, 21st July 2011 Caltech Ms Gwen Rudie [email protected] star-forming galaxies and their accompanying . Through the use of absorption systems, 3 . 7 2 . 2 ∼ ∼ > > z z 93 2 physical Mpc) of the line of sight to a background . The Lyman alpha forests in the QSO spectra have been ∼ Notes UV absorption seen in high-resolution spectra of 15 ultra-bright < Abstract We present the analysis of a unique spectroscopic survey of 732 < Mapping the circumgalactic medium of high-redshift galaxies we can determine the impact of star-formingthan galaxies on can their be local probed intergalactic with medium direct (IGM) observations.utes out to Our ( much rest-frame larger UV distances spectroscopic survey includescarefully galaxies analyzed within and a we few will soon arcmin- begin analysisredshift on of metallic lines the in foreground the same galaxy spectra. arearound Spectral examined forming regions to of galaxies measure the at forest the various near kinematics the transverseHI and distances. column systems We density increase find of rapidly that neutral with the hydrogenapproached. HI decreasing present These column galactocentric measurements, density impact combined and parameter with the an andrest-frame number optical upcoming of as properties NIR associated the of spectroscopic these systemic observing galaxies will velocity campaignnature allow to of for of characterize the the inflows, the first galaxy galactic glimpses outflows, of is the and co-evolution the of effect galaxies and of the star IGM, formation the on both the IGM and on the future of the galaxy itself. Galaxy Formation, Durham, Thursday, 21st July 2011 University of Cambridge Dr Martin Haehnelt [email protected] 94 Notes Abstract Deep spectroscopic and narrow-band observations suggest the presencealpha of emission spatially extended around low most surface brightness DLA/LLS Lyman- Lyman-alpha host emission galaxies. can be I used as will powerful discuss diagnostic how of the the kinematics spectral of shape the galactic and winds spatial in distribution DLA/LLS host of galaxies. this Lyman-alpha emission Probing galactic winds from DLA/LLS host galaxies with spatially extended Galaxy Formation, Durham, Thursday, 21st July 2011 recycled back onto a recycle Leiden Observatory recycled winds from re-accreting that could largely more gas from efficiently streaming onto galaxies. [email protected] Dr Benjamin Oppenheimer prevent 95 preventing far more gas out of a galaxy than forms into stars. Second, more energetic ejecting Galaxy Growth Feed grows galaxies is the greatest determinant of how the present-day galactic mass function appears. It also Notes winds can significantly heat their circum-galactic medium Abstract Galactic superwind outflows dochallenges many of things. enriching the intergalactic Cosmological medium while simulationsstars. solving I show the will over-cooling they talk problem about need where three toocan to central many severely ways be baryons that suppress form invoked outflows galaxy into determine growth to the by solve growth of the galaxies. dual First, highly mass-loaded outflows How Outflows provides a challenge as this efficientlikely channel in of the accretion form needs of AGNs, to but be I quenched will by suggest a other possibilities mass-dependent to feedback mechanism, Finally, outflow materials ejected abovegalaxy the providing escape a velocity significant of and a oftenwind halo dominant more accretion source often of than gas not for re-accrete subsequent or star formation. Surprisingly, how solve the problem. Galaxy Formation, Durham, Thursday, 21st July 2011 nebula using α UC Santa Barbara Nebulae α nebula system and use them α [email protected] Dr Moire Prescott nebulae. In this talk, I will present observations α emission. In the last few years, substantial progress α 96 emission in this system. In addition, using deep rest-frame UV/optical α nebulae offer a window into the dominant physical processes at work during the Ly α HeII nebula, we are finally able to probe the kinematics of a giant Ly + α powering emission extending out to 100 kpc, overdense environments, and a close association with strong submil- α Notes of the morphology, the energetics, and -to for test the models first time of - superwind theplay line outflows an polarization important and of role a cold in typical flows. the Ly discrepancies accretion between Despite of the gas the observed onto fact morphology, galaxies thatcold and energetics, flow these in and simulations. the two polarization Thus, distribution physical relative while of these phenomena to metalsbe processes what in are the are the is only thought likely universe, viable predicted going to mechanism we on, by for find photoionization outflowspectroscopy robust by and of AGN the or star first formation known appearsthe Ly to more robust optically thindensity, HeII-1640 and line metallicity) and within put the meaningful line-emitting constraints gas. on the physical conditions (ionization state, Abstract With powerful Ly limeter and mid-infrared sources, giant Ly Caught in the Cosmic Web: Testing Theoretical Models of Giant Ly episodes of massive galaxy formation andrelies provide a first direct and probe foremost of the onhas gas understanding been within what the made is cosmic towards web. powering building a Leveraging the this theoretical Ly potential framework for studying Ly Galaxy Formation, Durham, Thursday, 21st July 2011 Swinburne University Dr Rob Crain [email protected] 97 Notes Abstract I will discuss how developmentsbetween X-ray in data the and theoretical gasdynamical models modellingintepretation based of on of X-ray hierarchical observations galaxy cosmogonies. of formation ’normal’ This L* has havesame galaxies. motivated X-ray reconciled a I scaling show review a relations for of the perceived (Lx-Lk, the first Lx-Tx), standard conflict timeemission a that from result disc disc and galaxies that elliptical is is galaxies produced incompatible follow bystars. with the starburst the winds I and standard that present interpretation, from whereby a ellipticals diffuse is simplenamely assocated alternative, gas with accreted in mass from loss which from the the evolved IGM. hot gas associated with both morphological types has a common origin, Theoretical and observational insight into the hot side of galaxy formation. Galaxy Formation, Durham, Thursday, 21st July 2011 University of Hertfordshire Dr Marc Sarzi [email protected] 98 Notes Abstract For a galaxy, the abilityhistory. to sustain a An corona halo of ofmass hot, hot loss X-ray gas emitting material gas can is can indeed quicklyX-ray be be absorbed emission a by an and key the such effective element precise an shield determining amountconsidering hot its against of the medium. star-formation hot the rather gas external loose Since around correlation acquisition galaxies the have betweenthe of discovery limited been the ability of cold the optical to such gas separate matter and with of X-ray whereas X-ray earlier long X-ray halos, luminosityray stellar- data debates, binaries the of the in and contribution galaxies. origin the particular from X-ray an when of This emission active nucleus, from the situation the thealso resulted unresolved intra-cluster contributed population from medium, of to although X- the such use an of impasse. looselyfor defined the By optical 260 combining data may early-type the have galaxies homogeneously-derived of photometricX-ray the and measurements, Atlas3D we kinematic have integral-field measurements shown spectroscopic that survey the with abilityand to intrinsic both flattening retain low- of an a and halo galaxy. of high-spatial hot Specifically, resolution gas inby the depends the framework crucially of on SAURON the the survey, revised dynamical classification we structure for early-type foundthat galaxies are that: advanced entirely consistent 1) with Slow what Rotators expected ifkinetic have the temperature hot-gas hot gas of halos originates the with from stars stellar-mass X-ray loss through luminositythat material shocks and that always is and temperature heated fall collisions. values up at short 2) the Fast offlattening Rotators and such have degree a hot-gas of prediction, halos rotation with support. and X-ray the luminosities more so the lower their dynamical mass and the larger their intrinsic The origin of the X-ray halos of early-type galaxies Galaxy Formation, Durham, Thursday, 21st July 2011 . 6 ∼ Durham University z [email protected] Dr Nikolaos Fanidakis 99 Notes The model also reproduces remarkably well theis a radio natural loudness consequence of of AGN, the suggesting accretion thatfor rate the and the spin jet clustering characterising properties its of of central quasars an BH. activegalaxies. and Based galaxy on radio this galaxies model, and I make explore predictions the statistical properties of dark matter haloes that host active Abstract I will present aembedded new in the theoretical GALFORM semi-analytical model model which of simulatesdark the the formation matter and formation universe. evolution of and Using galaxies in this evolution a codethe Lambda of cold I evolution active calculate of the galactic massive fundamental nuclei black parametersThe holes (mass, (AGN). model spin (BHs) The reproduces and hosted the calculation accretion at observed rate) is optical, the that X-ray galactic describe and centres bolometric and luminosity make functions predictions of AGN for up their to disc luminosities. Unravelling the properties of active galaxies in hierarchical cosmologies Galaxy Formation, Durham, Thursday, 21st July 2011 University of California, Santa Cruz could not have been triggered by a major 2 with CANDELS ∼ 2 z ∼ z [email protected] Dr Dale Kocevski 100 for the first time. This imaging was taken as part of the Cosmic Assembly 2 ∼ z . I will show that from visual classifications we have determined that AGN hosts do not exhibit merger or interaction 5 . 1 merger event in the recentanalytic past. cosmological I models will which compare incorporatediscuss the a the observed prescription implications properties for for of AGN merger-triggered, the feedback self-regulated models. AGN black hosts hole to growth what and is predicted from semi- signatures more often than non-activemorphological galaxies breakup of similar of mass these atresults galaxies this suggest and redshift. that find We the that have bulk a also of used high the Galfit fraction X-ray to of determine luminous the the AGN AGN population are at located in disk-like systems. Our Near-IR Deep Extragalactic Legacy Survey (CANDELS), whichz aims to > document the evolution of galaxies and black holes at Notes Abstract Using high-resolution HST/WFC3 imaging inand the colors J of X-ray and selected H AGN bands, hosts we at have examined the rest-frame optical morphologies Investigating the AGN - Merger Connection at Galaxy Formation, Durham, Thursday, 21st July 2011 Princeton University [email protected] Dr Gregory Novak 100 kpc. We carefully treat the forces on the gas due to dust ∼ 101 1 pc to ∼ Notes opacity in the UV, optical, and IR bandsfor from photons angular generated by momentum both transport, stars and allowing thethe central us AGN. axisymmetric We to code. include consider a prescription We galaxies considerrapid with the removal large of case specific of the angular angular including momentahole momentum steady (disk accretion of cosmological rate galaxies) a infall depends in strongly cold of on gas coldinfalling the disk gas, gas inner between to as radius 1 of mimic well and the the as 100 simulation,processes. effect the pc implying of case have that an physical a of important processes galaxy the effect that merger. on operate the on We true find black that hole accretion the rate black and the resulting feedback Abstract We have performed axisymmetric hydrodynamic simulations black holeof fueling and the feedback in central a black massive galaxy. holefeedback The on (in effects the the form temperature of and a broad-line momentumThe wind) of simulations are cover galactic treated a carefully gas using range resulting a of from detailed length and both scales physically radiative from well-motivated prescription. and mechanical Black Hole Fueling and AGN Feedback 102 Oral Programme Abstracts Friday, 22nd July 2011

103 Galaxy Formation, Durham, Friday, 22nd July 2011 Johns Hopkins University Prof Timothy Heckman [email protected] 104 Notes Abstract I will review our understanding of the physicalfocus processes on that the connect present-day supermassive universe black where holes we and havetwo their the disjoint host most families. galaxies. complete set I One of will is information. characterizedof The by local lower-mass strong AGN population emission-lines black consists and holes of traces inregion. the relatively Stars lower rapid may mass be growth the bulges. of source thedo of population not It both play the is a fuel significant closely for role. the associatedoutput black The with and hole second low and star AGN of growth family formation the rates. is feedback in characterizedcooling that It by of the limits comprises radio the its central hot the jets growth. X-ray powered most few-kpc-scale gas, Galaxy by massive and mergers blackThis black this holes feedback process holes with is may in low likely also the to radiant reduce be most the limited massive amount (at bulges. least of in star The part) formation fuel by that feedback source would from is the otherwise the radio occur jets in and such lobes. galaxies. The Galaxy-AGN Connection in the Local Universe Galaxy Formation, Durham, Friday, 22nd July 2011 . 5 . 0 z > Durham University galaxy population. The 5 . 0 z > Prof David Alexander [email protected] 105 Notes review will focus on the observational evidence gathered overa the primary last decade focus from on a suite advances of made multi-wavelengthactivity facilitiesm from to with deep date). X-ray I observations will briefly (whichin discuss provide (1) the the the triggering most connection complete of between AGN census AGN activitydistant of activity, and AGN distant (3) star population, AGN formation, the and (2) growth (5) the current role rates of searches of enviroment for distant the black most holes, heavily obscured (4) AGNs the and evidence their for properties. energetic outflows in the Abstract There is now significant evidencelution that of Active galaxies. Galactic Nuclei Theoretical (AGNs) modelsmassive have require galaxies had energetic and a AGN the significant outflows role seminalblack to in discovery holes terminate the of suggests or formation a that regulate and tight massive star evo- relationshipfrared, black formation radio, between holes in and grew the optical the in mass surveys most concert we of now with galaxy know the that spheroids host the and galaxy. majority their of From the central AGN a activity combination in of the deep Universe has X-ray, occured in- at Active Galactic Nuclei in the Distant Galaxy Population In this review I will discuss our current understanding of the role and impact of AGNs in the Galaxy Formation, Durham, Friday, 22nd July 2011 University of California, Berkeley Dr Philip Hopkins [email protected] 106 Notes The role of mergers and AGN in the form & evolution of the galaxy population Galaxy Formation, Durham, Friday, 22nd July 2011 z > Imperial College London . 1 . 0 Dr Daniel Mortlock [email protected] > HI f 107 black hole, the formation of which just 0.8 Gyr after the Big Bang places significant ⊙ M 9 10 × 2 . It hosts a 085 . = 7 because they have been identified primarily in optical surveys. Using data from the UKIRT Infrared Deep Sky Survey z 5 . restrictions on the possible models of blackcombined hole with growth. a The small Ly visible alpha sizeneutral of fraction transmission the of profile ionized the “near inter-galactic that zone” medium around is around the consistent the quasar, quasar with was a damping wing, provide strong evidence that the 6 (UKIDSS), it has been possibleof to search beyond this optical limit, resulting in the discovery of a new quasar at a redshift Notes Abstract Quasars are powerful probes of the high-redshift Universe, although previously none were known beyond a redshift of The discovery of a luminous redshift 7.1 quasar Galaxy Formation, Durham, Friday, 22nd July 2011 Stanford University Prof Tom Abel [email protected] 108 Notes The first stars and black holes Galaxy Formation, Durham, Friday, 22nd July 2011 7 to ∼ 10 z ∼ z Leiden University Dr Rychard Bouwens [email protected] 109 , but we have also been able to quantify galaxy growth from 10 ∼ z through studies of the luminosity function, stellar masses, and specific star formation rate. Studies of faint 4 ∼ z galaxies in fields like theIn Hubble this Ultra presentation, Deep I Field provide have a allowed brief us overview of to some estimate of the the contribution mostNotes of exciting galaxies new to observational reionization. results. Abstract One of the most exciting frontiers inallow cosmology us today to are the directly observations trace ofuniverse. very galaxy Fortunately, high-redshift growth this galaxies. whole from Such field observations earlygalaxy has times searches advanced and out very to rapidly explore in redshifts the the as likely last high role few as years. of galaxies Not only in have the we reionization been of able the to push The first galaxies Galaxy Formation, Durham, Friday, 22nd July 2011 Princeton University Dr John Wise [email protected] 110 Notes Abstract The first stars and galaxies hadthe a intergalactic profound medium. impact Here on I the presentfocus results universe, on from leading the adaptive to formation mesh reionization of refinement the and radiationstars first the hydrodynamics galaxies that chemical simulations with populate enrichment that a of the self-consistent first transitionobservations from galaxies. prior massive to metal-free These reionization. stars results to provide metal-enriched invaluable insight for interpreting the latest and future galaxy From the First Stars to Dwarf Galaxies Galaxy Formation, Durham, Friday, 22nd July 2011 University of Edinburgh Prof James Dunlop [email protected] 111 Notes Abstract I will present the latest results onfrom the galaxies number at density, z star-formation = histories, stellar 6 masses -(UDS and 10, and likely based UV GOODS-South). the escape on fractions the The HSTrates WFC3 presentation from imaging will McLure of both et include the al. our Ultraet Deep latest al. (2011), Fields, results and 2011), an the on and update first stellar new on CANDELSfrom measurements fields CANDELS masses the and, of and controversy possibly, the from over specific galaxy UltraVISTA the star-fromation at UVfor UV the luminosity models very slopes function of bright of at end. galaxy z= faint I formation,redshift 7 will high-redshift and briefly range and galaxies for discuss z z (Dunlop the answering = = implications 10 the of 8, - question these incorporating 6 results of the reionized whether the first the Universe. results growing population of galaxies seen in the Galaxies at z = 6 - 10, and cosmic reionization Galaxy Formation, Durham, Friday, 22nd July 2011 . This 3 − Mpc 4 − 10 × Texas A&M University the gas accretion rates are = 2 4 n z > . At 3 − the SFR overtakes the gas accretion rate, 4 Mpc 4 Dr Casey Papovich [email protected] − z < 10 × = 2 n 112 . This conflicts with assumptions that the SFR is either constant or 2 . 0 ± for galaxies with 7 selected at constant comoving number density, . 9 . 8 0 ) z = 1 α < z < (1 + 3 with ∼ α t gas f ∼ as , implying that the SFRs increase with time. I will present an empirical study of the cosmologically ) 3 t = 3 to Ψ( z as to = 8 3 z to , galaxies with this number density depart from these relations implying that star formation and gas accretion = 8 3 z = 8 z < z are slowed. as fast and may evenand exceed at the SFR: this is the “gas accretion epoch”. At allows the study of the evolutionthat of evolve strongly galaxies in not time. possible using Thisfrom analysis galaxies shows selected that at the constant cosmologically stellardeclines averaged mass SFRs exponentially or of in SFR, these time. quantities galaxies Furthermore, increaseThis smoothly the provides stellar evidence that mass the growth slope in offormation these the is galaxies high-mass much end less is of than consistent unity. the with IMFdisk Assuming this is growth that approximately derived under these Salpeter the relations SFH. unless assumption follow that the from the duty gasdecrease SFR cycle accretion from depends of (or on star mergers) the coupled local with gas galaxy surface density, then this predicts that gas fractions Notes Abstract Distant galaxies show correlations between their currentstar-formation star-formation histories (SFHs) rates are (SFRs) highly and similar. stellar Moreover, masses,grow observations implying from show that that their the UV luminosities and stellar masses The Star Formation Histories of Distant Galaxies and Implications for Gas Accretion averaged evolution in galaxies at Galaxy Formation, Durham, Friday, 22nd July 2011 . 3 ∼ z CEA-Saclay . 3 Dr James Mullaney [email protected] ∼ z 113 . Recent results from these facilities are painting a picture of differential BH and galaxy growth, in 3 ∼ z Notes Abstract There is now substantialwithin evidence their that host the galaxies. growth However,continued of when debate supermassive perpetuated and by how black our the holes lack tightobservations of (BH) links from observational between coincides constraints e.g. these in with this processes Chandra, star-formation field.and were XMM, galaxy (SF) forged Now, Spitzer mass however, is to and deep still Herschel, X-ray a and arewhich matter infrared these providing of links the were first predominantly forged glimpses inlevels of of short activity the periods being of joint largely intense unconnected. build SF and up Inwhich light AGN provide of of activity the BH this, with clearest I more view will common, present of moderate the how latest AGN results and from SF the activity Herschel-GOODS survey have co-evolved since The Herschel-GOODS View of the Build Up of SMBH and Galaxy Mass Since Galaxy Formation, Durham, Friday, 22nd July 2011 University of California Santa Barbara 114 Dr Vardha Nicola Bennert [email protected] Notes Abstract Supermassive Black Holes (BHs) seem toThe be tight ubiquitous empirical in the relations center betweendispersion of sigma, the spheroids luminosity mass - L, and elliptical of stellar galaxies the massgrowth and M) of BH bulges discovered BHs in and of and the spirals. the the local formation Universe properties and indicateresults evolution of a from of close a the galaxies. connection unique host-galaxy To between three-fold understand the approach. spheroid thebuild (i) origin (stellar a From of velocity robust a these baseline sample scaling of relations, of the I BH will 100spectroscopy mass present Active with scaling Galactic relations SDSS Nuclei (MBH-sigma, (AGNs) imaging. MBH-L, in MBH-M), thetime combining (ii) local spatially-resolved of Universe, We Keck 4-6 we study Gyrs the using evolution Keckpeak of spectra of AGN and the activity HST MBH-sigma and images. the and establishment (iii)spheroid MBH-L of We stellar the relations extend present-day masses out Hubble this using sequence, to study deep a a out multi-color look-backfrom to look-back time HST (i) of the images indicate 8-10 pivotal from that Gyrs. cosmic GOODS AGNs We time and follow measure precedes between the determine bulge the same the assembly. scaling MBH-M relations relation. as Combining Ourbeing inactive results results transformed galaxies. from into From bulges. (i-iii) (ii-iii) allows we us conclude that to BH test growth the hypothesis that evolution is driven by disks out to a Lookback Time of 10 Gyrs The Black-Hole Mass Scaling Relations of Active Galaxies: From the Local Universe Galaxy Formation, Durham, Friday, 22nd July 2011 Yale University moderate-luminosity AGN 2 ∼ z Dr Kevin Schawinski [email protected] is now accessible in great detail due to the infrared 2 ∼ z , while quasar-luminosity AGN reside on major, gas-rich 0 ∼ 115 z Universe: secular black hole growth and first 2 ∼ z Notes Abstract The peak epoch of both star formation and black hole accretion at HST-WFC3/IR Reveals the glimpses of seed black holes mergers. Slitless spectroscopy of obscuredindications AGN host of galaxies very reveal recent a quenching. diversityrelation. of I recent will star discuss formation histories implications including for co-evolution scenarios and the origin of the M-sigma capabilities of the Wide Fieldframe Camera optical 3. properties I of will AGN presentdata. host recent galaxies Early results in results and deep from describe fields WFC3/IR ongoinghost (CDF-N/S, efforts imaging galaxies COSMOS) to data is with characterize indicate very imaging the that and similar rest- the slitless to morphological spectroscopic that mix of of the population at Poster Programme Abstracts Sunday, 17th July to Friday, 22nd July 2011

116 Galaxy Formation, Durham, Poster Programme Gyr, and shows a decreas- University of Nottingham 13 /Fe] ratios because of the small Australian National University α University of Wisconsin-Madison Dr Hanni Lux [email protected] , and has higher [ 3 > ∼ [email protected] Dr Chiaki Kobayashi z Mrs Kathleen Barger [email protected] 117 /Fe] and increasing trends of [(Na,Al,Cu,Mn)/Fe] against [Fe/H]. However, the stars tend to have α /Fe] and lower [Mn/Fe] than stars. We also predict the frequency distribution of elemental abundance α contribution from Type Ia Supernovae.ing The trend disk of formed [ with ahigher constant [ star formation over ratios as functions of time and location, which can be directly compared with galactic archeology projects such as HERMES. Theories of galaxy formation are typically testedthe on satellites large of scales our with own sets Milky of Way thousands yieldscales. of a galaxies. unique For data However, set example, the with comparing proximity which the we of canLCDM orbits test simulations of galaxy can formation the yield models dwarf important down galaxies to constraints very on aroundVia small the the Lactea missing Milky to satellites Way address problem. with the We question orbits usetypical of of the model high how subsets and resolution well of simulation measurement the satellites orbits errors. in ofand We the evaluate then local their apply dwarf these galaxies agreement can results withdistribution be to subsets is determined the consistent of while ’classical’ with accounting subhaloes dwarf the for in galaxies mostgalaxies around the massive formed the subhaloes Via before Milky that Lactea reionisation. Way formed simulation. before z=10. We This find agrees that with the their notion mean that apocenter dwarf Abstract 1.3 Local dwarf galaxies and their links to galaxy formation Abstract We present chemodynamical simulations ofcludes a supernova Milky feedback Way-type and galaxy chemical using enrichment,In a and the self-consistent predict simulated hydrodynamical the galaxy, code spatial the distribution that kinematicalvations. of in- and elements chemical from The properties Oxygen bulge of to formed the Zinc. from bulge, disk, the and assembly halo of are subgalaxies consistent at with the obser- 1.2 Chemodynamical Simulations of the Milky Way Galaxy Abstract The Magellanic System exhibitsgaseous some structures of strewn the throughoutforces nearest the can partly halos examples - of of if not the interactions dominantlyInteraction - Milky with affecting produce halo Way this gas galaxy stripped and and material exposure evolution as the toand the with radiation their Magellanic Clouds ability from extended encounter to all Clouds. form each three stars. other galaxies and shapes In ModelsMagellanic the this their Bridge, Milky work, shown extended we a Way. structures, that use structure their the evolution, between tidal Wisconsin H-alpha thethe Mapper Clouds. amount to and study H the extent I faint, of studies warm the ionizedthe have ionized gas evolution extensively gas in of mapped the remains this the uncertain. system: neutral A How gasformation? census much in of Is gas this the this have region, material environment the but allows conducive galaxies us to lost to star to ask formation? this questions structure? addressing How does the gas loss affect future star Gas in the Magellanic Bridge using WHAM 1.1 Understanding the Evolution of the Magellanic System: A Survey of the Ionized Galaxy Formation, Durham, Poster Programme University of Vienna Swinburne University of Technology Dr Adam Ruzicka [email protected] Special Astrophysical Observatory, Russia Mr Simon Mutch [email protected] 118 Dr Lidia Makarova [email protected] We studied star formation anding associated the extended supernova–induced gaseous gas tails blowoutinvestigated. associated in with the the Magellanic Clouds Clouds. (the Magellanic Their Stream role and in the feed- Leading Arm) with matter was Abstract 1.6 Stellar feedback and redistribution of gas in the Magellanic Clouds Upcoming next generation galactic surveys, suchture as and GAIA and make-up HERMES, of will our deliverbenefit Galaxy, unprecedented our detail the broader about Milky knowledge the Way, of struc- respect galaxy and to other formation promise galaxies and of to its evolution radically type.Digital we improve Through Sky first modeling Survey our and and need understanding comparison Galaxy to with Zoo, of a we quantifyM31 it. large provide how are tentative sample yet undergoing of typical However, tantalizing galaxies a the evidence drawn critical to to from transformation Galaxy show the ofwith is that Sloan their both with global galaxies the properties. Milky midway Way Both between and appear nearby to thevalley’ possess distinct galaxies attributes that are blue are transition and consistent objects red whosefinding bimodal star reveals the formation color possible typically populations. future will of havetransformations In our all up extragalactic own but close. galactic surveys, extinguished home, in such and less opens ’green than a 5 new window Gyrs. of This opportunity to study such galactic Abstract 1.5 The mid-life crisis of the Milky Way and M31 Abstract We present a quantitative starthe formation vicinity history of of the the Local nearbywas Group observed dwarf of within galaxy galaxies our UGCA HST/ACS in project 92. thebranch. number zone 9771 This We of (PI irregular have I. strong dwarf Karachentsev) constructed Galactic and is modelsdependence extinction resolved situated of on into (IC time. the in stars 342 resolved According including group to old stellar of our red populationsThere measurements, giant galaxies). and stars the measured main looks The star star galaxy mostly formation formation metal-poor, activity raterecent period with and star occured the metallicity about formation 8 mean starting - metallicity about 14star [Fe/H] 2 Gyr formation ago. of Gyr period has about ago higher metallicity and -1.5 of enhanced to aboutof -0.6 moderately -2.0 the to till IC dex. -0.3 342 dex. to group There In our and our time. are study its we indications possible It also of influence have is analysed on very the the spatial likely star structure formation that activity. the ongoing 1.4 Star Formation History of the UGCA 92 and IC 342 Group Structure Galaxy Formation, Durham, Poster Programme dex, 08 . 0 ± 14 . 1 and a magnitude limit 2 . The ratio between these Saint Mary’s University 01 . university of Hertfordshire 0 0.8 deg ± ∼ 20 . ) = 1 [email protected] Ms Liz Arcila K − J ( Miss Lisette Sibbons [email protected] 2 from the CFHT Legacy Survey. ∼ 2.5 and distinguish between star-forming and passive galaxies. 119 < z < and the colour separation for C- and M-type stars falls at 11 . 0 ± 41 . 24 (AB magnitudes). The combination of depth, area, and four independent sightlines give us an excellent way to < = 17 We obtain galaxy number counts and luminosityat functions. this From epoch the and luminosity the functions we stellarpeak infer mass of the density the stellar of passive mass the galaxy function Universe. luminosity function,and An and a important the handle characteristic large on of area cosmic our and variance. four results independent is sightlines that give they us go excellent past statistics the of K probe the galaxy population at highthe redshift. CFHTLS filters) We to use select the galaxies BzK with redshifts selection 1.4 criteria (adapted to a gzK selection criteria to match Abstract We present results from the four CFHT Legacy Survey Deep fields with an effective area of 2.1 Passive and Star-forming Galaxies at z with noticeable variations when examined asmagnitude a function of of the galactocentric tip distance. of Astructures variation the within has the red also galaxy been giant relative detected branch to in our which the line isSummarizing, of believed I sight. to will present be an due investigationvarying to metallicity of and either the AGB a resolved stellar density AGB composite have populationing population been across of identified or and the the overlapping how evolutionary NGC they history 6822; may of be discuss this interpreted how to galaxy. regions further our of understand- Abstract NGC 6822 is a small Irregulara dwarf unique that opportunity forms to part study of galacticThe the metallicity evolution Local gradient within Group. and the Its the Local close distribution Group of proximitycomponent without the and of stellar the apparent population the influence isolation have provide of population been strong studiedcarbon- in dynamical using and NGC the factors. oxygen-rich asymptotic intermediate-age 6822. branch AGB (AGB) starsK have Using been deep isolated. The high tip quality of the near-infrared red photometry, giant branch taken has with been located UKIRT, at the galaxy NGC 6822: an IR study of AGB stars 1.7 The old- and intermediate-age population of the isolated Local Group dwarf populations - the C/M ratio -and has the then distribution been used of to the derivethe AGB the galaxy population [Fe/H] centre. were abundance Our then across analysis analysed the indicates galaxy. as an a overall The C/M [Fe/H] function number abundance of ratio radial of distance 0.29 and and a azimuthal mean angle [Fe/H] about value of Galaxy Formation, Durham, Poster Programme 2 > ∼ ESO 3 . = 2 z 1 dex from z = 2.2 to Durham University ∼ . Thus, the average ISM 1000 times more intense 3 2.2. Galaxies with log M ∼ − ∼ Dr Gabriel Brammer [email protected] cm 4 10 ∼ n 2 Ms Alice Danielson [email protected] ∼ 2.2; however, the nature of massive red galaxies < z < at a level of detail that has only recently become possible Msun can explain much of the strong density evolution of 3 . 2 11 ∼ 120 10 z > submillimetre galaxy SMM J2135–0102. We obtain very high signal-to-noise ratio detections of 11 3 . = 2 z . 1 . 0 z < found by the NMBS. quiescent galaxies, due largely to thegalaxies, steepness which of show the a exponential similarly end steep of increasefor the in mass building their function. up number This densities. the is We massive notby propose (quiescent) true that transforming for galaxy mergers galaxies less are population, massive from primary while mechanism theWFC3 less star-forming grism massive population. survey quiescent that Finally, confirm galaxies the we are bimodal present continuously population promising formed of early truly quiescent results and from dusty the star-forming 3D-HST massive galaxies at z 10.5 Msun are nearly all redchanges in remarkably rest-frame with U−V redshift. over We the findquiescent, full an ”red range increasing fraction and 0 of dead” dusty galaxies star-forming with galaxiesthe redshift. and present The a day, mass decreasing whereas fraction density the of of mass quiescentgrowth density galaxies (i.e., increases in a by star-forming factor galaxies of is two) roughly of flat individual over the galaxies same at time M period. Modest mass transitions from three species and limits onstrengths a to investigate further the 20 gas transitions mass, from kinematic ninefor structure species. and a interstellar We two-phase medium use (ISM) medium the chemistry 12CO, within and [Cunderlying find this I] strong extended high-redshift evidence and cool, HCN starburst line low-excitation galaxy, massive comprisingshow a component. that hot, on Employing dense, average a the luminousthan molecular component suite the gas and of is Milky an photodissociation exposed Way, region to with models,density an star-forming and we ultraviolet far-UV regions radiation (UV) having field radiation intensity a field areto characteristic similar that those to density is those found of found in in local the ultraluminoussystem. central infrared The galaxies regions 12CO (ULIRGs) of spectral and line typical energy starburstkinematic distribution galaxies, and components line even with profiles though different give strong conditions, the evidencewithin including star that clouds, temperature, formation the likely system and as rate a comprises line is result multiple ratios of fara high suggestive higher star wealth of formation in of high density. information this cosmic-ray By on virtue flux the ofat star the lens formation amplification, and these ISM observations at uncover Abstract We present an analysis ofthe the lensed molecular and atomic gas emission in the rest-frame far-infrared and submillimetre from 2.3 The properties of the in a star-forming galaxy at Abstract We use the NEWFIRM Medium-Band Survey to study the buildup of massive galaxies since z 2.2 The Buildup of the Massive Red Sequence Since z Galaxy Formation, Durham, Poster Programme ) ). ∼ 0 . % to 059 . ). We 11 10 ∼ = 0 Gyr ) 3 . s z ), weakly star 0 INAF-OABO ⊙ − logM 1 /(1+ . M z 0 ∆ 65 . ∼ σ 10 τ 1 dex for 10 –3.0. We have studied the University Of Manchester ∼ 4 . , ⟩ ∼ 5 . 1 = 1 M ⟨ is dominated by the star-forming z ∼ 5 . z in the redshift bins considered, being 1 to > ∼ 7 dex . z 1 2 ∼ ∼ . These observations will provide a powerful, 5 z , e-MERLIN gives us our first truly reliable view of [email protected] Dr Melanie Gendre 1 Mrs Helena Dominguez Sanchez [email protected] 1.4) quiescent galaxies over an effective area of z > . The fraction of star-forming galaxies decreases from ≥ z > , while the quiescent population increases from ⊙ ⊙ M 8 M 1.4 in the COSMOS field with multi-wavelength coverage ex- . 0.15) and small e-folding time scales ( 0 . 10 ≥ ≤ 121 11 10 10 ≥ ∼ 0.5–1.5 kpc at M < M one. We have derived accurate photometric redshifts ( µm 18000 galaxies at z the contribution to the total MF of the quiescent galaxies is significant and becomes 24 ∼ 1.4–1.6 for 5 . 1 ∼ z < ∼ . Spitzer z 7 . 2 ∼ z is an epoch of transition of the GSMF: while the MF at 2.5–3.0 to 5 ∼ ) at . 3 1 z − ∼ 22.0) selected sample of z Mpc < ⊙ % from in the COSMOS field. Galaxies have been divided according to their star-formation activity and the evolution of M µm 20 6 2 . 3 6.0 deg % at the same redshift and mass intervals. We compare the fraction of quiescent galaxies derived with that predicted by % to ∼ 7 . mag 50 theoretical models and find significantmode. discrepancie Finally, with we calculate some the ofand stellar them find mass and that density the a of stellar the goodρ star-forming mass agreement and density with quiescent of the populations the as Millenium-based quiescent a galaxies function decreases of by redshift 60 tending from the U band to the the different populations, in particular of( the quiescent galaxies, has been investigated in detail. We have studied an IRAC 1 We find that galaxies at all stellar masses, at higher than that of the star-forming population for obscuration-independent tool for measuring thetracing massive the star development formation of the and stellar AGNof populations 50–200 activity and mas in the in C- black high-redshift and hole galaxies, L-Bands, growth correspondingthe hence to in distribution the of first star-formation massive within typical galaxies. galaxies Withwere at being a the formed. resolution epoch e-MERLIN where will the disentangle bulk the ofthe relative the apparently contributions stars of simultaneous in AGN the growth and present-day star-formation, of Universe an thedeveloped essential step black a given holes strategy and comprising stellar of populationsquestions nested about in tiers, the galaxies. which formation together To and achieve provide jointdata these evolution a product goals, of single, with AGN we coherent lasting and have legacy survey galaxies. value addressing The for fundamental completed the survey whole will astronomical community. provide a homogeneous Abstract This Legacy survey exploits e-MERLIN’sand unique evolution combination of of star-forming sensitivity galaxies and and spatial AGN resolution out to to study redshifts the of formation 2.5 The e-MERGE Survey: e-MERlin Galaxy Evolution Survey through a SED-fitting procedure.the Other galaxies important have physical been parameters obtainedintermediate (masses, and using ages quiescent Maraston galaxies and depending (2005) star on models. their formationgalaxy specific stellar rates star We mass formation (SFR)) function have rate of (GSMF) (SSFR=SFR/M). divided We ofproperties our have the of computed total sample high the sample redshift into and quiescent actively galaxies the finding different star-forming, forming that stellar populations populations they at with are low old dust (1–4 extinction Gyr), (E(B-V) observe massive a ( continous evolution of the quiescent stellar mass function from Abstract The goal of this work is to study the evolution of high redshift (z 2.4 The Evolution of Quiescent Galaxies at High Redshifts Galaxy Formation, Durham, Poster Programme . . 7 7 . . = 5 = 5 UCSB z z Durham University São Paulo University Dr Alaina Henry [email protected] dropout luminosity function − i emitting galaxies (LAEs) at α Dr Thais Idiart [email protected] Mr Christopher Harrison [email protected] kpc) [O iii] emission indicates the presence of large-scale 4 emission from a small sample of sub-mm bright galaxies host- ≥ 122 5007 λ can find the faintest galaxies by maximizing the contrast with the sky back- 6 ∼ z emission at . Extending observations to ever fainter populations is therefore critical in order to quantify α 6 > ∼ luminosity function of these galaxies, giving the first constraints on the faint-end slope at z α searches for Ly radio galaxies. I present some of the results from our Gemini-North Near-Infrared Field Spectrometer (NIFS) 2 z > Galaxies are the beacons that lightlogical up models distant are regions very and successful at also explainingare the the building-blocks able largest that structures to chart in form the the Universe. Universe, theirtypes, but Modern stars elliptical a cosmo- coherent and (E) picture galaxies their of seem evolution howobserved galaxies to properties. through be Usually cosmic we the time search simplest in isis ones, these still essentially observable with properties missing. related mass an to indicators imprint Among their of presentingful their the stellar robust tools previous population different formation correlations for formation history, morphological deriving with which history. mean many agesanalytical Particularly, and model spectroscopy chemical of and abundances E color of a indices galaxyintergalactic given are gas formation stellar continuously power- and population or evolution, distribution. during including mergerdriving Here the episodes. the we progressive presented possibility The enrichment an of feedback of the is proto-galaxytually interstellar governed formation producing medium mainly (ISM) galactic by by by winds. accretion supernova metals Two (SN) of andquenched phases the explosions, and energy of a injection ISM cold into are and the considered: neutral ISM,SN phase a even- where explosions hot stars and and are those ionized formed. returned phase The toradiative in ionization the cooling which rate ISM followed is the by by estimated star recombination stars. by processes formation the The transformages is hot part onset and gas of of metallicities generated the galactic for by hot wind a gas removes sample intohierarchical the hot of model, cold gas early is phase. discussed. from type The the galaxies A resulting system comparison are mean evolution. is presented and made and the with the the apparent results of down-sizing cosmological effect, simulations opposite of to galaxy the formation and Abstract LAEs are now confirmed withshifts. luminosities I that present have the only Ly beenThis achieved unprecedented for measurement a allows a fewmeasured comparison strongly by to lensed Bouwens the galaxies et steep at al. faint-end similardiscussed. (2007). slope red- Additionally, of the the faint LAE contribution to the hydrogen-ionizing background will be 2.8 Galaxy Evolution Through the Cosmic Time the ionizing output of galaxiesSpectroscopic and definitively determine that the intergalactic medium was reionized by star-formation. Faint star-forming galaxies that areionizing beyond background current at observational limits are often said to contribute a large fraction of the ground. I present results from a Multislit Narrowband Spectroscopic search for Ly Abstract z=5.7 2.7 New Constraints on the Faint Population of Lyman Alpha Emitting Galaxies at ing active galactic nuclei (AGN). Theredynamics. is High a velocity, wide broad variety and inenergetic in their outflows. some [O cases Winds iii] extended radiatively properties; driven ( with by multiplebe the responsible. components AGN and and/or turbulent supernovae winds from intense star formation are likely to programmes. We have taken observations of the [O iii] Abstract Leading models of galaxy formationtheir central require black large-scale holes. energetic outflowsrare However, to current regulate observational the support for growth this of hypothesis distant at galaxies high and redshift is mostly limited to 2.6 Extreme Gas Kinematics in Starburst-AGN Composite Galaxies Galaxy Formation, Durham, Poster Programme . 3 1 . 1 > ∼ z ∼ − Caltech α depth of J=24.2, σ Ehime University . We also investigated the 1 from MOIRCS Deep Survey, > ∼ Mr Tucker Jones [email protected] , and J=25.1, H=23.7, Ks=24.1 3 2 z galaxies < ∼ 3 z − 3 < ∼ 1 ∼ [email protected] Dr Masaru Kajisawa ) galaxies at = 2 z ⊙ National Astronomical Observatory of Japan z galaxies relative to low-mass galaxies at M ∗ 10 M , and the evolution of the normalization for quiescent ∼ -10 5 . 9 2 123 < z < 5 . 0 Dr Masakazu Kobayashi [email protected] PSF FWHM diameter aperture) over 103 arcmin × . We found that the low-mass slope of the SMF becomes steeper with redshift from as well as the gradual decrease of the normalization of the SMF. The evolution of the number 3 3 ) galaxies is stronger than low-mass (10 ∼ ⊙ ∼ z M z 11 at 6 10 . 1 even at ∼ ( ⊙ of the survey area. We used the deep NIR data to construct a nearly stellar-mass-limited sample down to ∗ M ∼ − 2 M α 10 ∼ to -10 1 5 . 9 ∼ 10 z Abstract We have been constructed a theoretical modelgalaxy for high-z formation Lyman-Alpha (Nagashima emitters (LAEs) & based Yoshii onextinction 2004). a semi-analytical and model Our galactic-wind for model into phenomenologically thereproduces incorporates escape all the probability of effects the of available of LyA observational interstellar photons statisticaldistribution) quantities dust from of (LyA their and the UV-continuum host LAEs luminosity galaxy. at functions z=3-7 andis It Lya (Kobayashi clumpy EW is et so al. found that that 2007, LyA 2010). ourphysical photons model Our quantities can model of escape predicts high-z even the LAEs dust if based geometryselected large on in as amount the our LAEs. of ISM theoretical dust of model exists LAEs and in discuss them. what type Here of we galaxies present can a be prediction observationally to the which is a deep NIR imaging survey with Subaru/MOIRCS in the GOODS-North region. The data reach 5 galaxies more strongly evolves than star-formingthe ones number in the density redshift of range. quiescent The galaxies results causes suggest the that rapid the increase strong of evolution of 2.11 A Model Prediction to the Nature of High-z Lyman-Alpha Emitters We present results on the evolution of the galaxy stellar mass function (SMF) at Abstract 2.10 Evolution of Galaxy Stellar Mass Function since density of H=23.1, and Ks=23.1 (Vega magnitude, 2 in 28 arcmin ∼ at SMF for quiescent galaxies andsignificantly star-forming flatter galaxies than that separately. of star-forming The galaxies low-mass at slope of the SMF for quiescent galaxies is Abstract The detailed study of high-redshiftof galaxies is these hampered limitations by can their beare small overcome angular highly by sizes magnified observing and by gravitationally faint massive lenseding apparent clusters. galaxies, magnitudes. of where galaxy We Both the clusters have apparent and identifiedbrightest size extensive high-redshift a and spectroscopic sources large luminosity followup. with number the I of OSIRIScombination will integral strongly of field describe lensed strong unit these lensing galaxies and and surveys from adaptive adaptive and optics HSTThe optics focus system provides data imag- on on a reveal the source observations coherent Keck plane velocity of resolution II fields, the that as telescope. multiple we fine The giant are as witnessing star-forming 100 inside-out regions, parsec growth and in ofof steep these turbulent high-redshift galaxies. metallicity rotating galaxies. gradients, galaxies which which These suggest observations will provideELTs. only a become uniquely detailed routine view with the next generation of telescopes such as ALMA, JWST, and 2.9 Resolved spectroscopy of gravitationally lensed Galaxy Formation, Durham, Poster Programme 65 ∼ UCLA Observatoire de Paris Dr David Law [email protected] University of California, Los Angeles , whereby star forming galaxies appear to 1 Mr Loic Le Tiran [email protected] − ) z (1 + Star-Forming Galaxies with 3 ∼ r − 2 124 1. In addition, I will discuss the apparent relation between galaxy Miss Katherine Kornei [email protected] ∼ ∼ 300 spectroscopically confirmed galaxies with stellar masses in the z > . With 42 orbits of F160W imaging distributed amongst 10 fields, our survey covers . I will discuss the typical morphological properties of these galaxies and the evidence for 5 . ⊙ 3 M 11 10 < z < − 5 9 . 1 = 10 M morphology and the characteristics of galactic-scale gasesous outflows. evolve onto the local late-type mass-radius relation by z Abstract I will present results fromspectroscopy. observations Taking of advantage more of this than large 50these sample, galaxies. galaxies I as will These first seen observations paint as reveal awill a they brief explain surprisingly picture were why of high 9 this the amount effect to very of is particular 12star random real physical formation Gyrs motions (not nature in ago due in of these to with the objects, observational gas outlining integral-field limitations) whyUV inside and observations we these in why conclude galaxies. a it that subsample star is of I these formation probably objects, ishigh a we self-regulated. consequence mass also of suggest end, Using that the additional an their rest-frame intense effect Initial Mass thatI Function may is will flatter be than also due Salpeter to at discuss the the ourgalactic high evolution conclusions turbulence, where as within we could has the detect been the context suggestedlines? effects of by and rate some cosmological of theories (quasi-)adiabatic gas of accretion gas star-formation. in our accretion: studies of is the there rest-frame optical a emission phase in Turbulence in the ISM, on Self-regulation and on the IMF. square arcmin to a depthrange of 27.9 AB and contains 2.14 The Effect and Influence of Star Formation and Gas Accretion on the a growth in galaxy structures at fixed stellar mass of the form I will describe some resultsredshift from range our recent HST/WFC3 rest-frame optical imaging survey of star-forming galaxies in the Abstract 2.13 Rest-Frame Optical Imaging of Abstract Outflowing winds have been observed in galaxies atquenching a of variety star of formation redshifts and and the are enrichment thought of tothe the play prevalence intergalactic an medium. important and role We properties in present both of the the resultsimaging. outflows of in We a study a investigate at sample if z = a of 1 criticalfor DEEP2 tracing star estimating objects formation galaxy with rate area rest-frame surface based UV density onformation spectroscopy is a rate and required physically surface HST to motivated optical drive density luminosity outflows, may threshold. usingmethod be Previous a of most work new estimating has strongly technique the suggested correlated area that withof over the outflows a which star (as Petrosian star opposed or formation to half-light is thelikely radius. occuring origin star represents We of formation an these discuss rate); features improvement fine (which over our structure arebasis the not FeII at commonly simple emission z observed adoption in in = local light 1, starbursts). we ofpopulations, By are galaxy and conducting able properties analyses star to on and formation examine a investigate surface the per-object density, the relationshipthe at between present the outflow day. epoch properties when and the individual global galaxy star morphology, formation stellar rate is beginning its decline to 2.12 The Prevalence and Properties of Outflowing Winds at z = 1 HST/WFC3 Galaxy Formation, Durham, Poster Programme , = 2 z –5 = 2 ETH Zurich z –5. The formation Durham University ), and that suggests a University of Oxford 7 = 2 − z 3 ∼ z [email protected] Dr Christian Maier , we find a possible “morphology-density blobs), which are likely to be the formation [email protected] Dr Yuichi Matsuda = 3 [email protected] Mr Silvio Lorenzoni α z with recent data from WFC3 on HST, including the 9 − blob) with a spatial extent to 7.5-arcsec (60 kpc), which and beyond, and the emerging picture of many studies 8 –5 with UKIRT/WFCAM and Subaru/S-Cam. We detect α 1 ∼ ∼ = 2 z from HST/WFC3: Implications for z z 125 9 blob candidates, and identify several new proto-clusters. At − α 8 than expected from lower redshift data ( ∼ 9 200 Ly z > − 8 surveys for proto-clusters and giant gaseous nebulae at emission-line nebula (or H ∼ α α z imaging surveys around several potential signposts of over-dense regions (QSOs, HzRGs, emitter, and α and H α α surveys for proto-clusters and giant gaseous nebulae at zCOSMOS galaxies, I have been able to study the physical conditions (e.g., gas metallicities, gas , we find a new proto-cluster associated with the HI over-dense region. Narrow-band surveys are and H 5 . α α 2 = 5 2000 Ly z > blobs: filamentary blobs tend to reside in lower density regions while circular blobs tend to reside in higher α and H < z < 5 α . 0 emitter, α 100 H and evolution of galaxiesobjects in often clusters discovered are in thought the to proto-clusters be are accelerated giant gaseous relative nebulae to (Ly that in low-density regions. Characteristic We present our on-going Ly Abstract is one in which, beginning atred, the bulge-dominated highest spheroidals masses, galaxies in transform whichhas from established star blue, a formation star-forming, powerful disk-dominated has galaxy systems been evolutionmodel into framework makes quenched. clear describing predictions how A and galaxies recent identifies areassociated simple the born, with main empirically live drivers these and based of drivers die model galaxy have (are evolution,sample quenched). still although of some to The actual be physical identified. processes Using recent VLT and SUBARU near-infrared spectroscopy for a 2.17 Ly sites of massive galaxies and indicative of theinteractions accelerated between galaxy galaxy formation and in the the over-dense surrounding environmentswe galaxy/IGM. through have frequent In carried order out to Ly studySMGs, the and galaxy an formation HI in over-density) the and proto-clusters, > known proto-clusters at fraction, AGN contribution, star formationresults rates) of of this these near-infrared galaxies, spectroscopy,of by and galaxy analysing discuss evolution. their how emission these Specifically,information line and (e.g., the fluxes. morphologies, future environment), near-infrared observations can I observations, give can insights willrelation, in in constrain present and the combination the origin their of with evolution main the with SFR-mass drivers the time, relation wealth and and metallicity-mass shed of light additional on the COSMOS physical mechanism(s) that quenches galaxies. The bimodal nature of the galaxy population is apparent to Abstract Spectroscopy 2.16 Constraining the Main Drivers of Galaxy Evolution with Near-Infrared significant evolution. Implications for the reionization of the universe will be discussed. is 34-arcsec (280 kpc) awayrelation” for from Ly a bright QSOdensity at regions. the At same redshift. At Abstract I will present a selection of robust galaxy candidates at redshift efficient routes to map over-dense regions atsurrounding high-z large-scale and galaxy/IGM to structures. understand the relation between the growth of galaxies and their 2.15 Star-Forming Galaxies at Hubble Ultra Deep Field and theto Early fit Release the Science characteristic images number of density thefound and GOODS-South fewer the field. characteristic Lyman-break We luminosity now galaxy for have at the enough UV candidates Schechter function at that redshift. We we find the first candidate for giant H Reionization Galaxy Formation, Durham, Poster Programme between 13 . 0 , and GALEX ± 5 . 11 2 . 1 − − ) 5 Leiden Observatory z . 1 ∼ (1 + z Galaxies 5 University of California, Berkeley . 2 University of California Santa Cruz 2 ∼ ∼ z Mr Moein Mosleh [email protected] z ), BM/BX galaxies at 5 . 3 − -band images (corresponding to rest-frame optical/NIR) s [email protected] Ms Sarah Newman 5 . K 2 [email protected] Dr Elizabeth McGrath ∼ 126 to the present. Evidence that massive quiescent galaxies undergo z 5 . galaxies. We are able to characterize properties of the wind using 2 2 ∼ ∼ z z -drop technique ( U ). The median sizes of these UV-bright galaxies evolve as 5 to the present has been steadily increasing. The compact sizes of high-redshift quiescent . 1 1 − 6 z > . 0 ∼ kpc and there is little difference in their size distribution to the UV-bright star forming galaxies. z 45 . . The sizes of the galaxies are measured from 0 5 . ± . The UV-bright galaxies are significantly larger than quiescent galaxies at the same mass and redshift by 3 5 . 90 ∼ . 3 dex. We also verify the correlation between color and stellar mass density of galaxies to high redshifts. The sizes 2 z − 09 . 5 0 . 0 ± , [NII] and [SII] line emission. These massive winds have very large outflow rates, often in excess of the star-formation ∼ 45 α . Abstract Using SINFONI/VLT integral field spectroscopyresolved with adaptive giant optics, star-forming we clumps have in observed several large-scale galactic outflows from 2.20 Outflows From Massive Star-Forming Clumps in H rates of the clumps.starburst We galaxies, study to the understand structure how star-formation ofis varies the also at wind important different using for redshifts. constraining emission Examiningon the line the galaxy recycling ratios properties evolution. of and of heavy these relate elements winds this into to the observations IGM of and local the effects of star-formation feedback Abstract We study the evolution offield the up size to - stellar mass relation for a large spectroscopic sample of galaxies in the GOODs North 2.19 The Evolution of the Mass-Size relation to z=3.5 in the GOODS-North Field galaxies imply densities that are upHowever, it to is two unclear orders whether measurements of to-date, magnitudeunderestimated many greater of due which than to have galaxies effects relied in on such rest-frame thethese as near-UV compact local signal-to-noise imaging, galaxies Universe have and could been of survive age as similar or the mass. halos metallicity cores through of gradients. dry massive ellipticals Recently mergers, in thus it the preserving has localDELS the Universe, been imaging central growing suggested mass at low-surface-brightness that density both while rest-frame increasingof near-UV the passive and effective galaxies optical radii. for wavelengths the The allows first depthgrow time us of their over CAN- to a halos reliably large and measure region how sizes of they and the evolve sky, color onto enabling gradients the us local to size-mass determine relation. when early-type galaxies start to from the Subaru 8m telescope.given mass We evolve reproduce with earlier redshift. resultsgalaxies based Specifically, (LBGs) on we selected photometric compare through redshifts sizes the that of the UV-bright galaxies sizes at of a galaxies range at of a redshifts: Lyman break Abstract Using high-resolution imaging dataDELS), from we examine the the growth Cosmic of Assembly spheroids from Near-Infrared Deep Extragalactic Legacy Survey (CAN- 2.18 The Growth of Massive Quiescent Galaxies since dramatic size evolution from 0 of sub-mm galaxies in the same fieldof are SMGs measured is and compared with BM/BX galaxies. We find that median half-light radii LBGs at low redshift ( z Galaxy Formation, Durham, Poster Programme have 1 galaxy, at fixed . These ∗ 2 5 Caltech . 1 M ∼ z < CEA Saclay z < z < 0 /yr of star formation, at carry very small amounts Saint Mary’s University ⊙ 2 over 2 M ∼ ∼ show a strong correlation with 50 z to date, comprising 17 high-S/N ∗ > L 6 Mr Andrew Newman [email protected] 1.4–2 times higher than that given . 1 ∼ are important contributors to keeping Dr Maurilio Pannella [email protected] ∗ results are correct, they imply enormous L 2 galaxies at that’s < z < ∗ ∼ 3 . 1 L . z 2 1 [email protected] Prof Marcin Sawicki ∼ and 4 are host to z 20% of UV photons escape from a typical red sequence. Comprehensive studies at 3 ∼ ∼ = 0 z /yr. We interpret this as shut-down of star formation in the z ⊙ 127 galaxy population to study how galaxies build up their masses. M 2 2 halos at ∼ ∼ ⊙ z M . Until recently, there were very few high-quality spectra of red galaxies in 12 2 1.7 only 10 results seemingly requires dramatic size expansion by another factor of 2 over ∼ 2 ∼ z ∼ < z < z 1 +3 one; this paucity of dust means that sub- ∗ M /yr, and at ⊙ . Turning to clustering measurements, we find that the star formation rates in the most massive ) into the UV-selected 2 M ∼ 20 = 28 z ∼ lim R they produce 2 . 2 ∼ most massive halos and evidence thatdark galaxy matter downsizing halos is that related host not just them. to galaxy stellar masses, but to the masses of the z more than half make it outthe Universe of ionized an at haloes decline with redshift, so that while First, we find that star formation rates in galaxies below the luminosity function knee at galaxy stellar mass. This correlationof suggests material that into star their formation darkshallower in halos. surveys these would low-mass Next, suggest, objects the resulting is low-mass inby fueled end a extrapolations by stellar of of ongoing mass the most accretion density stellar of at somewhat mass the more function shallower rapidly is surveys: than was steeper apparently previously thanof the thought. dust extrapolations build-up compared We from to also of their find stellar more that luminous mass sub- cousins, in so the that while universe only has proceeded We probe deep ( early, massive systems are farto from 5 being times fully-formed smaller ellipticals. inshown size Rather, relatively than they little their change appear likely in extremely descendants the compact on massive and galaxy the may population. be Thus, up if the examples. Using accurate dynamical mass measures, we confirm a growth in size by a factor of Abstract 2.23 The build-up of mass in faint UV-selected galaxies at high redshift I will discuss the UV-to-IR propertiesuse of a galaxies sample, at selected from redshift highly between accurate 1ing photometric and analysis redshifts, 4, drawn across from i.e. their the over full GOODS North theGOODS multiwavelength field, main Herschel spectrum, and epoch IR perform spanning of a dataset from galaxy stack- and the assembly.of all optical I these the Subaru galaxies way imaging, and to through UV the the dust VLA ultradeep attenuation 20cm and continuum. on how I these will properties present all first ultimately depend results on on their the stellar star mass. formation Abstract 2.22 Star forming galaxies at high redshift: news from Herschel structural evolution over the interval this interval with which totelescope, dynamically we calibrate have the assembled stellar the mass largest scale. library Using of new spectra red-sensitive of CCDs spheroidsmass. in at To LRIS maintain at continuity with the the Keck Abstract Many recent observations have established the presence of a substantial population of quiescent galaxies at Redshifts 1 and 2 2.21 Investigating the Rapid Growth of Compact Massive Galaxies Between less than 2 Gyr. Ito will quantitatively also assess discuss the results role from that a accretion high-resolution of imaging low-mass systems campaign may using have laser in guide driving star this adapative rapid optics growth. Galaxy Formation, Durham, Poster Programme m, the µ 9000 galaxies with ∼ Durham University Leiden Observatory . At wavelengths, 24–70 5 . 15% of spiral galaxies show an excess in = 2 ∼ z Prof Tom Shanks [email protected] Mrs Maryam Shirazi [email protected] Max Planck Institute for Astronomy (MPIA) m and to at least µ 128 Mr Kasper Schmidt [email protected] emission-line images from the grism spectra of the individual galaxies, we α m observations, also fits the Herschel/BLAST number counts and redshift distributions at 250–500 µ 60% of all star formation took place. Here we present first results on the spatial extent of the star formation across the COSMOS, GOODS, Hubble UDF, UKIDSS/UDS and AEGIS fields. This redshift range probes the ∼ 5 . 3 < z < m. A significant AGN contribution would also immediately improve the prospects for fitting the Herschel/SCUBA source m and longer Herschel wavelengths, the model fails, with our model of normal galaxies accounting for only a few percent of Abstract We present the results from NIRat IFU z= spectroscopic 2.73, study using of the SINFONIdynamical 8 on status o’clock VLT. and arc, We recent a and study gravitationally on-going the lensed star Lyman physical formation Break properties activity. Galaxy of its interstellar medium, its chemical make-up, its 2.26 Near-IR Integral Field Unit spectroscopic study of the 8 o’clock arc We show that optically defined PLElocal models, galaxy where dust templates, reradiates fit absorbed galaxy optical counts light and into infrared colours spectra out composed to of 8 Abstract µ counts in the context of the LCDM cosmology. 2.25 Extending Pure Luminosity Evolution Models to Herschel Wavelengths 1 epoch where show how this can be mappedof back star to forming the regions. (continuum) near infrared image of the sources, yielding the spatial distribution model is able to reproduce themid-IR observed flux source due counts to with a reasonable warmerµ success dust if component and a higher SFR,sources in in these line bands. with However, observations we show of thatfit local a to starburst PLE model X-ray galaxies. of and obscured At AGN, 850 160 which we have previously shown to give a good in some of these galaxies. By extracting the H Abstract The ongoing Hubble legacy treasury program 3D-HST is taking near infrared (WFC3) grism spectra of 2.24 The Distribution of Star Formation in High Redshift Galaxies Galaxy Formation, Durham, Poster Programme 7 2 and ∼ ∼ 1 z galaxy z 2 ∼ z ∼ , z 2 ). Our results 5 . ∼ 2 z 6–7 galaxies in the ∼ Leiden University ∼ for Leiden Observatory Leiden Observatory z are already in place for 46 . 0 = 0 − z hours of integration time using source with a H-band magnitude 2 and 7 33 ∼ . 0 z − Miss Renske Smit [email protected] , 47 . Mr Daniel Szomoru [email protected] 0 − Mr Jesse van de Sande [email protected] = remains a highly debated issue, and can only be solved 2 ) and smaller effective radius (factor median 5 . ∼ )) color profiles for these galaxies and show that most 1 r z . With our high S/N, we determine accurate stellar population g ∼ 129 80 − log . u = 1 )/∆( z 2 rest g ∼ − u z (∆( colors and lower Sérsic indices than quiescent galaxies. These correlations are very similar to . We find a large variety of galaxy morphologies, ranging from large, blue, disk-like galaxies to g 2 − ∼ u z ) quiescent galaxy at a redshift of ⊙ M 11 10 galaxies. This result is consistent with an “inside-out” scenario of galaxy growth. We find that the median color × 2 2 , respectively. Using structural parameters derived from surface brightness profiles we confirm that at ∼ ∼ 24. To put our results in context, we compare our findings with those for other highly magnified z ∼ = 0 massive galaxies at this early epoch. X-Shooter on the VLT, we obtainedsive a ( high signal to noise, high resolution, Ultra-Violet to Near-Infrared spectrum of a mas- The remarkable compactness of massive quiescent galaxies at properties and a stellar velocity dispersion.relation The found for stellar low-redshift and galaxies dynamical in the mass Sloanin are Digital SDSS, in Sky our good Survey. galaxy agreement, However, has and for a galaxies consistent with higher with similar velocity the dynamical dispersions masses (factor Abstract using X-Shooter 2.29 A precise stellar velocity dispersion of a compact massive galaxy at z=1.80 using kinematic measurements. Dynamicalsumptions masses regarding are the initial less mass uncertain function, metallicity compared and to photometric redshifts. stellar With masses, and do not rely on as- confirm the existence of massivevelocity dispersion quiescent is galaxies required if with these high galaxies stellar are to mass become densities, local early-type and galaxies. that evolution in both size and those at lower redshift, suggesting that the relations that give rise to the Hubble sequence at Abstract We use ultradeep HST WFC3/IR imaging ofsample the of HUDF to galaxies investigate at the rest-frame optical morphologies of a mass-selected 2.28 The Hubble sequence at compact, red, early-type galaxies. We derive rest-frame galaxies behind Abell 1703. This sample is a particularly large one – and includes one morphology correlates well with specificradii, star bluer formation rest-frame rate. At the same mass, star forming galaxies have larger effective Abstract How galaxies build up and evolve atwell-established early constraints times exist is on one how of this thestory build-up most - occurs fundamental from questions the in rest-frame build-up extragalactic UV astronomy. of studies,already an While stellar emerged equally mass for important - high part of redshift isgalaxies the galaxies far remain (like less essentially the well unknown. non-evolution understood.SFR of This density, specific is Although UV SFR), a a density, the major and few likely stellar gap notablefaint provide masses in sources results the our of at photons on knowledge lower high that the reionize redshift since luminosity stellar the ischallenges, lower universe. with mass we luminosity Spitzer, The have take galaxies only but advantage dominate way with of of the SpitzerHST gravitational obtaining one – lensing data is allowing on from for faced these galaxy detailed with stellar clusters serious population to S/N modelling. magnify limitations. Here the we To light apply surmount seen such these a with technique Spitzer to and study with a sample of lensed 2.27 Modelling the stellar populations of high redshift galaxies of literature. z galaxies in our samplepartly have be negative caused color by radial gradientsof variations such in that dust their content, they coresgradient point is are to fairly red. the constant existence with of Although redshift: older these stellar color populations gradients in the may centers Galaxy Formation, Durham, Poster Programme - 1 < 1 ∼ = 2 z z 7 Yale University - Leiden Observatory = 2 – is star formation in IR- z with infrared 1 2 - ∼ z , biases in SFR indicators, and the = 1 Dr David Wake [email protected] z = 1 z Steward Observatory, University of Arizona , unless the assembly of galaxies by mergers, or Dr Simone Weinmann [email protected] = 2 z 130 Dr Benjamin Weiner [email protected] where gas accreted earlier is consumed. We find that it is difficult to simulateously = 2 I will show how the relationship between galaxy stellar mass and mass has 1 z . = 0 Gyrs. By combing these measurements with the halo model of galaxy clustering I will demonstrate z 10 = 2 and results from modeling their stellar populations. z 2 ∼ z and the SDSS at 2 , as found by Gonzalez et al. (2010), Stark et al. (2009) and others, are puzzling in the context of current galaxy-formation models. Since the predictedtimescale specific for dark star matter formation decreases, accretion current rate semi-analyticalsignificantly models increases with and redshift. steeply SPH Despite towards simulations the predict earlier tentative thata nature time, the study of and sSFR of the their increases the observational implications. data, dynamical Using this the markedthat simplified conflict the semi-analytical with model sSFR theory presented plateau motivates by Neistein can & bea Weinmann reproduced (2010) time-dependence we of by show the non-trivial star modifications formation to efficiencyfollowed the and/or by feedback, standard which models. a makes These period star formation modifications around at include high redshift inefficient, 7 reproduce both the plateau and the presence of massive galaxies by Abstract The indications for a constant specific star-formation rate (sSFR) at a given stellar mass throughout the redshift range the strength of merger-induced bursts, is increased compared to standard models. 2.32 On the puzzling plateau in the specific star formation rate at Abstract As astronomers’ focus on galaxy evolution moves to higherare redshift, made faint galaxy difficult spectra in by the near-IR the becomebut atmosphere. important, but very Slitless sensitive spectroscopy and withComparison with HST’s of high WFC3-IR star provides multiplex formation spectra advantage. indicators that between are I H-alpha, low will far-IR, resolution and discuss [O results II] from at WFC3-IR grism surveys, including: i) 2.31 Measuring star formation and stellar populations at spectroscopy from HST implications for obscuration in star forming galaxies. ii) Measurements of diameters of the star forming region in Abstract Using measurements of the stellar mass dependent clustering from the NEWFIRM medium band surveys I and II at mass since 2.30 The changing relationship between galaxy stellar mass and dark matter halo z < changed over the last that the halos that are most efficient atclustering forming measurements stars move and to the lower halo halo massI model in find may more recent be that times. used the I to will stellarmassive also directly mass show galaxies link that assembly increasing such galaxies their rate at mass of different at galaxies epochs. the depends slowest Using strongly rate this over on method, this their period. stellar mass (or halo mass), with the most galaxies, using the spatial resolutionluminous of galaxies HST, centrally and concentrated thegalaxies or nature at spread of out IR-luminous in galaxies at a disk? iii) Continuum spectroscopy of passive and reddened Galaxy Formation, Durham, Poster Programme galaxies 500 Yale University University of Oxford , a higher redshift than has been probed 3 –3. We show evidence for a clear bimodal 5 . ∼ galaxies provide important insights into the galaxies using a pixel colour z Mrs Katherine Whitaker [email protected] Dr Stephen Wilkins [email protected] 3 = 0 - 3 1 - z 1 ∼ z ∼ z 131 Insitut d’Astrophysique Spatiale, CNRS & Université Paris-Sud XI . This scatter in color arises from the spread in ages of the quiescent galaxies, where we 2 Dr Niraj Welikala [email protected] ∼ z The ultraviolet luminosity can be usedticularly as useful a at robust very-high diagnostic redshift of wherefraction the the of ongoing rest-frame the star UV UV formation is continuum activity shiftedthen light in into only is galaxies. the represent reprocessed This lower observed by limits is optical/Near-IR. dust. on par- However,sic the some star Star intrinsic formation star formation rates formation rates of rate. galaxies inferred (e.g. While fromBalmer several combining decrement, the techniques UV etc.), observed exist measurements these UV for with are Far-IR, obtaining luminosity typically H-alpha thetive only luminosities intrin- accessible is corrected to to using moderate the correct redshifts the for observedempirically large UV found samples luminosity to of be using galaxies. sensitive observations One to of the alterna- aimed the degree of UV at dust continuum measuring extinction. slope the In which redshift this isI’ll work evolution both discuss I’ll theoretically and present in the and detail luminosity results the dependence of interpretation aalternative of collection of strategy the of for these constraining studies rest-frame colours the utilising UV fraction of galaxy continuum obscureddistribition formation star colours. (CSED) models. formation combined using with Further, In the the ocally addition, observed observed I’ll Cosmic UVto briefly spectral luminosity place energy discuss density strong an history. constraints on Combining these the two average observations fraction allow of us obscured star formation over Cosmic history. Abstract 2.35 Probing the Dust Obscuration of Star Forming Galaxies Over Cosmic History color distribution between quiescent and star-forming galaxiesso that persists far. to Additionally,galaxies we in measure the an NMBS out increase to see in both the quiescent red, intrinsic old galaxies scatter andconfirm of quiescent the blue, the quality younger rest-frame (post-starburst) of galaxies U–V the towardgalaxies NMBS colors higher using redshift.Finally, redshifts HST/WFC3 of we grism and massive, data stellar from quiescent population the parameters 3D-HST survey. of a sub-sample of these massive, quiescent We have performed a unique near-IR medium bandwidth surveyBand of Survey the (NMBS) AEGIS gives and COSMOS redshifts fields. accurate to The 1-2% NEWFIRM Medium- for 4000 galaxies at Abstract spectroscopy 2.34 Quiescent galaxies through cosmic time from (ultra-) low resolution NIR formation history of these objects.units While (as this has can been be done approachedunderlying in stellar using a populations, spatially potentially number resolved for of spectroscopy large studies), samples usingin of the integral the these colors field GOODS-VIMOS high-redshift of objects. survey subcomponents I whichtematic use of have effects approximately galaxies multi-band in extracting also ACS properties provide imaging of a resolved andrate) stellar way spectroscopic in populations individual to redshifts, (such pixels, as unveil in from their the order age, theirthe dust, to colors metallicity technique, using study and the including the star ’pixel-z’ those formation sys- method that (Welikalato arise et the from al. pixel differences 2008, colors. in 2009). The input Iones, systematic stellar analyse uncertainties pixel-by-pixel, systematics population in and in synthesis the their models derived stellararising distribution whose from population SEDs over model properties are the differences are fit can galaxy compared be to sampleof well the combining is constrained statistical the with characterised. optical the data available with I optical near-infrared data. show colors. I that also systematic examine uncertainties the systematic effects Abstract Spatially resolved studies of stellar populations and substructure in 2.33 Substructure and stellar populations in approach: systematics Galaxy Formation, Durham, Poster Programme 5 . = 1 MPE z decrease with 3 − Yale University are approximately 3 Mpc − 6 is one of the key results galaxies based on stellar − we achieve higher spatial [email protected] Dr Stijn Wuyts Mpc 3 2 10 2 5 ∼ ∼ × − 5 z z and lends support to theories of 10 z > 1 × 3 5 N > z > Swinburne University of Technology > observed with LGS-AO on Keck to obtain [email protected] Ms Rachel Bezanson 6 . . At higher redshift, we find that the number 11 < z < = 0 < 1 z ]) ⊙ M [ ∗ M ( Ms Emily Wisnioski [email protected] 132 in the WiggleZ Dark Energy Survey log 5 < . 8 . 9 galaxy kinematics revealing that even the most extreme SFRs at = 1 α s decreases, but the number of high dispersion galaxies is constant or even z / , whereas the dispersions of galaxies 5 . km 1 is very similar to the VDF at 5 − . spatial emission which extends over 6–10 kpc in 4 of the galaxies. We find evidence 0 0 200 α ∼ ∼ < and stellar mass z z , velocity dispersions appear to have been even at high redshift. The analysis encompasses 5 . 3 1 − − from 2 7 Mpc . . 1 4 − = 1 emission. With comparable intrinsic luminosities to IFU samples at ∼ 10 z α × 5 redshift by a factor of constant. Above a number of sources of uncertainty and we suggest several avenues for further calibration of inferred velocity dispersion. resolution and comparable signal-to-noise in a muchcomponents, shorter or exposure ‘clumps’ time. within the We H detectof multiple ordered emission, 1–2 orbital kpc motion size in sub- indicative the that majority a of different galaxies mode of as star would formation be could found be in feeding unstable gas gaseous to galaxies disks. at This unique data set is density of galaxies with dispersions increases. At fixed cumulative number density, the velocity dispersions of galaxies with Abstract The distribution of the stellar velocity dispersionslocally of using galaxies, or dynamical the measurements Velocity from Dispersionmodels Function the (VDF) for Sloan has Digital galaxy been measured Sky formation Survey. andvelocity The even dispersion evolution measurements cosmology. of of the Direct manyVDF VDF thousands studies places using of of constraints photometric galaxies. the on data VDF In frommeasured are this the central paper difficult UDS we velocity at present and dispersion high a NMBSindex redshift and study of COSMOS as the galaxies of in Surveys. they velocity the the require dispersion evolution SDSS. We We ofa inferred apply begin function the this by of by relation the redshift. to calibrating galaxies stellar The in the VDF mass, the relation photometric at effective surveys between and radius examine and the inferred Sersic VDF as spatially resolved H cold dense gas flows from the IGM. population modeling on a pixel-by-pixel basisresolved of stellar the populations 7-band vary ACS as +modeling WFC3 a also imaging improves function in estimates of of GOODS-South. position integrated We stellar in describe population the how properties, SFR-mass the such diagram, as the and galaxy-averaged demonstrate stellar how age. resolved SED 3.1 The Evolution of the Velocity Dispersion Function The existence of a fairly tight relation between star formation rate and stellar mass out to Abstract 2.37 A resolved view on the SFR-mass diagram at appear to take place inEnergy disks Survey rather with than mergers. The sample consists of 13 star-forming galaxies from the WiggleZ Dark from extragalactic surveys in recentmechanisms years. driving star This formation. relation In has particular, the profoundprovides scatter implications and important zeropoint clues on evolution on of our star this understanding main formation sequence of histories,refine of which the star the formation proceed dominant measurement predominantly of in a the fairlycross-calibrated SFR-mass continuous SFR relation fashion. indicators including and Here, Herschel/PACS add we photometry a frommass the new, diagram. PEP resolved survey, dimension. and We use it We thensurveys to first exploit construct to establish the high-resolution quantify SFR- a ACS variations set and of inand WFC3 carefully galaxy mode data of structure star from along formation. the and We COSMOS, across present GOODS, the resolved ERS2, stellar main mass, and sequence, stellar CANDELS revealing age a and SFR link maps between of the level Abstract I will present the results from a new sample of H 2.36 Clumpy Star-formation at Galaxy Formation, Durham, Poster Programme 24 ∼ INAF a wavelength that over an area of Durham University µm 5 . 22 Embry-Riddle University < Dr Alexander Fritz [email protected] AB I [email protected] Prof Shaun Cole [email protected] Prof Nick Devereux images of the Extended Groth Strip. The classifica- gives magnitudes at rest-frame 2.2- 133 Hubble Space Telescope (Guzzo et al. 2011). Based on 5-band accurate photometry from the CFHTLS, 2 . Spitzer Space Telescope 1 < z < 5 . 0 . This is the largest galaxy redshift survey ever performed at ESO and is comparable to the 2dF Galaxy Redshift Survey 1. Complementary imaging with the 2 ∼ closely reflects stellar mass. Theand combined compared data to allow local the ones. luminosity functioncompare Some to the morphological be observed types computed evolution show for with evidence each that forwhich morphological predicted significant will type by be evolution presented the whereas at GALFORM others the semi-analytic do meeting. galaxy not. evolution We model, the results of Abstract The VIMOS Public Extragalactic Redshiftdistribution Survey of (VIPERS) galaxies and is to an measure ongoing itsvolume statistical ESO of properties Large and the related Program Universe cosmological to parameters at map over an in unprecedented detail the spatial tions are directly comparable to thosespectroscopic used and for photometric nearby redshifts galaxies and allow arez us not to based define on complete colors samples or of other galaxies proxies. of Ground-based various morphological types at 3.4 First results from the VIMOS Public Extragalactic Redshift Survey VIPERS is using VIMOS at the VLT to measure 100,000 redshifts for galaxies down to We have visually classified galaxies in existing Abstract 3.3 Evolution of the Luminosity Function Since z = 1 Abstract We present a Maximum Likelihoodfunction method (LF) of and jointly the overdensity determining,is as from to a a develop function a galaxy of simple redshift algorithm redshift.works catalogue, to by both One produce cloning utility random the each (unclustered) of luminosity galaxy versions thissolution. in of approach, the Each the original which of original catalogue these we galaxy with cloned focus catalogue.volume, galaxies the on The is number taking in algorithm then of this account assigned clones paper, a of determined randomThe by the redshift resulting the survey uniformly random Maximum distributed magnitude Likelihood catalogues, over limit(s) which thethe accessible and can information available survey be optionally in employed the both original in luminosity catalogueredshift traditional distribution. and and hence estimates They are number are of superior particular density suited galaxy to to simply clustering,galaxy evolution. studies fitting of in make a the the functional dependence fuller of form random use galaxy to catalogue clustering the of onThe has observed galaxy derivation the properties of as the same each joint list overdensity and of LFto properties estimator the reveals as standard the were 1/Vmax limit in measured LF which estimate. for the Namelyoverdensity. Maximum the Likelihood when galaxies The estimate one reduces in new makes ML the the prior estimator genuine assumption cana catalogue. that be density the viewed corrected are as no Vdc,max. a fluctuations in generalization the of radial the 1/Vmax estimate in which Vmax is replaced by 3.2 Random Galaxy catalogues in the local Universe.VISTA, There SWIRE, is VLA, XMM-LSS. a great synergy withWe other will surveys give at an update various onconstruct wavelengths, the the such redshift current space as status two-point e.g. of correlation function thefirst and project GALEX, give detailed and constraints UKIDSS, spatial on will clustering the present bias of the parameter.the galaxies first Further, observed between results we fields. 0.5 dz [email protected] Mr Samuel Leitner Prof Nicolas Lehner [email protected] based on recent observations from the Cosmic Origins 1 z < 135 . We use narrow-band imaging to identify galaxies with extremely high emission-line equivalent widths. These 8 . 0 ∼ z emission lines fall outside therarity narrow-band of such filter galaxies, and we cover produce a a wide volume significant by excess probing a in large the redshift range broad-band ( imaging. Due to the that are thought to be responsiblepoor for metallicities cosmic (less reionization. than 0.1 These solar, young for galaxiesthat example) are and formed, often high searching star characterized formation. for by extremely While lowerthe it metal redshift states is important of analogs to their will find ISM, the permit and earliestat kinematics. detailed galaxies I studies will of present their a new morphologies, survey gas that metallicities we are and conducting to search for metal-poor galaxies fields, COSMOS, Subaru Deep Field, andthan Subaru-XMM past Deep surveys Survey. (Hu This et surveylow al.). is metallicities I by a detecting couple will [O of also III] orders discuss 4363. of future magnitude follow-up larger spectroscopy with Keck, which is crucial to confirm their Identifying and studying galaxiesmodels in of their galaxy earliest formation. stages Future of facilities formation and observatories is aim an to important search step at towards testing cosmological Abstract 3.10 A Search for Young Metal-poor Galaxies at Intermediate Redshifts Abstract We attempt to compile aWe concordant first picture constrain the of star the formation history assemblyevolution of and of these SFGs evolution galaxies as by of they adopting evolve actively a in simple, mass starobservations data-driven and forming from redshift, framework, Herschel and galaxies which applying traces and (SFGs) that the VLA-COSMOS framework today. toanalysis analysis. recent of multi-epoch the We star fossil formation then record rate confront of SDSS thesetwo Data constraints methods Release with for 7. understanding VESPA’s Finally, the archaeological we growth will of highlight and SFGs, parse which outstanding are differences now between systematic the in nature and persist down to 3.9 Tracing the Assembly of Present-Day Star Forming Galaxies Abstract Lyman limit systems are clearly seenThey to therefore trace provide phenomena a associated path with forcan the studying circulation yield the of metallicity a matter distribution measure into of andshow of circumgalactic out and gas the of discuss in galaxies. covering the an factor distribution “unbiased” manner. of for the This infalling metallicity streams of LLS vs. at outflowing winds as a function of redshift. Here we 3.8 Probing Galactic Outflows and Infall with Lyman Limit Systems at Spectrograph. Galaxy Formation, Durham, Poster Programme 221 − 143 ∼ , with effective 1 e σ ∼ z University of Florida Most Compact and ICG, University of Portsmouth targeted in the Baryon Oscillation 7 . 0 = 1 z . The spectra are best fitted by SSP models ⊙ < z < M 3 . 11 0 10 · is able to select a sub-sample of BOSS galaxies with Mr Jesus Martinez-Manso [email protected]fl.edu 4 Dr Karen Masters [email protected] 35 ; ii) passive luminosity fading combined with mass/size − . 2 2 . = 1 > z = 1 136 ⋆ M % of the early-type BOSS galaxies are unresolved multiple systems in the SDSS 4 ± . If confirmed for other similar galaxies, this result would argue against the strong 7 23 ∼ kpc and photometric stellar masses 4 . 2 − 5 . = 0 %) possess an early-type morphology (elliptical or lenticular), while the remainder have a late-type (spiral disc) e 6 R ± 90% early-type morphology and thus more comparable to the earlier Luminous Red Galaxy (LRG) samples of SDSS-I/II. 74 with approximately 1 Gyr ofkm/s, age yielding dynamical and masses solar up metallicity. toevolution 10 of times We smaller these find than galaxies these their and stellar galaxies findPlane mass have that relations. estimates. this velocity When We mechanism dynamical dispersions model by masses the itself are passiveminor is considered, luminosity mergers inconsistent we show with is that the consistent a local with combinationbeing mass-size of both and overestimated fading Fundamental local by and relations. a size/mass evolution factor via mass-size We of evolution conclude proposed that: for these i) extreme the objects since stellar masses of these galaxies are likely > The remaining 10% of galaxies above thisfound (g-i) cut at have lower a redshift. late-type morphology We and find may that be analogous to the ”passive spirals” imaging. We estimate thatrepresent at a significant least ”dry 50% merger” of fraction, mostof these likely BOSS multiples dominated galaxies by are which minor likely mergers. we real find Westatistical compare to associations correction the be and for SDSS systematically pipeline the not larger sizes difference. projection (byselection effects 40%) These criteria, than and details dependent those of may measured on the from their BOSSdistance HST science galaxies scale images, will applications. and and help provide expansion For users a rate example, ofdetails of the the of the target BOSS main selection data Universe goal may fine-tune to of become their percent-level BOSS important. precision is – to a measure point the where cosmic systematic effects due to the radii growth due to minor mergers cangalaxies. plausibly evolve our objects to match the properties of the local population of early-type Spectroscopic Survey (BOSS) usingCOSMic publicly Origins available Survey (COSMOS). Hubble Our sample Space (240 objects)of Telescope these provides galaxies a (HST) which unique were opportunity imaging, targeted to based and check solely the( on catalogues, visual stellar population morphology from modelling. We the find that themorphology. majority of This BOSS galaxies is as expectedslowly evolving from galaxies, the for goals use of asfor the cosmological galaxy BOSS probes, evolution while target studies. still selection obtaining criteria We a which show fair that aimed fraction a to of colour actively predominantly star cut select forming of galaxies (g-i) We study the morphology and size of the luminous and massive galaxies at Abstract 3.12 The Morphology of Galaxies in the Baryon Oscillation Spectroscopic Survey Abstract We present GTC/OSIRIS spectra of 4 of the most compact and massive early-type galaxies at redshift 3.11 Velocity Dispersions and Stellar Populations of the Massive ETG’s Galaxy Formation, Durham, Poster Programme ), 0.66 (Pa-beta) α Nagoya university 14,000 visually classified galaxies were able Mr Katsuhiro Murata [email protected] ∼ INAF - Astronomical Observatory of Bologna 23 AB magnitude from the COSMOS/ACS catalog Institute for Astronomy, University of Edinburgh < ) end of the H-alpha luminosity function. We present the early 1 137 [email protected] Dr Preethi Nair < z < 0 ( [email protected] Miss Salome Matos z ). Because the lines in the Pa series are essentially unaffected by dust, these could become an alternative to γ 20,000 equally detailed visual classifications from the zCOSMOS survey (Lilly et. al. 2007). In addition, I will present The role of bars inin driving the secular local evolution universe, of theirconsistent galaxies evolution results. is with Recently, redshift, still Nair and highly & their debated. Abraham role (2010) Studies in using on building their the bulges sample and fraction of triggering of AGN barred have galaxies not yielded Abstract 3.15 Secular Evolution of Galaxies and 0.95 (Pa results from a spectroscopic campaign usingemitters, the and AAOmega Paschen instrument luminosity functions to derived confirm using the these identifications and of photometric these redshifts. non-H-alpha (Leauthaud et al. 2006).Then,chain galaxy we candidates checked in the their COSMOS morphology field.properties. by We would eyeball like to inspection. show you Consequently, some examples we of found the candidates almost and discuss 100 their to reconcile the disparity in∼ local bar fractions. Inresults this on work, the I impact of will bars extend on the the analysis metallicity evolution to of high-redshift, galaxies using and a their sample correlations with of AGN activity. H-alpha and be used as SFcompare with tracers. the Hence, existing luminosity we functions aimare derived at expected from to obtaining H-alpha yield the some within constraints first-ever HiZELS. on derived Moreover, the low these SF Pa rate emitting history galaxies from Pa emitters and Abstract Galaxies with unusual morphologicalChain structures galaxies have are one been of discoveredwithout such by examples bulges. with recent They unusual deep are morphology. and1995). first They high Since discovered are then, resolution by characterized approximately the by observations. 200 elongated HubbleBergh chain et knotty galaxies space al. have structures telescope been 1996, (HST) Elmegreen discovered thanks et withand al. to the formation HST 2004, its have 2005, at high been 2006, high proposed resolution Miley redshift (Noguchiorigin et (Cowie universe is 1998, al. (van et still Taniguchi 2006). den al. controversial & Although and Shioya some remains 2001,Hence models mysterious. it Immeli to This is explain et is crucial their al. to partly structures examine because 2004, much ofchain larger Dekel the galaxies sample et based small of on al. chain sample the galaxies size HST 2009), for used ACS further their instudies. i-band understanding. previous data For We in studies. this the selected purpose, COSMOS geometrically we field, searched which thin is galaxies nearly in 10 times appearance larger with than I those of previous 3.14 Chain galaxies in the COSMOS field Abstract The study of the star formationunderstanding history of of the galaxy Universe formation and of andwell the evolution, calibrated star however SF formation tracer the rate in as star the a formation nearbyLine function (SF) Universe, of Survey) although, epoch indicators has like is are found, all crucial in numerous. Balmer for its lines,alpha the H-alpha narrow-band is emitting dust is K galaxies obscured. filter, a and HiZELS a among (High-z wide-range those Emission of some line are emitters, likely of Paschen which (Pa) about line half emitters are at potential redshifts non-H- 0.13 (Pa 3.13 Paschen Star Formation History of the Universe Galaxy Formation, Durham, Poster Programme m µ . We used a 9 . 0 Leiden Observatory < z < University of Pittsburgh 6 . and the Role of 0 9 . 0 Instituto de Astronomia-a-UNAM 0.8. For halos hosting early-type galax- < Dr Shannon Patel [email protected] < z < 6 . 0 Prof Jeffrey Newman [email protected] . We find that the decline in the SSFR-density relation at 0 mag. We utilized a stellar mass-limited sample of 986 galaxies Aldo Rodriguez-Puebla [email protected] 138 ∼ 3 . z 23 < AB z . We find approximately the same magnitude of decline in SSFR even after removing the 4 for galaxies with ∼ to conduct our main analysis. With three different SFR indicators, (1) Spitzer MIPS 24 01 . ⊙ 0 M ∼ ) 10 z 10 × is driven by both a combination of declining SFRs of star forming galaxies (SFGs) as well as a changing mix 8 /(1 + . z 9 1 . σ 0 M > < z < 6 . Abstract The baryon mass-to-halo mass ratiothe (baryon key ingredients fraction) of required the togalaxies galaxy by match formation matching the the and corresponding observed evolution cumulative observed processes. baryon galaxyhalo baryon mass mass We mass function function function infer to (HMF). their this encloses For corresponding baryon halos all cumulative hostingmass fraction late-type for function galaxies, late- as we and subtract well from early-type as the those total HMF halos the with observed a group/cluster central major merger since redshift 3.18 Connecting the galaxy stellar/baryon mass function and galaxy scaling laws ies, we used the complementgalaxy of population models this in function order to to study thedominated its galaxies. total. consistency with structural Finally, and the dynamical scaling resulting relations baryon for fractions disk and were bulge used as an input in We study the star formation rates (SFRs) of galaxies as a function of local galaxy density at Abstract 3.17 The Star Formation Rate-DensityStar Relation Forming at Galaxies Abstract The recently completed DEEP2of and galaxies DEEP3 within Galaxy the RedshiftCANDELS context Surveys imaging of provide in the their unique Extended underlying datasets Grothrecent dark Strip. for results on In matter studying the this halos. the relationships talk, between evolution I starfound. will These formation summarize history, datasets AGN the activity, current will and status soon the of environments be the in surveys which strengthened and galaxies are via present deep 3.16 Studying Galaxy Evolution with DEEP2 and DEEP3 low-dispersion prism in IMACS onprecision the of 6.5 m Baade (Magellan I) telescope to obtain spectra and measured redshifts to a imaging, (2) SED fitting, and (3)low-density [OII]3727 field emission, to we the find cores the ofmass. median groups specific For and SFR the a (SSFR) SED rich and and cluster.SFRs, SFR [OII] the to This decline based decline result is SFRs, from holds a the the even factor declinesample of when of in looking galaxies SSFR at near is galaxies the roughly at(SF) cluster. an a order activity fixed Galaxies of stellar than in magnitude groups galaxies while and in0 for a the the cluster field, MIPS at based these as redshifts is therefore the have case lower at star formation of SFGs and quiescent galaxies. above Galaxy Formation, Durham, Poster Programme 1 < . The general = 0 z Indiana University to kpc) than other green- 5 . 1 40 ∼ z D > 4000 late-type disk galaxies from Royal Military College of Canada ∼ Swinburne University of Technology Dr Samir Salim [email protected] 1 . 0 Dr Chiara Tonini [email protected] Dr Kristine Spekkens [email protected] ∼ z 139 times smaller than that of the halo spin parameters produced in ), and were thus limited by its 5” FWHM. Poor UV resolution left 7 1 . 0 ∼ ∼ z ) ETGs shows clear evidence of extended SF, usually in the form of wide ⊙ M 10 10 × 5 ∼ /yr) of star formation that causes strong excess in the UV flux, yet leaves the optical colors red. Many of these studies ⊙ Brightest Cluster Galaxies (BCGs) are the most luminous and massive galaxies observed from Abstract 3.21 The evolution of brightest cluster galaxies the SFI++ catalogue, in order toand constrain size-rotation models velocity of (RV) galaxy relations, formation and andinstead show of evolution. that disk using We scale homogeneously lengths focus derived, produces on significantly inclination-corrected theSFI++ tighter isophotal size-luminosity RL relations radii than relation (RL) previously is reported. 2.5–4 times In particular, smallerstems the than from scatter found the in for reliability the other of large measured galaxycorrelated isophotal samples: measurement radii errors we suggest relative demonstrate that to that the this disk intrinsicthe improvement scale scatter small lengths. in the intrinsic Detailed RL scatter error relation of budgets isof independent that the disk of account SFI++ spin luminosity. for RL parameters Combining allowed relation by withcosmological the simulations. a data Unless simple is angular model momentum at redistribution for least insuggest, disk late-type this disks galaxy discrepancy is formation, more implies effective we that than findthan current the cosmology models that halos predicts. the hosting range Sc galaxies have a much narrower distribution of spin parameters consensus for these objects, mainlymassive. based Recently, on Collins SED-fitting et al. techniques, (Nature, isgalaxies, 2009) the that main claimed they cause that residing hierarchical are in models their old cannot earlythe and reproduce fast Croton assembly the et passively and al. observables evolving, late of (2006) passive and these model, evolution. based very (2005). We on studied the While the Millennium it properties simulation, is of equipped true BCGs with that in a modelnonetheless photometric BCGs model the are based not evolution on passively Maraston of evolving and colors formthese most and objects of luminosity theirs as stars correctly “red over reproduces a & widecomplete. the dead” range data. of is epochs, not This the suggests only that viable the option, interpretation and of that our understanding of these systems is far from being other possibilities for UV excessHST/ACS open, images of such optically as quiescent early-type the galaxiesof old with strong these populations UV moderately or excess. an massive The new AGN. ( images We show present that three-quarters high-resolution far-ultraviolet Abstract We derive scaling relations between the sizes, luminosities, and rotation velocities of Hosting Sc Galaxies 3.20 Size Does Matter: the SFI++ Size-Luminosity Relation and the Spins of Halos M were based on GALEX imaging of SDSS galaxies ( or concentric UV rings.valley UV-excess galaxies, ETGs which have argues on for“rejuvenated” average an Possible less rejuvenation external dust mechanisms origin include and for minor largeraccretion. gas-rich the UV mergers Further gas and sizes details that intergalactic are ( is medium given (“cosmic in driving web”) Salim the & SF. Rich Thus, (2011). most of these galaxies appear Abstract In recent years a significant fraction of early-type galaxies (ETGs) in the local universe was found to exhibit low levels ( 3.19 Rejuvenated Early-type Galaxies at Galaxy Formation, Durham, Poster Programme Max Planck Gesselschaft Kapteyn Astronomical Institute Institute for Astronomy, University of Vienna [email protected] Dr David Wilman 140 Mr Oscar Antuñano Vaquero [email protected] [email protected] Prof Bodo Ziegler solar mass haloes in which stripping of the hot gas associated to a galaxy is 13 10 ≥ solar mass haloes, compatible with expectations of bulge growth in mergers; S0s and passive disk galaxies 13 10 ≥ . We place constraints on evolution utilizing a variety of physical prescriptions applied to two different semi-analytic 0 ∼ Abstract I compare the weak lensingfrom signal, OWLS scaling hydrodynamical simulations relations that and have the dark-matter sameWe fractions einstein do mass of the and 22 comparison effective for radius SLACS different as strong galaxy the formationthe observed lenses scenarios, strong different with lenses. and scenarios. halos find a taken We similar complement weak lensingfor this signal which with to the the observational observed study limits one of for aremotivated their now galaxy-formation scaling becoming models relations (OWLS) available. and and inner a Our dark-mattercuss well-selected study mass the sample is fractions implications of the observed of first strong our lensingand detailed study galaxies in comparison on (SLACS). particular between I galaxy on physically dis- studies formation of theories their (i.e. stellar and cooling, dark-matter feedback, mass etc) distributions. of massive early-type galaxies 4.1 Lensing twins: probing the physics of galaxy formation with SLACS & OWLS We present results of ourRXJ1347.5-1145 ongoing at photometric z=0.45. and spectroscopic We campaign useVIMOS centered VLT photometric spectroscopy on redshifts to the identify derived and most from characterize X-ray structures ugriz9ks around luminous imaging this CFHT cluster: cluster to MEGACAM on study a photometry the scale together star-formation of 20x20towards status with Mpc. of higher We cluster use densities, members. GALEX We but findGALEX the that selected star-forming the star-forming blue galaxies galaxies and have are star-forming similar fractions atigating properties decline the constant at environmental all fraction effects environments, of within suggesting a the theof fast cluster, the blue transformation. optically blue population. Inves- selected fraction groups with Furthermore, andby galaxy the the the density cluster field, for galaxy we the population. find first little two or types no of correlation environment. Most of the environmental signal is carried Abstract 3.23 The Cosmic Web and galaxy evolution around the most X-ray luminous cluster Abstract The history of a galaxy isformation encoded of in a its disk, morphology: withina the which angular bulge; stars momentum and and form; the dissipative presence mergers propertieshistory or of of of lack galaxies gas a of and leads a galaxy to tidal gas is the interactionsthe disk also potential randomize drives encoded well stellar the (the in orbits, level centre its forming of ofbe environment: disk the stripped main star sub-halos in halo) formation and a in and their dense which (apparently)evolution, surrounding galaxies they spiral we medium, live; rarely features. examine found and merge, the gas only The except halo disks in atz and and massive the the stellar haloes. hot bottom mass gas To of dependence which distinguish of feedsmodels the morphology them and mechanisms separately can compared driving for only galaxy to central a andcentre local satellite of SDSS-RC3 galaxies matched at sample. We find ellipticals primarily in massive galaxies, and at the 3.22 The hierarchical origins of observed galaxy morphology are created via two independentfeedback, channels: and as as central satellite galaxies, galaxies withprobably in responsible star for formation the suppressed suppression. possibly as a result of AGN Galaxy Formation, Durham, Poster Programme 0.1. From this ∼ University of Victoria 1 cannot be explained fully by pure 2 magnitudes fainter in comparison ∼ ∼ University of California, Santa Cruz Ms Kaushala Bandara [email protected] 1.1924 with a median redshift of z = 0.6053. Lensing ≤ z [email protected] Mr Jacob Arnold ≤ Institute of Astro- and Particle Physics, Innsbruck, Austria 141 1. ∼ 1 respectively. We compare the luminosity-size relation of the SLACS disk galaxy Dr Asmus Boehm [email protected] ∼ 250 disk galaxies at redshifts up to z=1 with Very Large Telescope spectroscopy and > 1.0 kpc and n ∼ 0.5. We will present first results of this project which aims at a better understanding of the interplay ∼ > z < 2.5) to an unprecedented local galaxy sample, which consists of 670,131 SDSS galaxies at z ≤ Hubble Space Telescope imaging.and We total use masses; we spatially also resolved investigate rotationconstant disk over sizes, curves the stellar to population past derive properties 8 etc. Gyr, maximumhand, favoring The rotation a the ratio velocities HIERARCHICAL between mean buildup Vmax stellar stellar of and mass-to-light the totalthe dark mass ratios mean matter is stellar evolve halos ages more the are strongly disks lower for resideevolution in low-mass in. of the galaxies the On than low-mass stellar the for galaxies populations other high-mass (aka than galaxies.paign, ”downsizing”), in This possibly we points high-mass due took to galaxies to an very supernova and ANTI-HIERARCHICAL deep feedback.mean spectra In redshift a of recent disks observational at cam- the extremes of the galaxy mass function: sub-M* and super-M* spirals at a We have constructed a data set of Abstract between galaxy mass and i)utilize the the evolution correlation between of Vmax scaling and relations central like velocity dispersion the to Tully-Fisher study ii) bulge star growth in formation spirals history. since z=1. We will also 4.4 Kinematics, structure and stellar populations of disks since z=1 Abstract We utilize the advantages of gravitationalLens ACS lensing (SLACS) to Survey analyze that detailed span properties a of redshift 62 range strongly of lensed 0.1965 galaxies in the Sloan 4.3 Utilizing nature’s telescope to resolve intermediate and high redshift galaxies Abstract We present the wide-field kinematic andcuss metallicity these structure results of in nearby the early-typeassembly context galaxy paradigm of bulges is and inside-out/two-phase the stellar galaxy ability halos, of formationearly-type and idealized models. merger dis- galaxies. simulations A to While key broadly these success reproduceadvances comparisons of the in kinematic have the properties technology hierarchical generally of and mass been observed observing relegatedcases. methods to Here, are we within now use the an extending central extensivetary this dataset half-light nebulae that baseline and radius, includes by wide-field deep recent multi-band nearly spectroscopy photometry. of aneffective We integrated order find radii, stellar-light, that of globular contrary some clusters, magnitude to rotational plane- general in profiles expectations sharplyargue some decrease for that beyond major a these merger couple observations remnants, are asgalaxies well well form as early explained in large by a scale violent a metallicity dissipative two-phase gradients. phase formation followed We by scenario the where gradual assembly the of inner the outer regions parts of via minor early-type mergers. 4.2 Kinematic Signatures of Two-Phase Galaxy Formation sample (n magnification allows us to probe the propertiesto of direct a galaxy galaxy imaging population surveys. that The islines SLACS typically in lens the systems SDSS were spectra initially and selected thesemeasure systems based have on the been the rest-frame imaged presence with B-band of HST-ACS multiple luminosities, inSLACS emission the sizes lensed broad and galaxies I-band, show which Sersic a allows indices us primarily of to compact,tions reliably “disk”-like the corresponding population lensed to with galaxies. the peaks The of the derived size properties and of Sersic index the distribu- comparison, we find evidence that thesize evolution evolution of but the must luminosity-size relation bemoderate since caused size-growth. z by Our a observations size-dependent are luminosity consistentof evolution with disk previous or galaxy observational luminosity-size a and relation combination theoretical since of studies z luminosity of the evolution evolution and Galaxy Formation, Durham, Poster Programme Swinburne University Instituto Astrofisica de Canarias Prof Duncan Forbes [email protected] Kasi Astronomy and Space Science Institute (KASI) G can be used to study the structure of galaxy disks in 4 G; Sheth et al. 2010, PASP, 122, 1397) aims to obtain space- 4 [email protected] Miss Anna Ferre-Mateu 142 Dr Sebastien Comeron [email protected] 50) (Ferre-Mateu et al. in prep). This data allowed us to explore the star formation histories > m imaging of 2331 galaxies located at a distance smaller than 40 Mpc. As the mid-infrared traces µ m and 4.5 µ 15 effective radii. From such data we have detected the transition radius from a dissipative to accretive-dominated ∼ I review the results of ‘near-field cosmology’ studiestrace using major the star globular formation cluster events (GCs) over systems all ofStarting epochs, nearby with are massive relatively galaxies. the robust Milky GCs and Way, offer I a discussFrom unique the probe our relative of survey contributions the of outer of in-situ halos early-type of vsto galaxies. galaxies accreted GCs with and the the Subaru growth of andhalo. the Keck stellar Our telescopes, halo. data I support present a picture metallicitieshierarchical in which accretion which of probe galaxies low halos grow mass from out galaxies a into compact the ‘seed’ massive at red high sequence redshift galaxies (akin to we ‘red see nuggets’) today. via the Abstract 4.7 Massive Galaxy Formation as Revealed by their Globular Cluster Systems edge-on galaxies in a more accurate way thana in thick previous studies. disk. Most, In if not most all,of models disk the galaxies thick galaxy. have disks a We thin are (classical) will thought diskon present and to galaxies. the be results In a this of necessary study a consequence we studylikely have of to of fitted the yield the one-dimensional more disc thick luminosity accurate formation profiles results disk than and/or with properties theaverage physically evolution in rather more motivated a ad-hoc massive functions, functions large than which used sample previously are in of previous reported, studies.We carefully and will selected that, We discuss find typically, edge- that the the thick implications thin disks this and are on result the has thick on disk have galaxy a formation similar models mass and amount. on the missing baryon problem. of these galaxies with accuracy, finding that alltions the (having galaxies at in least our a sample contribution have of verymassive 70% tiny of or galaxies young none which fraction populations of are in old light). found stellar This to popula- in is be mass unseen typically or in all old, in previous light while known of we normal-sized mass, size old find and stars. that age for of We the 4 think massive ofthe that compact our early galaxies nearby found mechanisms galaxies compact at of there massive high-z. the is galaxies These formation no are closer of contribution objects almost massive could either perfect galaxies open counterparts the in possibility in unprecedented to terms detailed. explore of based deep 3.6 well stellar mass distribution and is not much affected by dust, the S Abstract The discovery that massivetionized galaxies our in understanding of the the early assembly offraction universe these of objects. were these compact Some more massive model objects compact renditions in predictducted than the the in nearby presence present order universe. of to day a Following find non-negligible such counterparts such expectations, relicsmasses has several from works and revolu- the have early sizes been universe con- similar in to ourof vicinity. those these found So objects far, at revealed only high that a redshifts tiny theythe fraction has were stellar of been surprisingly populations, nearby the younger detected. galaxies kinematical than which and Preliminary expected. thewith analysis morphological In high of properties this quality of the spectra talk seven (S/N stellar I of will population these present nearby compact a massive detailed galaxies analysis of Local Universe 4.6 Young Ages and other intriguing properties of Compact Massive Galaxies in the Abstract The ongoing Spitzer Survey of Stellar Structure in Galaxies (S 4.5 Thick disks: the lair of missing baryons? Galaxy Formation, Durham, Poster Programme MPIA Lowell Observatory Univ. of Nottingham Miss Vesselina Kalinova [email protected] [email protected] Dr Boris Haeussler [email protected] Dr Kimberly Herrmann 143 Abstract The mass of a galaxyinfer by is constructing the dynamical most models important thatfollows fit parameter after the to subtracting motion the understand of luminous the itsdistribution matter stars structure of and inferred and a gas from evolution. sample in colors the of and/or galaxy. 18field The spectra. spiral The spectrograph total Here, galaxies, dark SAURON mass using we matter (Ganda we two-dimensional content focus et can then stellar oncomponents, and and al. measuring compare gas the them kinematics 2006). mass with obtained structural and with Weto stellar the dynamically PMAS/PPAK population integral- properties. integral-field decompose The spectroscopic these developed data Sb/c/d techniquesIntegral will of Field galaxies be Area into applied survey (CALIFA). bulge The 600 and resultsstars nearby on disk and the galaxies gas kinematic being to mass distribution help obtained will understand as be the connected part evolution with of of properties galaxies of the the from Calar the Alto blue cloud Legacy to the red sequence. 4.10 Dynamical bulge-disk decomposition of spiral galaxies Recently it has beenminority, well where shown the that light there fallsexponential are off to with three a a break different single radius surface and exponential;shallow brightness then exponential (II) falls profile beyond truncated, off the types the more break majority, in steeply;characteristic radius. where spiral color and the trend (III) Additionally, galaxies: with light anti-truncated, Bakos, respect where falls (I) Trujillo, to theperhaps off & the the a light with break Pohlen special falls location. one (2008) Type off II In showed with case: dwarf that aWe disk the each will more galaxies, light show type however, the profile has different there is color a is flat trends a ondisk for galaxies the fourth these and inside type four explore profile and which the types ramifications then is from of falls the afor off differences large this between exponentially multi-wavelength spirals research beyond photometric and study from the dwarfs. of the break We dwarf National radius. gratefully Science acknowledge funding Foundation (AST-0707563). Abstract 4.9 Surface Brightness Profile Breaks in Dwarf Galaxies Abstract Most galaxies are fundamentally multi-componentcomponents systems, often have comprising largely a independent spheroidal origins,constrain bulge models separating and of a their galaxy thin properties formation disk. providesto and As important allow evolution. these the information However, routine with current use whichin automated of to which methods this we are technique are not on sufficiently developingcomponents large developed an samples of accurate, of galaxies robust galaxies. imaged tooltried-and-tested for by In galaxy measuring large this fitting/decomposition techniques the talk multi-band (e.g. key we surveys. GALAPAGOS physical introduce &as quantities GALFIT) the routinely The to of produced MegaMorph fully primary the by utilise project, multi-band focus modern individual imaging, surveys,Using structural of both all our ground-based the work (e.g. available is GAMA/SDSS)in multi-colour the and terms information space-based extension of (e.g. in of physically-meaningful the CANDELS/HST). current parameters.parametric galaxy components fitting We to process will naturally enables also accountmodel much present for component, further more non-smooth and improvements, robust galaxy ensuring such decompositions features, thethese as quantifying optimisation the enhancements the is inclusion allows evidence both of us for robust non- and including todetail. computationally each examine efficient. the properties We will and demonstrate evolution how of galaxy components in previously unattainable multi-wavelength surveys 4.8 Measuring the physical properties of galaxy components in modern Galaxy Formation, Durham, Poster Programme 2 × ∼ 3 and . 1 ESO − 3727 1 . λ 1 /[OII] 5007 λ 40% of the galaxies show signs of Dr Harald Kuntschner [email protected] vs. [OIII] ∼ Universidade do Vale do Paraíba β H 5007)/ λ was obtained, and a dynamical mass of 1 [OIII] yr) population, with the fraction of this population to − 8 [email protected] Dr Angela Krabbe 10 4959+ × λ 144 1 ≤ ), where we compared the observed values with the ones obtained [OIII] 3727 λ 3727+ λ /[OII] 6584 =([OII] λ 23 R vs.[NII] survey (Kuntschner et al. 2010, MNRAS, 408, 97). Remarkably, , increasing outwards in the galaxy disc. On the other hand, the stellar population of AM 2322A is 3727 λ 5 870 SAURON λ /Fe] ratio compared to the main body of the galaxy. /[OII] α ). Spatially restricted cases of young stellar populations in circumnuclear regions can almost exclusively be linked within a radius of 4 kpc was estimated using this deprojected velocity. Asymmetries in the radial velocity field ⊙ 5007 Gyr observed over the full field-of-view covering about the half light radius are restricted to low mass systems ( ⊙ M λ 3 M 10 ≤ 10 10 10 [OIII] from photoionization models. Suchin gradients typical of isolated oxygen spiral abundanceinteraction-induced galaxies. gas are flows significantly from This flatter the metallicity outer for distribution parts this to is the pair interpreted centre of of as galaxies the the galaxy. than gradients having been destroyed by a contribution from a young stellar population.of The most extreme cases of post-starburst galaxies, with SSP-equivalent ages were detected for the companion,and very companion galaxies likely was due modelled using the numericalthe interaction N-body/hydrodynamical simulations, current between with the stage the galaxies. result of indicating thethe that The stellar-population system interaction components would between in be the both about main The galaxies was 90 companion analysed galaxy Myr using is after the dominated perigalacticum. stellar by population a The synthesis very code spatial young STARLIGHT. variation (t in the distribution of Abstract I will present the spatially resolvedgalaxies stellar from population the analysis of the absorption line strength maps for 48 nearby early-type 4.12 Spatially resolved star-formation in nearby early-type galaxies to the presence of star-formation in astellar thin, population. dusty disk/ring, The also seen flattened in componentsto the with near-UV be or disk-like mid-IR connected kinematics on to previously top ofdisks identified regions an in and older of underlying all rings distinct fast with stellar rotatorsmore increased populations. are massive shown metallicity structures with These preferentially extended range found disk-like kinematics, fromdepressed in which [ the are intermediate-mass observed young, fast to have still rotators, an star-forming increased to metallicity circumnuclear apparently andUsing mildly old radially averaged and stellar population gradientssystems, being we slow-rotators, find exhibit a the mass shallowest -petition between metallicity metallicity-gradient different gradients. relation star-formation where This and the assembly is scenarios mostmore interpreted following massive as equal a a mass general consequence trend mergers of of with diminishing thesigns increasing gas com- of fractions mass, recent and leading star-formation. to the most massive systems being devoid of ordered motion and the total flux at heterogeneous along the slit positionsusing observed. two Spatial diagnostic profiles diagrams of ( oxygen abundance in the gaseous phase were obtained × Abstract We present an observational studygen about abundances of the the impacts components of(AM2322B) of galaxy the with the interactions a galaxy in deprojected pair velocity the AM2322-821. amplitude kinematics, of 110 A stellar km fairly populations, s symmetric and rotation oxy- curve for the companion metallicity of AM2322-821 with Gemini/GMOS 4.11 The effects of the interaction on the kinematics, stellar population and Galaxy Formation, Durham, Poster Programme L / ) of M bul ESO L relation, in σ − BH M Max-Planck Society, MPIA luminosity - bulge magnitudes . By means of new, deep and highly total [email protected] Mr Pierre-Yves Lablanche bul often remains. In conclusion, usage of L to the bul L BH M Mr Ronald Läsker [email protected] Korea Astronomy and Space Science Institute (KASI) 145 Dr Joon Hyeop Lee [email protected] ) of central Supermassive Black Holes (SMBH) and the bulge luminosities ( BH M relation is at least as high as that from relating bul L − BH M 100 pc, which may be a photometric indicator of AGN properties. ∼ both optical and near-infrared (NIR)data (2MASS), bands. or on These inhomogeneous data relations sets were with mixed based techniques on of either measuring poorly resolved and relatively shallow often differ considerably from publishedsamples values - - bulges the cannot low bequality data intrinsic reliably and scatters extracted detailed given via decompositions in abulge provided, magnitudes the ‘standard’ ambiguity as literature in bulge+disk SMBH determining are decomposition mass indicator a inrelation is of result most practically galaxy-SMBH of cases inferior co-evolution. cropped to - total even magnitudes, with and questionable high- as a ”fundamental” Abstract A pixel analysis isthe carried F435W, out F555W on and the F814Wnoise interacting (BVI) ratio bands. for galaxy each system After pixel, M51 weas 4 derive (NGC blue/red by several 4 5194 color quantities binning cut, + describing of red theparameters 5195), the pixel pixel reflect using color-magnitude HST/ACS sequence the the diagram images parameters, internal (pCMD) HST/ACS to blue ofexpected properties secure images to M51, pixel be of sufficient in useful such sequence for M51 signal-to- quantitative parameters comparisons such of and thedistributions as pCMD blue-to-red of features age, between pixel stellar different metallicity, galaxies. populations, ratio. To we dust investigatesynthesis divide Those the content spatial models. pixel and stellar galaxy As populations morphology, using apopulations the result, and in pixel we are their color-color find dust diagram that and contentactive the population galactic and nucleus spiral mean (AGN) area arm stellar of pattern NGC age.is 5194 and R show the In a tight tidal addition, sequence at interaction we the significantly find bright-end of affect that the the the pCMD, of stellar pixels which spatial corresponding extent to the central their host galaxies has beenin widely galaxy used as evolution a models. SMBH mass It predictor has in been black claimed hole that demographic its studies intrinsic and scatter as a evenresolved constraint matches wide-field that NIR of imaging, the aextract dedicated bulge NIR-sky and substraction total procedure, magnitudesscatter and from of detailed a the 2D galaxy image sample decomposition, spanning we all morphological types. We show that: - the intrinsic 4.15 HST Pixel Analysis of the system M51 The correlation between masses ( Abstract 4.14 Total magnitude superior to bulge magnitude as Black Hole mass predictor Abstract A large fraction of diskevolution. galaxies (spirals, The lenticulars) Atlas3D harbour volume-limited tumbling samplecally bars, on provides the which a dynamical significantly modelling unique of affect benchmark suchWe their systems on and dynamics have which the and therefore to influence of built test a a the bardistributions. library on impact These the of of simulations star N-body allowed formation bars, us and models specifi- to metals for investigate re-distribution. mined the various from recovery mass anisotropic accuracy of Jeans distribution, basic axisymmetric kinematics, stellar models. dynamical gas parameters We fraction deter- uncover and some metallicity systematic biases in the recovered values for 4.13 The impact of bars on axisymmetric modelling of galaxies and the velocity dispersion anisotropy duelas3D to dataset, the and presence how of such the high bar.population resolution We evolutions numerical then in simulations show barred allow how early-type us this systems. to applies better to understand the the high dynamical quality and At- stellar Galaxy Formation, Durham, Poster Programme Keele University of the luminous components. A L / relation is parallel to that which holds M σ – M Miss Rachael McQuillin [email protected] Kapteyn Astronomical Institute, Groningen, NL Astronomy Department, University of São Paulo 146 [email protected] Dr Walter Maciel of the disk can be derived from the vertical stellar velocity dispersion. One Mr Thomas Martinsson [email protected] L / M relations can be understood as a consequence of momentum-conserving feedback from the nucleus which dependence is locked in. Previous treatments of this problem have assumed outflows into galaxies modelled σ σ − − M M direct and absolute measurement of the for central supermassive black holes (SMBHs) inobserved massive galaxies. Several authors have shownsweeps previously the that ambient both medium of into these a shelland that the expands into the galaxy. Ifas the singular shell escapes, isothermal the spheres, growth and of have theWe focussed nucleus present is on a cut the off consolidated behaviour analysis of ofrealistic the the shell cases only problem in very in which near the the or isothermaltrace dark very sphere the far matter case, dark from halo and matter the need we distribution. nucleus. extend notM-sigma With this be and these work related a considerations, to scalings singular we include for isothermal explore both more sphere, a SMBHs and more and nuclear detailed the clusters. parameter gas space in influencing the the galaxy need not of the main goals of themeasure Disk-Mass the Survey kinematics is of to the useare gas the calculated and two from stars custom-built the in integral-field measured units nearly stellarI (IFUs) velocity face-on will SparsePak dispersions spiral present and and galaxies. the thus PPak the first to The disk-halomost robust total degeneracy galaxies results mass can the from surface radial be the densities stellar broken. Disk-Mass velocity of Inexists dispersion Survey, the this profiles between based disks talk, follow the or in maximum IFU detail rotation and thehaving speed radial 21-cm light and radio a distributions. the synthesis sub-maximal A velocity observations. disk. very dispersion tight In observations of Measurements relation of the of stellar stars, the and with gas asymmetric a rotation driftthe clear curves, combined allow indication useful HI+Halpha for rotation for for curves all estimating deriving are galaxies disk decomposed thegalaxies, mass into stellar contributions providing surface from velocity unambiguous densities the density at dispersion various profiles larger dynamical from of constituents redshifts. of the Finally, the dark matter halos. In the last decade observations with the Hubblethe Space centres Telescope of (HST) the have majority revealed of the low presencemass and of scales massive intermediate with star mass clusters galaxies. the at velocity An unexpected dispersion observational of result the is host that nuclear bulge, sigma. This Abstract 4.18 Momentum Driven Feedback from Galaxy Nuclei Abstract The observed relative mass fractionsmodels. of A major dark roadblock and for this luminousas measurement matter inferred is in from the disk-halo galaxies rotation degeneracy; provide curve derived a density decompositions profiles strong depend of test dark critically matter for on halos galaxy the formation adopted 4.17 The Disk-Mass Survey: Breaking the disk-halo degeneracy Abstract Radial abundance gradients are a common featurein of the spiral galaxies, Local including Group the and Milky beyond. Way,and Andromeda stars, These and and gradients other are objects can very be probably observedfor linked in to elements several the such formation objects, process such as of as Fe,objects, the HII galactic O, e.g. regions, disc. planetary Ne, Recent nebulae HII Ar determinations of regionsnebulae and the and and S gradients open young suggest clusters. stars, that In andnebulae there this those are and work, determined differences compare we from between the present intermediate new thenebula results determinations and central gradients with of stars older derived those the on objects, from derived gradients the such younger fromcomparison from basis intermediate can as other of age be planetary objects. age-metallicity planetary made relations with Individual asdiscs objects of well ages of spiral as are different galaxies, using ages. especially estimated their concerning for Some the kinematic the conclusions star properties, formation can planetary so rate be that as obtained a a regarding function detailed the of the formation galactocentric of distance. the 4.16 Radial Gradients and Disc Formation in Spiral Galaxies Galaxy Formation, Durham, Poster Programme ) as a basis for > . The depth of the 2 s σ K + 2 V √ < R Institut d’Astrophysique Spatiale / University of California Santa Cruz > | V | < R = R λ profiles and draw correlations with varying formation . We find that fast rotators are nearly oblate, and slow ϵ R λ Dr Nicole Nesvadba [email protected] − Department of Astronomy, Stockholm University, Sweden σ / 147 Mr Christopher Moody [email protected] V ), obtained in the span of six years from ESO NTT and NOT. The majority of s Surface Photometry of 45 BCGs [email protected] Ms Genoveva Micheva s UBVRIHK of dense molecular gas, which appears at least a factor 10 less efficient in forming stars than expected ⊙ UBVRIHK M 9 10 rotators are triaxial. Except inmerger-produced galaxy a as single a instance, slow where rotator the is rare. total initial angular momentum is zero, we find that viewing a Baryons matter, even in aknowable Universe unknowns” forming of hierarchically current under galaxy thecretion evolution gravitational to models forces galaxy are of merging closely dark and linked feedback matter.the to from ISM, the Most star energy hydrodynamics of formation that of the and must baryons, AGN. ”un- of be from All dissipated molecular gas of before gas ac- these stars as processes can an injectities, form. agent mechanical gas (and I energy masses, tracer) into will of report and the on dissipationmolecular our dissipation timescales gas, on-going of but in efforts mechanical we the of energy, are multiphase quantifying by onlyin warm the starting measuring the role and to bulk shocked understand cold and the gas gas. turbulent potentialemission veloc- trigger consequences It lines, a for is and galaxy cycle well makes evolution. of known molecular Turbulentarchetypal molecule that examples gas cascades destruction shocks to an illustrate and can important that heat (re-)formation, (and thislutionary could which so phases. be boosts far significant In largely in the the shaping ignored) luminosity galaxies overlaplocal coolant of during dissipation region of astrophysically rate molecular of of very the the kinetic different ISM. energy Antennae, evo- injectedfind I we by several will find the merger. that discuss In recent two nearby, star gas-rich formation radio appears galaxies like directly 3C326N related and to 3C293, we the kinematic classification of slow andscenarios, fast triaxiality, rotators. kinematically We decoupled construct cores, and Abstract from the Schmidt-Kennicutt relationship, a consequenceboth of examples, the I injection will of mechanical discusshierarchical energy paradigm how by of these the galaxy results radio-loud evolution. may AGN. For contribute to solving some of the outstanding open questions of our 4.21 Much More Than Just The “Fuel of Star-Formation” Abstract Rich two-dimensional integral fieldDEIMOS unit are spectrographs producing such richprofiles as observational of data SAURON the stellar sets and components yielding large ofnor insights hydrodynamic multi-object and simulations into spectrographs major sampling galaxy galaxy binary such merger formation. mergersquantifying as formation and the scenarios We projected a including mi- stellar create program angular mock of momentum cosmologically-motivated kinematic per mergers. unit mass Emsellem ( et. al (2007) use a proxy Compared to Observation 4.20 Two-Dimensional Kinematics of Hydrodynamic Simulations Abstract We present new and previouslyinfrared unpublished broadband observations of filters 45 ( Blue Compact Galaxies (BCGs) in seven optical and near- 4.19 Deep the observations are the deepest to date, with exposure times in some cases as long as 5.6 hours in observations allows us to carryalso out able detailed to analysis separately not examine only theerrorbars on properties for the each and target structural central and parameters starburst each of usually filter. the present underlying in old BCGs, stellar but host we with are reasonable Galaxy Formation, Durham, Poster Programme Centro Astronomico Hispano Alemán Ludwig-Maximilians University / MPE (3 sigma), using PPAK/[email protected] CAHA 2 23 mag/arc ∼ 148 Ms Rhea-Silvia Remus [email protected] [email protected] Dr Sebastian F. Sanchez , to a depth of 03 . 0 < z < 005 . 0 600 galaxies at ∼ with two instrumental setups (low2010-2013. and high We present spectral here resolution). the The current status project of has the been survey. granted with 210 dark nights along Abstract We report on the current statusspatial of the resolved CALIFA spectroscopic survey. properties CALIFA of is thein an galaxies the IFS in color-magnitude survey the with diagram, the Local and main Universe,basis (3) aims (2) of trace of understand their (1) the the fosil characterizing chemodynamical records. the nature and ofa To starformation the sample achieve history dichotomy of these evolution goals of CALIFA galaxies is on obtaining the IFS data covering the complete optical extension of Report 4.23 CALIFA: Calar Alto Legacy Integral Field spectroscopy Area Survey, Early Abstract Observations of the velocity dispersionsvariety of of Planetary velocity Nebulae dispersion profiles, in some the flatteningsome outer decreasing to fast, nearly halos showing constant of nearly values, no elliptical some evidence galaxies increasingof for again the have a in Dark dark revealed the matter Matter a outer halo. halos part huge ellipticals In and of this are elliptical work embedded we galaxies in, address by and the measuring what questions velocity of weprojection dispersions the can effects in nature and learn the the about outer number the of halos. formation observedof Furthermore, mechanisms Planetary simulated we and Nebulae are histories elliptical are interested for galaxies these in with measurements. howmayor different important Therefore, merger evolution we events, scenarios, study in a covering which sample a wethe wide collide resulting range two ellipticals of in galaxies detail, galaxy with and masses: mass cosmologicalminor ratios simulations High merger between with resolution evolution gas 3:1 and scenario to star and 1:1, particles, the to toouter influence study study halo of the the profiles, the effects dynamical and environment. of values we the We of show multiple range, are that while able star there to formation, is reproduce gas no the content significant full difference andmechanisms. between range environment the of play outer observed an halo important profiles role resulting from for the probing different these elliptical formation 4.22 The Outer Halos of Elliptical Galaxies Galaxy Formation, Durham, Poster Programme 1.0 kpc − NASA/MSFC Kapteyn Astronomical Institute Dr Douglas Swartz [email protected] University of Arkansas at Little Rock Miss Chiara Spiniello [email protected] 149 Dr Patrick Treuthardt [email protected] 250km/s) of the early-type galaxies, by combining ,stellar population studies > relation. We have been studying this phenomena using deep, high-resolution, X-ray observations of several ⋆ σ − BH Abstract NGC 3124 is an unusual SB(r)bcof galaxy the in outer spiral that arms. the bar We willband seems show images to from some be the preliminary a Carnegie-Irvine results Nearby of very Galaxy our opento Survey. photometric spiral recreate analysis We pattern the of will winding high observed also resolution in show morphology B, some the through V, preliminary opposite inelastically R, results sense colliding and from our I- test attempts particle simulations. 3124 4.26 An Investigation of the Apparent Counter-Winding Bar-Spiral Hybrid of NGC in diameter. Massive-star feedback fromand this hence starburst evolution activity along may theM ultimately Hubble affect sequence, the the growth formation of andnearby galactic fueling galaxies pseudo-bulges of hosting central circumnuclear rings. SMBHs,circumnuclear and We the regions, report physics on correlations determinations behind of of the feedback hot the on physical gas gas parameters with inflow of onto other the any hot signatures central gas object of in and local the gas star outflow into formation, galactic and halos. estimates of the role of We report on our study ofof how normal barred feedback, galaxies. implied Bar-induced by inflow the often presence forms of a hot circumnuclear ring X-ray-emitting of gas, intense operates star-formation in some 0.5 the central regions Abstract 4.25 Feedback from circumnuclear star formation in normal barred galaxies Abstract I present first results from the X-shooter Lenshigh-mass Survey end (XLENS),which (sigmaETG aims to study the darkand matter and strong stellar gravitational content lensing. of the We observeand a thanks sample to of the lens huge galaxies wavelength withdetailed coverage, X-Shooter,a stellar-population we powerful and are broad-band kinematics able spectrograph studies to ofhigh-precision obtain the high-resolution strong spectra most gravitational from massive lensing the ETGs estimates UVB upinside of to to Reff, the the redshift and near-IR total 1. to for masses test We toI a combine obtain present possible these their results correlation data precise from with between dark-matter the internal massredshift pilot dark program fraction z matter of = fraction the and 0.444(Spiniello project: galaxy etstellar mass The al kinematics and Comic 2011, and size. Horseshoe in strong (SDSSJ1148+1930),a In prep).In gravitational very thisthe particular, lensing, massive lens. talk, by galaxy we We at combining measured find constraints the that from logarithmic darkthe effective matter X-shooter slope radius. is spatially of By unambiguously the resolved computing present the total and spectralwe mass evolution accounts calculated of for density a the more galaxy second profile than with independent of several 50% estimate starIMFs. (99% of formation the CL) histories We from stellar of find SSP mass the models, that fraction mass a inside within We the Salpeter have same IMF also aperture tested is for IMFs preferred, with Salpeter steeper providing and profiles a& Chabrier in fraction the Conroy(2010). lower in mass We perfect range (0.1 infer agreement - with thatvery 0.7 Msol the massive dwarf-rich )following ETG, one IMFs a as inferred suggestion steeper they by by than van result lensing. Dokkum in Salpeter a (slope stellar of mass 3 fraction that or disagrees even with 3.5) the are lensing result unlikely,at at least a for confidence this level of 95%. structure of ‘The Cosmic Horseshoe’ 4.24 XLENS: The X-shooter Lens Survey ￿ dark matter, IMF, and internal Galaxy Formation, Durham, Poster Programme erg/s) 38 Oxford 10 × 6 < University of Alabama [email protected] Dr Michael Williams Universität Duisburg-Essen, Germany Dr Mihoko Yukita [email protected] 150 Dr Janine van Eymeren [email protected] NGC 2903 is a nearby SBc galaxyChandra with intense observations circumnuclear of star formation this induced central bythe a star central young forming 15” stellar bar. (650 region. pc) We of present The the deep data nucleus reveal along with high eleven surface point-like brightness sources. diffuse None of emission the within point sources (Lx Abstract 4.29 X-raying the Circumnuclear Star Formation in NGC 2903 coincide with the galacticcompact center central of object. mass, Lower surface and brightnessand we emission column extends place density to stringent maps the indicate north upper a andrest limits west possible of of hot on the the gas the hot nucleus. outflow gas X-ray from X-ray is temperature the emission probably circumnuclear confined from region to to any the the accreting disk. northwest; however, the Williams, Zamojski, Bureau, Kuntschner,about Merrifield, half de of edge-on Zeeuw disk and galaxies.this Kuijken may If Boxy imply these and that bulges are their peanut-shapedof nothing hosts bulges giant more are are disk and pure nothing galaxies seen disk less formed in galaxies thanthere in with bars a is no viewed hierarchical nothing classical in universe special bulge. projection, with about then real our But edge-on disk current classical galaxies, galaxies understanding bulges this are of are raises irreconcilable galaxy a with thethese formation ubiquitous our possibility bulges. physics. understanding feature that A of handful Since a galaxy of demographically them, formation. including significantindependent It that of population is in height the therefore of above Milky crucial the Way, to disc. have better beenpure In observed understand disk order to interpretation to rotate is assess cylindrically, consistent i.e. whether with such with their behaviourof velocity stellar is a populations, ubiquitous targeted we in sample have boxy of analysed bulges, the five and stellar whether boxy kinematics a bulges. and populations Abstract peanuts 4.28 Bulgeless galaxies with big bulges: the stellar kinematics and populations of Abstract Both the stellar and the gassidedness distribution is of still galaxies poorly are understood. often Possible characterisedbut scenarios by include also asymmetries. tidal an The interactions, minor origin offset mergers, of of asymmetricwithin this gas the so-called the accretion, lop- stellar Westerbork HI disc Survey inthe of a neutral Irregular halo hydrogen and potential. are Spiral measured, Galaxies. Wewith in several investigated Both galaxy most a the properties, cases e.g., morphological large far the and sample morphologicalrelation beyond kinematic of type, of the lopsidedness morphological star nearby and formation optical of kinematic disc rate, radius. lopsidedness. and galaxies, theWe Early-type observed We environment. galaxies do seem compare not We to find find the be a a more degree strong correlation lopsided of cor- between than late-type lopsidedness lopsidedness galaxies. and the environment or the star formation activity. 4.27 Lopsidedness in nearby galaxies Galaxy Formation, Durham, Poster Programme Gyr. Their prominence 2 University of Waterloo The Ohio State University . Few group galaxies inhabit ⊙ M < τ < 1 . with radius within the cluster. This 10 Gyr 6 10 . BH 0 1, using Gemini (GMOS) nod-and-shuffle ˙ > M , and for blue galaxies we sample masses as < / ⊙ star z Mr David Atlee [email protected] Dr Michael Balogh [email protected] M M < 1 . SFR 10 10 > star 151 M -corrections to the observed galaxy luminosities, which we also use to K . We compute stellar masses by template-fitting the spectral energy distributions; our spectro- . The fraction of total mass in galaxy starlight spans a range of 0.25–3 per cent. Like lower-redshift 14 ⊙ < M 8 . ⊙ 8 M 10 / detections in COSMOS. From completed observations of the first seven groups, we find the dynamical mass ∼ dyn M star XMM M log per cent of the galaxies. We postulate that these are a transient population, migrating from the blue cloud to the red < 30 sequence, with a star formation rate that declines with an exponential timescale the “blue cloud” that dominateswith the intermediate surrounding colours. field; The instead, “green valley” we that∼ find exists a at low large redshift and is instead possibly well-populated distinct in population these groups, of containing galaxies among the group galaxy population, and thevironment marked either lack of directly blue, reduces star-forming star galaxies, formation provides incycle evidence member of that galaxies, the galaxy or group evolution. at en- least prevents its rejuvenation during the normal groups, these systems are dominated by red galaxies, at all stellar masses low as suggests that AGN fueling in cluster membersones is in most our closely related sample to are stellarunusually a mass. low poor Therefore, SFRs tracer low for luminosity of their AGN cold like stellarthan gas. the mass. being Furthermore, This rapidly indicates we truncated. that find star a Thus,stripping formation substantial to we must transition create favor slowly the population slow decline SFR-density of in processes relation. galaxies cluster such with members as rather strangulation over rapid processes like ram-pressure spectroscopy. When complete,tended the survey will consistestimates of are in sixteen good groups13 agreement selected with from the spectroscopically masses confirmed,scopic estimated sample ex- from is the statistically X–ray complete luminosity, for all with galaxies most with of the groups having Abstract I present preliminary results from a new survey of galaxy groups at 0.85 5.2 Group Environment Evolution Collaboration (GEEC) Abstract Due to their high densities, galaxy clustersWe use are optical an and excellent mid-infrared location imaging to to construct studywe spectral the energydistributions fit impact (SEDs) for of using galaxy environment cluster model on members, galaxy which templates. evolution. These fits yield 5.1 Clusters as a Galaxy Evolution Laboratory: A Multi-Wavelength Approach measure stellar masses and star-formationX-ray rates luminosities. (SFRs). The two We AGNpartially populations identify are to AGN largely obscuration from disjoint. in the their The shapes hostsignificant difference of galaxies. is difference due their The compared to SEDs duty to varying cycle and sensitivities the of from and field, AGN at their relative but least to we star do formation see in variation galaxy clusters in shows no Galaxy Formation, Durham, Poster Programme cold . We 5 Λ . 24 photometric ≈ S Kapteyn Institute Durham University University of Arkansas ugrizJHK 2 ∼ with (AB) depths of z 2 Dr Rich Bielby [email protected] deg 4 Miss Burcu Beygu [email protected] . 2 [email protected] Dr Joel Berrier ) formed within a set of cosmological ⊙ , B, J&K and UV and the HI imaging of the gas M α 0 . 14 152 band imaging over a total area of s K and H , J catalogues. We analyse the clustering of galaxies as a function of mass, type and redshift using derived s . For star-forming galaxies we see that clustering strength increases for higher stellar mass systems, however little ugrizJHK 2 ≈ quantities from the photometricforming template galaxies fitting. across our entire Passive redshiftz galaxies range, whilst are we seen see to littlesign redshift be of evolution a consistently in mass the more dependence clustering clustered in of passive than either galaxies sample star- is to seen observed over the range in stellar mass that is probed. combine this deep near-infrared data with the deepcatalogues optical data in of the each CFHTLS to of produce the 8-band fitting four of CFHTLS the photometry Deep to fields. estimatein photometric Taking the redshifts, these galaxy catalogues, types, star-formation we rates use and the stellar Le masses of PHARE sources code to perform SED We present deep near-infrared imaging in the fourThe CFHTLS WIRDS deep fields, data taken as incorporates part of the WIRCam Deep Survey (WIRDS). Abstract 5.5 The WIRCam Deep Survey: Mass Selected Clustering to dark matter N-body simulations, and tracklogical the fractions accretion histories in of cluster cluster and subhalos.within field By the populations, comparing cluster we the environments. observed estimate morpho- anphenomena. Galaxy approximate They clusters timescale are provide for the a morphological largest interestingarchical collapsing transformation environment structure objects formation. in for the Through the universe, understanding study and, thesuch of formation as studies several allow of such, us clusters, they astrophysical to we are place probe constraints an key onstructure. observable several parameters constraint processes Simulations in in of provide cosmology the hier- us and formation and with evolutioneffects tools of that to galaxies the as interpret cluster well the as environment growth large may scale andof have assembly galaxy on of galaxies cluster these that sized objects have dark allowing beenaccreted us matter accreted into to into halos the the probe cluster in cluster. the environment simulations I assamples and examine well of examine the as galaxy formation the the clusters timescales allow possible necessary simple effects to models on affect to the this be tested. change. morphologies Comparisons of with galaxies observed Abstract Voids are unique environments for galaxiesobservational to survey evolve. of We 60 are geometrically conducting selectedand a void stellar Void content, galaxies. galaxy kinematics Survey The and which aim dynamics istelescopes of of a and these the multi-wavelength satellite galaxies survey to and is get their basically deep companions. to imaging We study in use in different a detail wavebands wide the like range gas H_ of ground based 5.4 Interacting Void Galaxies as well. Within this sampleone we companion got having very a interesting tidal examples tailof of and three interacting ring aligned systems like galaxies such structure with as suggesting oneundergoing a a showing interactions possible system a merging of in sign event. three voids of galaxies Another are a with these one important major underdense is merging prototypes regions also is event for expected a obvious testing to system from progress current its slowly.from galaxy extreme the Here formation morphology. we Void want theories Galaxies to Galaxy since present Survey our evolutiongalaxy first and in interactions. results discuss of interacting the void possible galaxies merging scenarios and the role of low density environments on the Abstract We study the formation of galaxy cluster-size dark matter halos (M > 10 5.3 Galaxy Cluster Assembly and Environmental Effects on Galaxy Morphology Galaxy Formation, Durham, Poster Programme AAO 0. I will also ∼ 0.1. Three of the BCGs ∼ Dr Sarah Brough [email protected] University of Hertfordshire Kapteyn Astronomical Institute parameter which offers a new and unique R λ Dr Nicky Brassington [email protected] Mr Marius Cautun [email protected] 153 Abstract Using the Multiscale Morphology Filterclusters, we filaments dissect and in walls. aterms scale-free of We way Betti analyze the numbers, and structure following characterizenumbers of the to the instruments the discriminate of topological Cosmic alphashapes between structure Web and different into ofWeb persistence. cosmological and its the parameters that The elements: resulting of and results its halo offer show environments populations new the (clusters, insights potential in filaments in of and walls). Betti the topology of the Cosmic have close companions within 20 kpccompanion and (1:4) one is has not no bound, companion theBCGs within two in that nearly 0.35 radius. Gyr equal in I mass major, will (1:1.45 drypresent show and mergers. the that 1:1.25) I stellar while companions conclude kinematics the are that lowest of likely BCGs mass to these continuemeans to merge systems, to grow with analysed measure from their using the major host the merging stellar SAURON evenall angular at these momentum z massive of galaxies BCGs have and lowcompanions make are angular a found momentum direct to as comparison be one to fast-rotating mightgalaxy galaxies other expect. with evolution early-type high and galaxies. One angular the of momentum, formation Not thereby the of providing four Intra-Cluster a BCGs Light. new and test two for of models of the massive 5.8 Topology of the Halos in the Cosmic Web I will present Integral Field Unit (IFU) spectroscopy of four brightest cluster galaxies (BCGs) at z Abstract IFU spectroscopy 5.7 Spatial kinematics of Brightest Cluster Galaxies and their close companions from Abstract It is widely believed thatwith very another few galaxy. galaxies exist These today interactionsclear that play activity. have a However not major the been role parameters formed that inGalaxies or influence the Survey this shaped evolution (SIGS) enhanced in of activity is some galaxies are addressing waylarge by poorly this sample by understood. triggering of question an 111 star The galaxies interaction by Spitzer formation in Interacting using different and stagesfurther IR nu- of present interaction. data radio In HI obtained this data with presentation which I the allow willon us provide Spitzer the to an overview Space interacting determine of the systems Telescope the properties that sample to of and containwith the study one the ISM a of opportunity gas-rich these to and systems. study one how I gas-poor coldwith will gas galaxy; specifically the from focus the Spitzer the damp gas-rich data, mergers. galaxy provide is Such affected constraints systems by on provide its the companion us and relationship thereby, between in the conjunction ISM and star-formation in interacting systems. Mergers 5.6 The Spitzer Interacting Galaxies Survey: The Behaviour of Cold Gas in Damp Galaxy Formation, Durham, Poster Programme McGill University University of Padua Swinburne University 2 that can be used to quantify the ∼ 5 [email protected] Ashley Faloon < Dr Jeff Cooke [email protected] 5 to z z ∼ < Dr Elena Dalla Bontà [email protected] 30 kpc, physical. The eLBG behavior suggests the < 3 aLBGs and eLBGs in 4-year stacked images of the ∼ 0.5) and affords a unique opportunity to study not only the ∼ 154 at z 3 LBGs. We use broadband color-magnitude criteria, tested using ⊙ ∼ M 1 as part of the Red-Sequence Cluster Survey: a unique and massive ∼ 15 10 ) pure samples of z 4 10 > 1 ∼ 400 Keck spectra, that produces large ( formation of the most massive structuresthe in galaxy the populations local within universe, them. buting also We 1925 the have redshifts effect assembled with that 211 an theimaging. confirmed extensive merging supercluster multiwavelength Using of members these data massive data thus set halos we far, has over identifyanalysis and on the substructure of deep structure and the optical, dynamically includ- specific near-IR, distinct star infrared, groups formation radio within rates the and of supercluster the X-ray and members present galaxies an as a function of their local environment. high-redshift structure, comprising three boundand and separated merging by galaxy less clusters thangenitors spectroscopically 3 of confirmed Mpc present-day to massive in galaxy lie the clusters at plane ( z of = the 0.9 sky. This supercluster is one of the few known examples of the pro- Abstract We have identified a spectacular supercluster at z Study of a z 5.11 Witnessing the Formation of a Massive Galaxy Cluster: A Multiwavelength growth of proto-groups and clusters and the precursor to the red and blue sequence observed today. Abstract We present a photometric analysis ofwith the 44 Advance early Camera type for Surveys galaxies (ACS) inphotometric on decomposition Abell board of the 1689, each Hubble based galaxy Space surface-brightness on Telescope distribution (HST). observationsboth using We a in the performed Sérsic the GASP2D a law two- fitting rest-frame and dimensional algorithm. V-band a Weby de adopted an Vaucouleurs exponential law. law. S0 The galaxies derivedquantify photometric were parameters how analyzed will it also be is taking used affected into to by account analyze the a the fundamental use disc plane component of of described different Abell decomposition 1689 techniques. and 5.10 Photometric analysis of 4 square-degree CFHTLS Deep fields. Analysisthe of behavior the of CFHTLS the auto-correlation LBG functionssteeper subtypes reveals slope on a indicative small significant of difference scales multiple in (one-halo massivetude term halos and regime). within a the We shallower parent find slope dark thattypical which matter aLBGs presence exhibits halo have of an whereas a a upturn eLBGs single large have at massive amplitude halo, aeLBG separations and cross-correlation with weaker of function a ampli- shows fraction an of anti-correlation eLBG signifying halosof the consisting intrinsic the difference of two in two mass closely subtypes. and separated spatial halos. Iare distribution largely will The aLBG- located discuss in a dense picture filamentarywill that knots conclude we and by are filament discussing intersections testing preliminary and results using eLBGs that the existing follow three-point largely this correlation within analysis function from the in z filaments. which I aLBGs Abstract I will present results of detailed angularrized correlation by function their measurements spectral of features. Lyman break TheISM galaxy analysis features (LBG) of (aLBGs) sub-types LBG and catego- subsamples those that exhibitingby exhibit dominant recent dominant Lya work Lya in investigating in spectroscopic emission absorption interacting and z and weak/narrow broad/strong ISM features (eLBGs) is motivated Quantifying the growth of groups and clusters from 2 5.9 Spatial anti-correlation of Lyman break galaxies based on their spectral features: ∼ Galaxy Formation, Durham, Poster Programme α of data with spectro- Leiden Observatory 2 University of Waterloo 250 deg ∼ Pontificia Universidad Católica de Chile with line luminosity, while the subsamples Mr Bryan Gillis [email protected] 0 Dr Stefania Giodini [email protected] r 155 Dr Harold Francke [email protected] with Lyman-Alpha line luminosity and equivalent width (EW), as estimated from the narrow- and broadband 0 r scopic redshifts for foreground galaxiesto and data shape from measurements the for CFHTLS-Wide background for galaxies. an empirical We comparison. plan to apply these results Abstract Galaxy groups are a ancentral ideal laboratory and to satellite study galaxies. thecompared distribution We it and studied to assembly different the of environments, distribution looking visible forWe of matter a and stellar look cross-talk the between mass for mechanism interplay in regulating differences between satellite galaxyoperates in and groups in central the galaxy from galaxies. groups survival the with rate COSMOS respectit survey of to to the and star the field. forming prediction We from satellite constrainbaryonic galaxy the galaxies, budget evolution shape in and models. of galaxy the constrain groups. Finally galaxy how we Our stellar estimate results fast mass give the function satellite useful contribution and guidelines quenching compare of to different galaxy types evolution of models. galaxies to the 5.14 Galaxy groups: a window on galaxy evolution Measuring the mass distributions withinsights dark into matter the halos, timing and inaround and simulated particular extent halos the of with masses various tidal of massdifferentiate stripping subhalos, distributions, between of can we groups show provide the which that have key subhalos. weak undergone in- power lensing tidal to Using provides stripping overcome a and halo the those sufficiently noise models which powerful inherent haven’t. tool to in to In simulate lensing, order it weak to will have lensing likely the signals be statistical necessary to have at least Abstract 5.13 Probing Halo Mass Distributions through Weak Lensing divided by EW showed no statisticallyously significant shown difference that in clustering clustering. strength scales Since with for continuum star-forming luminosity, galaxies our it result has could been be previ- a reflection of this effect on Ly Abstract We present updated results on large scalesurvey. structure clustering strength This of survey z=2.1 Lyman comprisesnarrow-band Alpha 4 OII Emitters (LAE) 3727 fields in filters, of the MUSYC allowing 30x30clustering for analysis arcmin the of each, selection the which of fourlength have LAEs fields. at been With this imaged the redshift additional both (Guaita samples, in 2010). we broadband were Here UBVRIz able we and to present measure the the joint dependence of correlation photometry. We found that these LAEs show a significant trend of increasing 5.12 Clustering segregation of Lyman Alpha Emitter Galaxies at z=2.1 luminosity, modulo some dispersion given by the distribution of EWs of the line and the physics involved therein. Galaxy Formation, Durham, Poster Programme 1 2 − ∼ field 2 z erg s ∼ 17 2 into blue − z < 10 × 4 . 1 Durham University University of Nottingham , except for the excess of the red 5 . 1 ∼ z . We use these early progenitors of galaxy 2 Dr Nina Hatch [email protected] National Astronomical Observatory of Japan z > Dr Violeta Gonzalez-Perez [email protected] 156 ? 2 Dr Masao Hayashi [email protected] z > =134Å), we identify 380 [OII] emitting galaxies down to λ ∆ 2. For the first part of this work we find an angular correlation function that agrees with =9139Å, λ . The discovery of such structures in this cluster enables us to investigate the dependence of < 0 . 3 emitters and compare their properties, including stellar mass, star formation rate, colour and area. We find that the [OII] emitting galaxies are distributed even in the cluster core, and further α 2 < z < 3 . 1 23 arcmin × . 2 in a 32 2 − cm along filamentary large-scale structures around theever identified cluster, at which are among the largest structure of star-forming galaxies properties of star-forming galaxies on the environmentfor at the z=1.46. [OII] The emitters star indicate formation that activities and thisregions. mass-matallicity cluster relation On has experienced the active other star hand, formationcompared a comparable with to significantly those those higher in in fraction the its other of surrounding which environments. [OII] host [OII] emitters These emitting is red AGN, seen galaxies rather are onapparently than more the no dust-reddened likely red longer star-forming to sequence [OII] a be emitters. in strong nearly the environmental Our passively results cluster variation evolving all core in galaxies suggest the that galaxy there properties is at Abstract We present a panoramic [OII]Cam/Subaru, emission and survey the in follow-up NIR andWith spectroscopy around NB912 narrow-band of a filter 16 cluster ( [OII] XMMXCS emitting J2215.9-1738 galaxies at in z=1.46 the with cluster Suprime- core with MOIRCS/Subaru. galaxies to those in proto-clusters,clusters some to of understand the how densest environment environments affects at galaxies during their formative epoch. We select clean samples of emitters. AGN feedback mayregions. be one of the critical processes to quench star formation in massive galaxies in high density 5.17 Star formation activities in a cluster and its surrounding structure at z=1.46 The effects of environment onments. galaxy evolution To are investigate most the obvious influence when of environment comparing in galaxies the in early highly Universe contrasting we environ- present a study which compares Abstract 5.16 Does environment matter at proto-cluster and field H specific star formation rate. I willgalaxies. show However, that the the proto-cluster proto-cluster galaxies galaxies aretheir are already field rapidly twice forming as counterparts. massive, stars Thus and in have the adense lower proto-cluster similar environments specific galaxies manner promotes star to galaxy are formation growth field further rates in evolved than thebefore than early the Universe, the and clusters field that virialized. galaxies. cluster galaxies This differed from study field implies galaxies that even Abstract Using the semi-analytical model developed in Durham,and GALFORM, we mass have selected studied samples the clustering at of z Extremely Red Objects z < 5.15 Clustering of massive galaxies and the evolution of clustering with mass, for observations from UKIDSS, one ofing the result largest that, and although deepest semi-analyticalclustering models near-infarred with predict surveys. mass a is clustering In clear that the and does at second odds not part with change we observations. with find Splitting luminosity, the the the mass surpris- variation selected of sample of galaxies at z and red, we find that theincrease correlation with length redshift, of a red result galaxies in stays qualitative rather agreement flat with with redshift, observations. while that for blue galaxies tend to Galaxy Formation, Durham, Poster Programme 3 = z . Using 3 < z < 1 NAOJ < z < 1 km/s. We present Durham University 4000 (CL0939+4713) and 4 . cz < = 0 , very similar to the typical halos z Dr Yusei Koyama [email protected] ⊙ M 1 level. We show that SMGs at − h σ [email protected] Dr Ryan Hickox 4 12 > 10 × Harvard-Smithsonian Center for Astrophysics 1 has probably played a key role in shaping at least a fraction 1 m-selected submillimeter galaxies (SMGs) at 157 µ z < z < Ms Lauranne Lanz [email protected] (RXJ1716+6708), with narrow-band filters of Suprime-Cam and MOIRCS on the Subaru Telescope. Taking advantage of 8 . for optical quasars. These results are consistentscenarios with in measurements which for optically-selected powerful quasars, starburst and and support quasars evolutionary are driven by a common mechanism. of the present-day cluster galaxies. The evolution of galaxies iswas greatly designed influenced to probe by a their range of interactions.It interaction parameters is The using infrared Spitzer comprised data Interacting complemented of by Galaxyassociation the a Survey likelihood. range Keel-Kennicutt of (SIGS) The other sample resulting (Keel observations. sample et contains 111 al. galaxies in 1985) 50 systems, complete located sample with of interacting galaxies chosen on the basis of Abstract 0 the wide-field capability of these facilities,structures we at these investigate high in redshifts. detail In the particular,emitters star we in forming report the a activity cluster discovery of of surrounding galaxies a environmentabrupt along surprisingly such large the break as number large-scale (i.e. of groups optically and red transitional filaments, H-alpha indeed environment). where MIR-detected the We dusty colour-density revealed starbursts, relation that shows based an demonstrate a on non-negligible our that wide-field fraction properties 15-micron of of imaging suchdusty galaxies with red starbursts, AKARI are H-alpha and satellite. that emitters indeed the are Thus, changing group-scale our environment ’before’ at results entering cluster environment accompanying strong 5.20 The Spitzer Interacting Galaxy Survey: IR-UV Photometry the photometric analysis of the completeinvestigate Spitzer the coverage variation and almost of complete starthose GALEX formation predicted coverage. along by This numerical the atlas simulations. interaction will sequence. be used We to describe observed trends and compared to We present our panoramic H-alpha emitter survey for the two distant clusters of galaxies at Abstract understanding environmental effects at 5.19 Red star forming galaxies in distant cluster outskirts: a key population for data from the Laboca ECDFS Submm SurveySMGs (LESS), we and employ galaxies, a using novel full technique to theprojected measure full two-point the probability cross-correlation correlation distributions between function for we photometric derive redshiftsWe the detect of linear clustering the bias in galaxies. the and cross-correlation characteristic From between dark the SMGsare and matter observed indeed galaxies halo strongly at masses the clustered for and the reside SMGs. in dark matter halos of mass a few Abstract We present a measurement of the spatial clustering of 870 5.18 Clustering and dark matter halo masses of 870-um selected SMGs Galaxy Formation, Durham, Poster Programme Academia Sinica University of Heidelberg Dr Yen-Ting Lin [email protected] North-West University, South Africa Dr Thorsten Lisker [email protected] Dr Ilani Loubser [email protected] 158 We have fitted the Mg2 absorption indexwe gradients have for obtained 21 high brightest signal-to-noise cluster ratio, galaxies long-slit (BCGs), spectraspatially-resolved, in on spectroscopic the the sample Gemini nearby of telescopes. Universe, BCGs for This which which is allows a possiblestellar sub-sample connections of population between a the large properties kinematical, optical, dynamical to and bemetallicity) studied. gradients and We mass investigate of thethese the existence galaxies BCGs, in of the and a centre whether correlation of such between the cluster a the gravitational correlation Mg2 well. is (and the therefore consequence of the special location of Abstract 5.23 Mg2 gradients as a signature of evolution The Millennium-II simulation allows semi-analytic modelsis still (SAMs) not to well probe understood the theoretically. regimeal. We of (2011) compare dwarf SAM the to galaxies, properties the whose and nearby evolution distribution clustersratio Virgo, of in Fornax, cluster the Coma dwarf and SAM, galaxies Perseus. the in Apartgalaxy the dwarf from Guo colour population the et systematically and of higher distribution. the dwarf-to-giant SAMbluer However, clusters in there is colour seems very to similar and to becluster, less the serving no dynamically as dwarfs Virgo relaxed. a in cluster local Coma equivalent universe This andthe benchmark. in Perseus, is huge When the in focusing important, number SAM: on terms of since the the of elliptical diversity Virgo Virgopassive of dwarf disk-dominated dwarfs is dwarf dwarfs galaxies are galaxy the are subpopulations, in nearest abundant. we the find andcould We real that transform interpret most galaxies universe this extensively morphologically. does by studied environmental not effects have not a included counterpart in the in model, the which SAM clusters, where Abstract 5.22 The content of present-day clusters: SAM vs reality Abstract We study the relationship betweencluster two medium major (ICM), baryonic using components 94from in Chandra clusters galaxy observations, that clusters, and span namely stellar masses the theSurvey derived galaxies redshift allow from us and range Wide-Field to the Infrared 0-0.6. trace Survey the intra- Explorer evolutionICM Accurately and of mass-total cluster Two-Micron measured mass baryon All-Sky relation total content is in and consistent a ICM withevolution self-consistent the fashion. masses in expectation We the of find self-similar stellar that model, the mass-total whiledifferent evolution there ways. mass of is the relation. no evidence for This redshift suggests that the clusters acquire their gas and galaxy contents in 5.21 A WISE-Chandra view of baryon content evolution in galaxy clusters Galaxy Formation, Durham, Poster Programme ), but otherwise ⊙ L 11 University of Victoria 10 University of São Paulo × 5 ∼ 1100 compact groups from the SDSS DR7. Special Astrophysical Observatory, Russia ∼ Dr Trevor Mendel [email protected] Prof Claudia Mendes de Oliveira [email protected] 159 ), with appropriately bright BCGs ( ⊙ Dr Dmitry Makarov [email protected] M 14 10 × 2 ∼ 25% of the non-BCG galaxies of ”normal” systems (clusters) of the same mass. The luminosity of the ∼ missing 75% of non-BCG galaxies amounts toof some 5 the times whole the luminosity system. ofwhere the central are Our BCGs all and the results twice baryons the therefore that totalform would, luminosity raise in in such a normal low systems, number richness go environments; of into(cannibalism)? and making interesting what up does questions. In the this missing other mean galaxies?; Probably, for words,while how the still what did the hierarchical allowing the process merging most the bright scenario or growth BCGs important for of environmental BCG are: a formation factor massive could BCG in inhibit the the centers of formation fossil of groups? galaxies in general, containing only We report the results ofcan the be deepest characterized spectroscopic as relatively study massive of ( fossil groups to-date. The study shows that many fossil groups Abstract Environments 5.26 Considerations on the Formation Mechanism of Massive BCGs in Low-Density Compact groups of galaxies representdensities ideal and laboratories low for the encounter studythese velocities. of dense galaxy environment I interactions using will owing a to present large, both homogeneously the their selected results high catalogue of local of an ongoing effort to understand galaxy evolution in Abstract galaxy evolution 5.25 The Bimodality of Compact Groups: Untangling the role of compact groups in I will show that the canonicalas photometric either selection substructure of in CGs a results largerthat group/cluster in isolated or a compact groups a bimodal host genuine population, a isolated where more structure.configurations prominent groups population An embedded can of investigation be blue, within of disk-like classified a galaxies galaxy than properties largeron similar shows (locally) structure. the dense study galaxy I of will interactinghierarchical galaxy provide structure pairs, formation. a and comparison discuss of the these interpretation results of with compact expectations groups based within the larger framework of Abstract We present a project on theLEDA study and of NED groups databases composed with of visual dwarf inspectionby galaxies on size only. SDSS of few images We tens and selected of on kpc such digital anddwarfs structures copy line-of-sight from using of velocity Tully the dispersion POSS. about The Hyper- et 18 groups al. km/s. are (2006).amount Our characterized groups of This are dark specific similar matter. to population associations It of of is multiple nearby very dwarf likely galaxies that such we as see I them Zw at 18 the may stage contain just significant before merging of its components. 5.24 Groups of Dwarfs Galaxy Formation, Durham, Poster Programme , but 1 < ∼ z galaxy cluster 1 McGill University z > Durham University Rochester Institute of Technology Ms Allison Noble [email protected] m. µ galaxy cluster (EN1-240) drawn from the Spitzer [email protected] Mr Nikolaos Nikoloudakis 871 871 . . Dr Rupal Mittal [email protected] = 0 = 0 z in Stripe 82 z 160 5 . results to the results of Sawangwit et al (2010) from 3 samples of galaxy cluster core. This link between SFR and stellar mass, along ) θ 62 ( . = 1 w z = 1 z JK imaging from Magellan, CFHT, CTIO, and VLT; and Chandra X-ray data. This cluster . We present arguments that this is not caused by systematics. ′ 1 z ′ i ′ r . Moreover, star-forming galaxies follow a universal correlation of increasing star formation ′ z > 1 g . We then compare the ′ 1 u ∼ z spectroscopically confirmed clusters, and has been carrying out an ambitious spectroscopic and pho- z < 1 at ) z > z ( 12 n ∼ It is now well establishedronment that regulates galaxies star in formation the (SF). In past particular, formed SF stars consistently more decreases rapidly with than increasing galaxy today, density and at additionally, that local envi- Abstract 5.29 Infrared galaxies in a rich cluster at reverses in the field at with the evolution of SFR overvary cosmic with time environment? and density prompts the question:We what address governs SF this in question galaxies through and an how infrared does (IR) it study of a We have measured the clusteringselected of 130000 Luminous LRGs Red via Galaxies colour in cutscorrelation Stripe in technique 82 R-I:I-K of using with the the Newman K angularcut,cross-correlating et band correlation the al data function. LRGs coming (2008) with from We SDSS to UKIDSS have establish QSOs,DEEP2 LAS. establish the and We the VVDS have galaxies. redshift used the distribution We cross- also of used the the LRGs AUS as LRg redshift a survey function to of colour has 93 spectroscopically confirmed members, 18 of which are detected at 24 Abstract 5.28 LRG clustering evolution to rate (SFR) with stellar mass.with Studies the have confirmation only of enhanced begun activity to in unfold a similar trends in high-redshift galaxy clusters, specifically SDSS LRGs at lower redshift tothe measure results the for dependence luminosity-matched of LRG clustering samplespassive on with models redshift simple for and evolutionary LRGs LRG models, and luminosity. such forfit We as the than have those HOD at compared expected lower models redshifts. from of long-lived, We Wakeappears find et some to al evidence flatten (2009) for in and evolution slope find in at the that LRG the correlation long-lived function model slope may in that be the a 2-halo poorer term Adaptation of the Red-sequence Cluster Surveysurvey (SpARCS). with SpARCS is currently thetometric largest follow-up completed survey of the richestIRAC and clusters. MIPS imaging; Our extensive multi-wavelength data for EN1-240 includes: deep Spitzer Abstract Active galactic nuclei at thehave emerged center as of heating galaxy agents clusters powerfulemerging with enough hypothesis to gas of prevent cooling self-regulated further times AGN coolingpresence feedback, that of of the infrared, are large intracluster optical much amounts medium and shorter of (ICM).understanding FUV than cold the Amidst observations detailed the the gas processes of Hubble in that clusters time several governsystems. also the brightest indicate fate cluster of This the galaxies the sample (BCGs). cold is gasmass in of We the and cooled are basis around gas, conducting BCGs along of a in withthe a a its project strongest Herschel sample temperature, aimed atomic of ionization Key at 11 cooling state, Project, cooling density lines flow NGC4696, and the and the cooling main dust BCG rate. of emission goals We the in of present Centaurus a the which cluster subset first of are detections of galaxies. of to our determine Herschel sample the and location focus and on one of the systems, 5.27 Linking ICM Cooling and AGN heating with Star Formation, Cold Gas and Dust Galaxy Formation, Durham, Poster Programme . JKCS041 62 . 2 and allow us to = 1 OA-Brera, INAF ∼ z University of Turku ). These results will be McMaster University 1 < z < 0 Dr Pasi Nurmi pasnurmi@utu.fi Dr Anand Raichoor [email protected] Dr Laura Parker [email protected] 161 . This study will ultimately provide further insight into the role of local 0 ≈ z Msun/yr) exhibit a strong environmental dependency, being virtually absent inside half the 5 > 2.2 JKCS041 cluster, we can probe galaxy formation and evolution at ages as young as less than 3 Gyrs and ∼ supplemented by the ongoing identical analysis on the second most distant cluster, ClG J0218.3–0510 at Abstract Thanks to the z 5.32 Evolution of galaxies in the richest environments up to the highest redshifts put constraints on the different environmentalPhotometric mechanisms affecting redshifts galaxy based evolution at on the 8neatly early bands disentangle stages cluster of photometry members the (u*grizJHKs) from cluster obvious confirm ages. of foreground the and galaxies, cluster background inside galaxies. redshift both half We to estimate andderived be JKCS041 one for z blue cluster a fraction virial consistent radius. sample We of show mass-selected that galaxies the in obtained clusters valuesstar are at forming in lower galaxies agreement redshifts (SFR with ( thecluster ones virial radius and aboundant outside it. Abstract Motivated by the mounting evidence that galaxy groupsdynamical play analysis a significant of role a in sample the evolution ofof of optically galaxies more and I than will X-ray present selected 100 recent groups groupsgroup at with samples. intermediate multi-wavelength redshifts. I imaging The will and GEEC discussproperties sample extensive of the consists spectroscopic central dynamical coverage galaxies. classification to We’ve of identify foundhost these group. that well-populated systems, the By the combining properties amount these of results of memberand with galaxies identified studies uncover depend at substructure the critically high processes and and on driving the low the the redshift dynamics transformation we of of can the study galaxies the in dynamical this evolution environment. of groups 5.31 A Dynamical Investigation of Galaxy Evolution in Groups By analyzing a collection galaxyerties groups to with observed different galaxy masses in groupsformation the in history. Millennium SDSS II DR7 The simulations data, spatial and wethe distribution comparing study formation of their how of galaxies prop- galaxy galaxy and properties groups the and arethe luminosity analyze simulations linked distributions and how to are observations. well their compared. we dark can halos We identify and also the the talk fingerprints of about recent mergers of galaxy groups in Abstract Groups 5.30 Fingerprints of Merger Events in the Observed Properties of Galaxies in Galaxy We find differences in the SFR-versus-stellarthe mass trend lowest for specific various populations, SFRs. withto the most We avoid massive overproducing discuss systems the displaying how cluster rapidlyenvironment mass on the at SF SF through mass of assembly massive,toward and higher cluster IR-luminous density infall, members regions. at the must pivotal be epoch quenched at which in the order most active sites of SF move Galaxy Formation, Durham, Poster Programme Observatory of Tartu University of Victoria Mr Tiit Sepp [email protected] Miss Jillian Scudder [email protected] 162 . We estimate that in our SDSS DR7 galaxy group catalogue more than 90% of the groups are 18. This is work is a result of collabraition work from Observatory of Tuorla and Observatory ⊙ < M r 15 M to 10 ⊙ M 8 The Millennium N-body simulation anddark SDSS DR7 matter galaxy halos, and the galaxy distributionand group of galaxies. catalogs subhaloes are inside We used the test to main hypothesiscomparison study halos that also the and reveals galaxy structure possible the groups differences of correspondence are between the widely between galaxylennium used dark systems semi-analytical simulations, matter galaxy hosted and models halos by the used real shared for galaxy galaxies mainfrom in properties halo the the in dark Mil- galaxy the matter group observations. halo. catalog Four SDSSand different The DR7. volume velocity limited dispersion Specifically, samples we distributions are compare derived andalways the find consider group the a richness, halo rather virial group radius, goodscales as maximum from agreement separation a 10 between system the with mock the catalog main and halo and observations. its subhaloes. We The halos we find encompass the mass Abstract in the SDSS DR7 5.34 Differences and similarities of galaxy groups in the Millennium simulation and gravitationally bound and the groupthe finding idea algorithm that can the find link realused between galaxy luminosity galaxies range groups in very galaxy well. groups and This dark work matter strongly subhaloes supports inside main halos is very strong at the Abstract Compact groups of galaxies provideopportunities for a frequent unique tidal interactions, galaxy while interaction theirof isolation testing large-scale from ground; other environment. structures their should, high ininteraction Gas-phase principle, local timescales limit metallicities densities the for and effects should both star provide galaxytrends: pairs formation high and rates metallicities galaxies have for in a previously cluster givenmay environments. been mass be in due used These clusters to as two and both low environments differences a121 metallicity in show probe for compact environment opposite a group and into given galaxies merger mass history. selected in from Towill galaxy the disentangle show pairs. SDSS these that These dependencies, which the differences I have behaviour present robustly ofrather sample measured a than of star galaxy on formation in the rates a high and compact localregions. metallicities. group densities depends I of on the the group large and scale I environment will of discuss the the compact implications group, for merger histories in locally dense of Tartu. importance of large scale environment 5.33 Offsets in Metallicity and SFR as interaction markers in Compact Groups: the Galaxy Formation, Durham, Poster Programme AGNs, the cross ), which indicates 8 . 8 . 1 Durham University ∼ University of Arizona = 1 3 . γ = 1 Mpc ( z 1 − h 5–6 Dr Russell Smith [email protected] = Dr Ramin Skibba [email protected] 0 National Astronomical Observatory of Japan r to 3.0 measured by using the Japanese ). Considering that our galaxies sample is based on optical 3 . 8 . 163 = 1 = 0 Dr Yuji Shirasaki [email protected] γ z Mpc ( 1 − h 3 ), we obtained correlation length of +6 − 9 . 0 400 red sequence galaxies spanning a very wide range in luminosity and mass, I explore ∼ z < , consistent with the redshift-evolution of the giant-to-dwarf galaxy ratio in distant clusters. In the cluster 5 . 0 . ∼ 2 . z 0 < ∼ the dependence of SSP-equivalent age on massgalaxies and correlate location primarily within with the their cluster mass, environment.cluster while The for centre. characteristic dwarfs ages there Among of is dwarfs giant a inthan stronger the dependence on core projected of distance the fromoutskirts cluster, the by approximately contrast, 50 almost per all centz joined of the the red passive sequence dwarfs more are recently young, with their star formation having been quenched only at Abstract I will present new resultsgether, from these a observations wide-field provide spectroscopic afrom and comprehensive the multi-wavelength remote view imaging past of survey to environment-driven the of present quenching the epoch. of ComaUsing star-formation a cluster. spectroscopic in sample To- clusters, of 5.37 Stripping and quenching of infalling dwarfs in the It is generally assumed thatenergy, is the also central the galaxy brightest halo in galaxycentral a (BHG), galaxy and paradigm dark that (CGP) matter it is resides halo, an at essentialof that rest the assumption CGP at is, made using the in a the centre various large of galaxy galaxy fields group the of withFor catalogue dark astronomical constructed the matter each from research. potential the lowest group I Sloan well. Digital test specific I This Sky the Survey potential positions compute validity and modeled of two group brightest catalogues. statistics, group R galaxies relativeand and to S S, the to which other those quantify group obtained members.data the from indicate detailed offsets By that mock comparing of in the catalogues, the a cumulative I non-zerogalaxy. line-of-sight distributions rule fraction of velocities out of In R and the haloes particular, null-hypothesis of projected that a Ithat given the these find mass CGP values that the are is BHG uncomfortably the correct. high is fractionmodels compared not Rather, of increases to the the galaxy predictions from central formation. from galaxy, 0.25 I halo but end occupation in instead, by statistics low a discussing and satellite various mass from implications semi-analytical haloes of to our result. 0.40 in massive haloes. I show observations with Suprime-Cam at the redshift range,objects it that are is observed expected to that be blue clustered star-forming aroundthe galaxies the Virtual AGNs. comprise Observatory the It system majority is can of successfully provide demonstrated a thatredshift powerful the AGNs. tool use for of investigating the the archive small through scale environment of the intermediate Abstract 5.36 Are Brightest Halo Galaxies Central Galaxies? that the AGNs at this redshiftat range reside higher in redshift a ranges similar reside environmentcorrelation around in length typical a local was denser galaxies. measured environment We as also than found 11 lower that redshift AGNs AGNs; For Abstract We present the result of projected crossVirtual correlation Observatory analysis of (JVO) AGNs was and galaxies usedWe at to redshifts investigated from obtain 1,809 0.3 the AGNs, to 3.0. Subaru whichclustering The Suprime-Cam is at Japanese images redshifts about larger and ten than times UKIDSS 0.6.For larger catalog We the a data found low significant sample around excess redshift than AGNs. of samples that galaxies ( used around the in AGNs previous at studies redshifts from on 0.3 AGN-galaxy to 1.8. 5.35 AGN and Galaxy Clustering at Virtual Observatory (JVO) Galaxy Formation, Durham, Poster Programme . , 3 . 61 . = 0 30 per = 1 z ∼ (Cl0332- imaging, I z 6 . α 1 area each, and ∼ 2 z Durham University University of Tokyo –1.0 epoch. 5 . [email protected] Dr John Stott 500 Myr. = 0 < ∼ z [email protected] Mr Ken-ichi Tadaki , corresponding to a dust-uncorrected star formation rate of 2 − 164 cm 1 − erg s 17 − arcmin) is very high, and that the ratio of the [OII] emitters to the red galax- 10 1 ), we identified more than 300 [OII] emitters on the basis of narrow-band excess × 0 62 . . 2 r < = 1 z . In CIGJ0218-0510 ( 1 − yr ⊙ M This opposite trend at high-zaccelerated to in high the density one regions in at high the redshift. local Universe suggests that galaxy formation and evolution is biased and 5 and photometric redshifts. We alsoforming sampled activity red-sequence in galaxies the on the clusteries color-magnitude cores increases diagram. ( towards We higher find density that regions. the star We obtain consistent results for the other cluster Cl0332-2742 at 2742 and CIGJ0218-0510) with Suprime-Cam onreached a Subaru 3-sigma telescope. limiting line Both flux surveys of cover about 800 arcmin Abstract It is well known thatvestigate the galaxy environmental formation dependence and of evolutionwe the is have properties for closely conducted star-forming panoramic related galaxies narrow-band to at surveys the the of surrounding peak [OII] environments. epoch emitters of in galaxy In two formation, order frontier to high-z in- clusters at 5.39 Biased galaxy formation and evolution in two frontier clusters at z=1.6? Brightest cluster galaxies are the most massivewells stellar and systems are in thus the ideal Universe, objects residing forHAWKI at studying the hierarchical imaging centres assembly. surveys of I the of present largest new 20 potential mass, results to of from investigate our the their Subaru merger most MOIRCS activity and distant since VLT of redshift X-ray this 1.5. selected sample In to clusters, a look parallel using for study evidenceevolution near-infrared we of further. exploit light an deep evolution as HST in imaging a the data proxy scale for size a for and subset stellar light profile shape of BCGs in order to constrain their Abstract 5.38 The mass and size evolution of the most massive galaxies The ongoing build-up ofact the of faint transformation red as they sequence encounter population the can dense cluster also environment. be Using probed ultra-violet by and narrow-band observations H of galaxies caught in the identify a sample of galaxies apparentlysuggest undergoing they gaseous are stripping being events. stripped Thecent by UV of ram and currently pressure, gas star-forming with morphology galaxies of star-formationorientation these within occurring shows objects 1 in that Mpc the stripping of tails is Coma of a are expelled first-passage phenomenon, undergoing gas.Finally, with this I Some a process; will timescale show their some distribution first in resultswhich from radius will a and help very to deep spectroscopic trace study the of emergence faint of red-sequence the galaxies clusters passive at population over the crucial Galaxy Formation, Durham, Poster Programme Hartwick College Tartu Observatory University of Sussex Mr Elmo Tempel [email protected] Dr Parker Troischt [email protected] Mr J. Antonio Vazquez-Mata [email protected] 165 Abstract Using the GAMA-I group catalogue, we estimateand the halo galaxy luminosity mass function for in galaxiesin order in groups the to in SDSS intervals understand of optical the redshift bandsunderstanding evolutionary the and processes connection are of between fitted galaxies these withpreliminary and systems. results. evolutionary their distribution power-law Luminosity in Schechter dark functions functions. matter are halos. estimated This In study this will poster, contribute we to present our 5.42 Galaxy And Mass Assembly: Galaxy LF on host group properties Abstract Most galaxies reside and evolvetitative in way. galaxy We groups present and results itArecibo from Legacy is a Fast important study ALFA to of Survey understand thebership, (ALFALFA) the environment and we environment surrounding Sloan find of galaxy Digital the groups group Sky most in WBLcalculate Survey the 368 a probable (SDSS). HI using quan- With optical deficiency data a counterparts of from determination the for the of group HI by group source comparing mem- our detections results of to member the field galaxies. galaxy sample These of are Solanes. used to 5.41 Determination of HI Deficiency in Galaxy Group WBL 368 Abstract We study the influence of thegalaxies large-scale of environment different morphological on types evolution and of colourssupercluster galaxies, in cores. comparing various the global As environments: additional luminosity data, functions in we voids, (LF)satellite use filaments, of galaxy galaxies , groups and separately. and study We the use importancedifferent the of morphology environment data and for from group colours. the central We Sloan and We have Digital use taken Sky special Survey the care (SDSS) global to to large-scaledependency correct construct luminosity galaxy for the luminosities density LFs the for for field LF intrinsic galaxies toelliptical dust of of define galaxies. attenuation. elliptical different The galaxies; environments. LF the ofthat We environment spiral spiral find galaxies galaxy is a is formation more strong almost has importantevolution independent environmental to of for of be group environment, red similar central both in and elliptical satellite for all galaxies galaxies blue types has than and of been red for environment different; spirals, (from it blue showing also voids depends to strongly superclusters). on the We environment. show that the 5.40 Tracing the galaxy evolution in supercluster-void environment Galaxy Formation, Durham, Poster Programme ) value for 2 χ Yale University University of Virginia North-West University [email protected] Dr Andrew Wetzel Ms Lisa May Walker [email protected] Miss Danièl Viljoen [email protected] micron) colorspace and specific star formation rates 0 . 8 - 5 . 3 166 Galaxies in groups and clusters exhibitgroup significantly truncated catalogs star created formation from rates and themorphologies evolved Sloan morphologies. of Digital Using satellites galaxy Sky galaxies Surveygroup in Data mass, groups/clusters. Release and 7, radius I I withinwithin examine focus groups, the the on I test group. specific how a star variety these Using of formationevolution. mechanisms galaxy high-resolution and rates timescales properties cosmological and for simulations depend to on star formation track satellite truncation satellite and mass, morphological galaxy orbits Abstract 5.45 The Evolution of Galaxies in Groups and Clusters Abstract Compact groups, with their high number densities,provide small a velocity dispersions, local and analog an ISM toencounters that conditions that has of not occur been galaxy in fully interaction compact processed, shown in groups clear affect the evidence the early that evolution universe. the ofhas compact the The group been constituent frequent environment discovered galaxies and has in in prolonged a myriad gravitational both strong ways. impact the on Recent mid-infrared galaxy work (MIR) evolution has IRAC - in ( particular, a “gap” Groups 5.44 Examining the Role of Environment in a Comprehensive Sample of Compact each component is used toare compared determine to whether previously a published SSPare results, or present as CSP determined in by represents the using the stellarhistories. Lick populations BCGs indices. of most We these accurately. find BCGs, that The and both obtained those young results BCGs, and old therefore stars show surprisingly diverse star formation (SSFRs). This gap ismay not affect seen the in evolution field of samplesexpanded member and sample galaxies. is of an 35 In interesting compact order groups newindividual to in galaxies). example investigate addition of the We to find how origin the that the and original anthe compact nature 12 underrepresentation full of groups group of sample, studied this environment galaxies lending by gap, in support Johnson we this tomore et color have the fully al. range hypothesis studied characterized of (2007) that the an IRAC distribution (yielding the colorspace of compact 171 region, is galaxies group persistant in allowing environment this in us inhibits colorspace, moderate to as SSFRs. quantify theThis full We this full sample have lower sample now density picks allows region up us a moreor to few fully density analyze galaxies show with in physical a respect this properties trend to ofvariances in the the in colorspace MIR sample, these within bluer properties revealing the being and that values too MIR neither represented small. redder projected by colors. physical this diameter sample. We hypothesize that this is due to the Abstract The aim of this projectcluster is galaxies (BCGs). to In study particular, the I(CSP) will stellar determine provides populations, if a the and Single most thereby Stellar Populations significant evolutionthe (SSP) fit and Gemini or Composite and star for Stellar WHT formation the Populations telescopes. histories BCGsVazdekis/Miles of By using stellar using brightest high population the signal-to-noise models ULySS ratio software toFurthermore, (S/N), package, simultaneously the long-slit the derive stellar data spectra, the populations will obtained SSP be will equivalent on fitted be ages against decomposed and the into metallicities Pegase. two of or HR the and more BCGs. components, and the chi square ( 5.43 Brightest Cluster Galaxies: Analysis of Stellar Populations Galaxy Formation, Durham, Poster Programme 2 star forming galaxies and [OIII] emission line University of Sheffield ∼ University of Cambridge 41 . 0 Case Western Reserve University < z < 3 . 26%) having double nuclei. This presents 0 ∼ Miss Patricia Bessiere p.bessiere@sheffield.ac.uk [email protected] Dr Idit Zehavi 80%) some evidence of interaction in the form of tails, ∼ Miss Susannah Alaghband-Zadeh [email protected] 167 [23,27]. The wide range of features suggest that AGN activity can be triggered ≃ r µ ∆ W. As the depth of these images allows the identification of extended features not previously 35 10 and a range of 2 > − ] OIII [ L 25 mag arcsec ≃ r ˜ Abstract We present deep GMOS-S Gemini optical broadska band et images al for a (2005) sample sample. of 19 The type sub-sample II comprises quasars quasars taken from in the thedetected, SDSS we redshift Zakam- use range the results derived fromtriggering this of sample quasar to discuss activity. the We significance of find galaxy that interactions 15 and/or of mergers in our the sample of 19 ( Sample of Type II Quasars. 6.2 Evidence of Galaxy Interaction from a Study of the Optical Morphologies of a luminosities shells, fans, irregular features, amorphous halosµ and double nuclei. We findbefore, a during median or surface after brightness the for coalescence of thea the features strong black of case holes for with 5 galaxy of interaction the playing 19 a objects significant ( role in the triggering of quasar activity. High-z ULIRGs, identified originally byformation their rates in emission the at Universe. submm Determining the wavelengths,their trigger of are extreme the properties. found ultraluminous bursts Local to in ULIRGs these have appear galaxiesonly some to is method key be of to of often the understanding formation formed highest at by high mergers star scaled-up redshift and and interactions versions there however of this is may significant those not evidence foundsample be to the suggest of locally. that high-z the ULIRGs I high-z which ULIRGs willand are allows NII present not for emission purely the lines, the within results mapping the of of galaxies. the The integral sample gas field is dynamics compared spectroscopy to and observations the metallicity SINS of fields, survey of a by normal tracing large z the H alpha Abstract 6.1 IFU observations of high-z ULIRGs in an effort to understand what causes the highof star other formation star rates forming in galaxies the at ULIRGs, this placing redshift.burst them well since The above kinematic one the information blue would can sequence expect provide different angalaxy insight morphologies, into harassment dynamics the scenario. and trigger metallicity of Hydrodynamical the profiles simulations ULIRG inwith have a the been major ultraluminous successful activity merger, being at minor triggered merger simulating in or these ato number submm the of galaxies ways. observations at to The z=2 outputs identify of whichin the ULIRG simulations the can real trigger be Universe in directly and compared the thus simulations help produces to galaxies understand which how best these match galaxies those form observed and evolve. Abstract The recently-completed Sloan Digital Sky Surveyof (SDSS) the has universe. been immensely We useful presenttrating for the on studies the latest of projected measurements two-point the correlation of large-scale function. galaxy structure clustering The clustering on SDSS from is galaxy particularly the properties, suitable and full for we investigating SDSSusing the focus halo DR7 dependence occupation on redshift of distribution the survey, modeling, dependence concen- and on showframework. color that and most This luminosity. of provides the We insight observed interpret trends onformation our can theories. the be measurements relation naturally between understood in galaxies this and dark matter halos and informative tests for galaxy 5.46 Galaxy Clustering and Dark Matter Halos Galaxy Formation, Durham, Poster Programme dis- λ ESO - Garching value. We also find λ , with bright (massive) r . We finally correlate the M 3 The University of Sydney ∼ z values and associated dispersions, while λ Mrs Margherita Bonzini [email protected] Mr John Ching [email protected] Korea Astronomy and Space Science Institute at all magnitudes, a behaviour probably imposed λ , which we estimate approximately through simple dynamical 168 λ Jy sensitivity of our survey, we are able to detect not only the radio loud µ [email protected] Dr Bernardo Cervantes Sodi radio sources, we use a multi-wavelengths approach to separate AGN from star forming 900 values and a broader distribution. A more striking difference is found when looking at ∼ λ cuts, while the spin of non-AGN galaxies presents an anti-correlation with r M for AGNs and non-AGN galaxies, the AGNs showing typically low . For AGN host galaxies we compute the mass of the supermassive black holes and find that this value tends to λ λ Jy level. From a sample of non-AGNs present higher galaxies having low spins, AGN host galaxies present uniform values of Feedback models suggest that radio-loud AGNtwo accrete modes material are in differ two in distinctselected modes, their galaxies a feedback in hot-mode mechanism, the and Galaxy stellar a and population, cold-mode.and Mass redshift cold- Assembly These mode and (GAMA) accreting survey, environment. radio-loud we AGN compare Using to the a test 5th sample the nearest of neighbour environmental radio densities dependence. of hot- Abstract 6.5 Local Density of hot- and cold- mode accretors tributions in thin by the fact that most late-typethat AGN the galaxies fraction present of a AGN narrowdecreasing hosting range in galaxies coluor in with our a samplebe typical strongly higher constant depends for on low the spinthe galactic galaxies, luminosity spin, even - increasing at black fixed dramatically hole mass luminosity, for relation. a result that could account, to a certain extent, for the spread on Using an extensive sample ofmomentum galaxies distribution selected of from AGN the with Sloan non-AGNthrough Digital hosting the Sky by dimensionless Survey late-type angular Data galaxies. momentum Release parameter To 5, this we end compare we the characterized angular the galaxy spin Abstract considerations. Using a magnitude limitedbutions sample, we of find a considerable difference when comparing the empirical distri- 6.4 The galactic spin of AGN galaxies accretion level of these radiomasses selected and morphological AGN appearances. with the overall properties of their host galaxies: star formation rates, stellar Abstract Recent theoretical and observational studies agree onfeedback the mechanism importance to of their radio emission host fromout galaxies. active to galactic high Key nuclei redshift ingredients are (AGN) to an as unbiased studyRadio AGN the observations sample as co-evolution are well between by as far central large less auxiliary SMBHX-ray data affected and band, to by galaxies which determine dust the allows extinction galaxies us physical compared to20 properties. to select cm similar a of surveys more performed the complete in Extended AGNµ the Chandra sample. optical Deep and We Field the have South therefore (E-CDFS) embarked to in explore a deep the VLA faint survey end at of the radio population, down to the 6.3 The Sub-mJy Radio Population in the E-CDFS: star formation and BH accretion galaxies looking at the ratio between theirX-ray FIR luminosity and and radio morphology. emission, Thanks their flux to ratio the in the optical and radio bands, the level of AGN, but also significant population ofcompleteness radio of quiet our objects sample, according we to the trace standard the classification. evolution Using of the the high AGN redshift luminosity function up to Galaxy Formation, Durham, Poster Programme INAF University of Florida Dr Fabio Fontanot [email protected] Institut d’Astrophysique Spatiale Prof Fred Hamann fhamann@ufl.edu galaxy should host a bright radio source, while ⊙ M Cédric Collet [email protected] 11 10 > ∗ M 169 mass and hierarchy (i.e. centrals or satellites) become available. In this paper, we DM dark matter halo and/or ⊙ M emission lines, OIII line strength and radio power). We demonstrate that all models used in M α 2-3 with rest-frame optical imaging spectroscopy obtained at the VLT. We search for outflows 12 ∼ 10 > DM , parent halo ∗ M M Quasar absorption lines provide valuable information onthe a central range of source, quasar ambient environments, gas includingare powerful in all outflows the important from host pieces to galaxies, the and,whether puzzle quasar perhaps, of outflows the quasar/SMBH/host carry gaseous galaxy enough evolution. remnants kineticcentral of energy SMBH, For as to example, recent described regulate by we galaxy some star can recent mergers. formation models. addressenvironments in the We These to can the question also further hosts of measure constrain the and galaxy amounts halt and merger/evolution metallicities furtherphenomena, models. of infall gas including I in onto will the 1) the extended describe an several studies HST/COSquasar-driven of spectroscopy outflows, quasar program absorption 2) line to an estimate outflowground-based the spectroscopy modeling mass to effort identify loss to and rates derive constraingalaxies and physical their and/or properties kinetic merger energetics for energy remnants. and the yields particular acceleration of lines mechanisms, that form and in 3) the extended host Abstract 6.8 Quasar Absorption Lines as Probes of Quasar-SMBH-Host Galaxy Coevolution only a small (few perdepend cent) strongly fraction on the of mass galaxies of belong theenvironments parent to halo in this mass data. in class the Our in models, results the whileof strong highlight data. the and that weak most In the radio promising addition, distribution galaxies discriminants are radio of between found AGN brightness in different activity similar is gas as expected accretion a schemes. to function of stellar mass provides one Abstract AGN feedback is believed to play an importantof role their in stellar shaping masses a variety and of star observedfeedback formation galaxy is rates. properties, believed as to In well play particular, as a in the crucial evolution role theat in current regulating low theoretical star paradigm formation redshift. activity of in galaxy galaxies Onlyon formation, residing AGN in stellar in relatively mass massive recent haloes, years,compare however, the fractions has of galaxies detailed belonging to statistical differentfrom activity information four classes (star-forming, on different AGN and and the radio independently dependence active) developedproperties with semi-analytical of into predictions observables models. galaxy (H We activity adopt empirical relations to convert physical 6.7 Galaxy activity in Semi-Analytical Models this study reproduce the observed distributions ofand galaxies the as a strongest function of radio stellar sourcesHowever, mass model and are predictions halo differ preferentially mass: from associated star observational measurements forming withthat in galaxies almost many low-mass every respects. and All high-mass models used galaxies/haloes, in our respectively. study predict Abstract There is growing evidence thatthe supermassive formation black of holes massive may galaxies playinterstellar at gas a in high crucial their redshift. host role galaxies. for Our Toradio galaxy this work galaxies evolution, end, at focuses we in redshifts are on particular z studying quantifying the during and kinematics the of other effects the signatures of ionized of gas radio-loud in feedback AGN 9may from moderately on plausibly the powerful the quench supermassive star black formation. holesrare, in AGN-driven outflows the radio have centers galaxies previously of at been these similarsignatures? identified galaxies in redshifts. This to would very evaluate suggest powerful, Do if that but mechanical, the galaxies also jet-driventhe AGN with AGN very early feedback evolution less may of well powerful, massive be and a galaxies. fairly more common common phenomenon during radio sources exhibit similar a Common Phenomenon? 6.6 Mechanical AGN Feedback in Moderately Strong High-Redshift Radio Galaxies: Galaxy Formation, Durham, Poster Programme ) 3 − ESO 1 NOAO ∼ z Msun – has important 6 Dr George Hau [email protected] 10 and 4 Dr Jeyhan Kartaltepe [email protected] 10 ) are all interacting and merging galaxies. ⊙ Max Planck Institute for Radio Astronomy L 12 10 > IR L 170 Dr Marios Karouzos [email protected] In the local universe, Ultraluminous Infrared Galaxies (ULIRGs, Abstract 6.11 The Role of Galaxy Mergers in High Redshift ULIRGs Abstract It has long been argued that there mightthe be a AGN causal population. connection between Together nuclear with activity and possiblein merger feedback events, the mechanisms, at these least standard for effects paradigm part highlight of of thefield, galactic importance we of evolution. study active the galaxies Using close the environmentdense environments new of around AGN VISTA-VIDEO them. (selected near-infrared Results in show survey radio X-rays, andOn data mid-infrared, mid-infrared the of selected and contrary, AGN the radio), to X-ray have looking XMM-LSS selected an for AGN excess of indications appear close of to companions. over- populate consistently under-dense environments. VISTA-VIDEO survey 6.10 Merger-driven nuclear activity in galaxies: Close environment of AGN in the To date, studies of ULIRGssample at sizes. high redshift Some have studies have foundfraction found a of that variety morphologically mergers of normal still results or dominatestructure due clumpy the at to star high galaxy their forming redshift morphology varying disks. since while selection itin others Near-infrared effects probes have the the imaging and found rest local is small a frame universe. crucial high optical forULIRGs. light Here, interpreting of These we galaxy a galaxy galaxies present and are the thusthe selected results we GOODS-Herschel based can of coverage compare on a of directly their morphological GOODS-S. to infraredthe We analysis studies luminosities same visually of measured classified redshift a using all and sample of 100 H ofcompare the and band our high ULIRGs 160 magnitude results as redshift to micron range well those ( data using as from from ACSand other a increased and classifiers comparison as sensitivity WFC3 sample well of data with as WFC3 from severalmergers over the automated among NICMOS classification GOODS high methods. for and redshift this The ULIRGs CANDELS high large consistently surveys. resolution sample for the of We first objects time. allows us to investigate the role of galaxy Abstract The existence of intermediate-mass black holes (IMBHs)– black holes of masses between black hole? 6.9 The hyperluminous X-ray source HLX1 – evidence for an intermediate mass implications for the formation and evolution of starthe clusters M-sigma and relationship, supermassive until black recently holes. an Although unambiguous IMBHs identificationHLX1 are has predicted located proved by elusive. in the The hyperluminous S0 X-ray galaxyfor source ESO their 243-49 existence. (Soria et Using alhave the 2010, performed Magellan Farrell deep telescope, et VLT/VIMOS al we UBVRI 2010)on have photometry represents the identified of one stellar the of HLX1 populations optical the and of counterpart strongest itsHLX1 the candidates for and host host the HLX1. cluster, star host the cluster. galaxy. Furthermore, constraints I we on will the nature present of the HLX1, latest and analysis examine the connection between Galaxy Formation, Durham, Poster Programme ) at 8 . 21 < Rutgers University of Massachusetts [email protected] Dr Peter Kurczynski %) in the mid-IR. With our large spectroscopic 50 > [email protected] Ms Allison Kirkpatrick 171 ? %) of our sample of (U)LIRGS are dominated by an AGN ( 3 30 in the Extended Chandra Deep Field - South (ECDF-S). To avoid AGN, we eliminate 12% of the original sample 3 ∼ < z < < z < Abstract We determine Star Formation Rates (SFRs) in a sample of color selected, star forming (sBzK) galaxies (K(AB) 1 6.13 Estimating SFR from X-ray through radio: Which method works best at sample and wealth of multi-wavelength data,explore we infrared are color-color in diagrams a to unique identifytechniques position different that to diagnostics cleanly study of separate in the the detail AGN SF thethe and and nature nature starburst AGN of of dominated these activity. (U)LIRGs sources; galaxies. We when these We by found diagnostics spectra several studying are are useful useful the not tools details available. to of determine properties We spectral of look properties these for (such galaxies evolution as using inmorphology, relative near-IR our PAH strength emission, imaging sample of dust with from temperature) PAHs, redshift HST. evolve absorption, and Our as etc.) luminosity the goal AGN is becomes and to more the luminous map morphological in out the how mid-IR. the properties of a galaxy (e.g. 1 that have X-ray detectionsstacking in analyses Chandra in Spitzer-MIPS catalogs. IR, APEX/LABOCA4 Photometric submillimeter, Ms VLA redshift CDF-S) and data. binned, GMRT We radio average includeSpectral and flux averages Energy Chandra of Distributions X-ray densities (SEDs). aperture (including are fluxes We in determine measuredUV, MUSYC total with UBVRIz’JHK radio IR images luminosities, and to compare X-ray determine SFR calibrations UV-through-radio estimator, wavebands, from SFR(IR+UV), and FIR, to 24 find within micron, errors preferredthat for calibrations 24 dust micron-only for corrected and each UV X-ray SFR and waveband.of estimates the Luminous should preferred We Infrared be radio Galaxies. used find SFR with consistency caution. calibration. Average with Our sBzK our results IR show luminosities best are equal to those Abstract (Ultra) Luminous Infrared Galaxies (ULIRGS) arestellar more mass buildup numerous in at today’s high-redshift massive and galaxies.(AGN) thus activity, (U)LIRGS contribute show indicating significantly signs a to of link the bothtroscopy between star is formation growth unique (SF) of in and the that active stellar it galacticAGN nuclei allows mass components us and of to the a simultaneously galaxy. central probe We black thesample have contribution hole. compiled of to a 150 Spitzer the rich (U)LIRGS infrared mid-infrared catalog luminosity in spec- of from the multi-wavelengthwe both data GOODS-N decomposed SF (HST, the and Spitzer, and mid-IR ECDFS Herschel) spectrum fields for into for aportion contributions large which ( to we mid-IR have luminosity Spitzer from IRS SF and spectroscopy. AGN For components. each A source, significant 6.12 AGN and Star Formation Activity in High Redshift (U)LIRGs Galaxy Formation, Durham, Poster Programme University of Turku University of Groningen Ms Heidi Lietzen heilie@utu.fi 18 arcsec, which resulted in the detection of ∼ [email protected] Mr Federico Lelli Institute for Astronomy, University of Edinburgh 172 [email protected] Dr Michal Michalowski 90% completeness of identification, which allows us to construct for the first time the unbiased ) millimetre survey to date at the resolution of ∼ 2 150 millimetre objects. We identified their counterparts at other wavelengths using the deep radio and 24um data and Understanding of the redshift distributionimportant aspect and of the the galaxy formation properties and evolution. offields, We the the address this dust-enshrouded, widest issue using (0.7 highly the JCMT/AzTEC deg star-forming survey of galaxies the SHADES is an sample of dusty galaxies.the We implications will of present these their results redshift on our distributions, understanding star of formation the rates galaxy formation. and stellar masses and discuss Abstract 6.16 Complete Sample of Millimetre-Selected Galaxies in the SHADES Fields ∼ completed the selection using a novel andreached successful an method unprecedented based on near-infrared fluxes and optical colors. In this way we Abstract Through the morphology-density relation we know thatThe the role properties of of feedback galaxies from depend an on active theirgalaxies nucleus large-scale can may environments. give be support important in to galaxy theof evolution different and active models the galaxies of large-scale evolution. on environments of supercluster In active environments, my scale. talk while I In radio-quiet will our quasars show recently-submittedsuperclusters our are paper latest are usually we results usually on found in older the that emptier than environments in radio galaxies regions. galaxy galaxies in evolution prefer void than It high-density radio regions. is galaxies,low-density This the known environments. low-redshift can that quasars explain are galaxies our more in results: likely the to If be dense quasars in are cores younger activated galaxies, of and earlier therefore, in 6.15 Large scale environments of nearby AGN Abstract Starburst activity plays aquench key intense role star in formation are the stillgalaxies, formation poorly characterized and understood. by evolution high Blue specific Compact of Dwarfs starburst galaxies. (BCDs) formation is occurring are rates, under The nearby low physical starbursting metallicities mechanisms and low-mass and chemical thatBCDs conditions large show trigger, similar amount strong to of sustain concentrations those of gas. of and HI high-redshift Therefore,gas with galaxies. the are steep In star- not velocity their observed gradients. central in regions, These moredynamics morphological quiescent and and dwarfs. kinematic the properties This compact of points distribution the toby of a focusing luminous close on and connection those dark between galaxies matter. themation that starburst, on have We the their been are large-scale stellar resolved performing gas populations into ametal-poor and single HI galaxies star stars study known. formation by of I histories. HST will a present observations, I samplethe evidence which will of presence for provide discuss BCDs an of the detailed interaction/merger an first infor- between extended two resultsflow gaseous extremely on of gas-rich tail gas I dwarfs. may from Zw Also, the be 18, IGM. interpreted one either of the as most a result of the tidal interaction or as a massive cold 6.14 Dynamics of Starbursting Dwarf Galaxies: I Zw 18 Galaxy Formation, Durham, Poster Programme University of Sheffield University of Tasmania Lawrence Berkeley National Lab , QSOs; 50,000 of which will be in 2 z > Dr Stanislav Shabala [email protected] [email protected] Dr Nicholas Ross Dr Cristina Ramos Almeida c.ramos@sheffield.ac.uk 173 ). BOSS is assembling an unprecedented sample of high, 3 30%) when similar surface brightnesses are considered. Our results contrast with those found for lower − ∼ 2 ∼ z Abstract I discuss the effects of kinetic AGN feedbackdifferent on picture the emerges colour evolution for of low galaxies intype and II local high-power (edge-brightened) groups sources and radio show clusters. much AGN. redder A Galaxies colours fundamentally thanthe located neighbouring radio within galaxies source. that the are By not lobes contrast, spatially of no coincident with the similar powerful effect Fanaroff-Riley observed is seen colours near near Fanaroff-Riley typeshock FR-II I overruns (core-dominated) radio radio a sources sources. galaxy. are Moreover, these consistent A clusters with carry similar an star analysis imprint formation of oflow-luminosity past being clusters radio AGN truncated with feedback. sources as no AGN with activity the short detectable inradio duty expanding radio the sources cycles. low-redshift emission bow is Universe an suggests These is important results that predominantly driver show driven galaxy of by that, galaxy colours despite evolution in even their in rarity, the feedback local from volume. powerful hand by summer 2011. As such,we it will give be the the initial premier spectroscopic results datasetclustering, from at as high-z measured the for by investigations the the into remainder luminosity of function theto this and new observational decade. the measurements measurements 2-point Here, of correlation of the function the respectively. obscuredSemi-Analytic quasar population We Models by relate number (e.g. these Hickox density results et Fanidakis and al. etlinks al. (2011). between central We 2011a,b), black also in hole place order formation, them to galaxy in begin formation the and to context AGN?” answer of the recent AGN question of “what *precisely* are the 6.19 AGN feedback and colour evolution of local galaxies Abstract We present key early resultsthe definitive from measurement the of SDSS-III:Baryon the Oscillation(redshifts luminous optical Spectroscopic AGN Survey (Quasar) (BOSS) Luminosity Quasar Function, Survey; at the namely height of the quasar epoch Luminosity Function and its constraining power for AGN Semi-Analytic Models 6.18 The SDSS-III BOSS Quasar Survey: The Definitive Unobscured Quasar luminosity AGN (as e.g. Seyfert galaxies), whereminor the interactions. nuclear activity However, is more these likely results triggered can byAGN be internal are secular reconciled processes on triggered and the in basis mergers/interactions, ofhosted since galaxy in evolution: larger less in massive fuel massive galaxies, supply galaxies, do is powerful not required. require such On a major the event other to hand, be low-luminosity triggered. AGN, Abstract Despite speculation that nuclear activity in galaxiesthe may true be nature triggered of by the mergers link. andthat interactions, I very 80-85% will little of present is their known deep galaxy about Gemini/GMOSphologies hosts imaging are show of signs consistent powerful of the radio interactions galaxies AGN atquiescent and relatively being ellipticals, quasars high we triggered which levels find at reveal of that any surfaceescent the brightness. stage ellipticals percentage The ( of of galaxy the morphological mor- disturbance interaction. in PRGs By greatly comparing exceeds with that a found control for qui- sample of 6.17 The triggering mechanisms of powerful AGN: evidence for galaxy interactions Galaxy Formation, Durham, Poster Programme Caltech 200 proper kpc). ∼ 3’ of one of 15 of the Durham University University of Tokyo ∼ –3 25” ( 2 ∼ ∼ Mr Ryan Trainor [email protected] z , as probed by the distribution of their 7 . 2 Prof Ray Sharples [email protected] [email protected] Dr Masayuki Tanaka ∼ z 174 ) of star-forming galaxies, where each galaxy lies within 2000 ∼ spec N We present an analysissurrounding of galaxies. the environments We of measurespectroscopic hyperluminous redshift the QSOs survey galaxy ( at distributionbrightest in QSOs three at dimensions these by redshifts.overdensity combining in We imaging the find data galaxy that distribution with the withWe a average furthermore a use large QSO velocity our scale in dataset to of our obtain 500function sample estimates km/s on of is small and the associated transverse galaxy-QSO a scales, cross-correlation in transverse through function redshift scale which andgalaxies we galaxy of with at autocorrelation can a infer these and significant compare redshifts. thegalactic halo Finally, peculiar mass scales velocities the of and precision QSOs thereby and of constrain star-forming QSOs. the our Taken dynamical spectroscopic together, mass these scale redshifts measurements of allows the willronments us larger help or groups answer to are or the merely constrain clusters question observed the containing at of these special distribution whether times QSOs of in inhabit an extremely otherwise unique normal envi- process of galaxy evolution. Abstract 6.22 Galaxy Distributions as a Probe of QSO Environments at Abstract We characterize the relationship betweennovel method AGN to activities identify AGNs and that allows host us (1)et galaxy to al. identify properties 1981) 3x does, more using AGNs (2) data than to the from estimate commonlydue used SFRs SDSS. to BPT of diagnostics star We the (Baldwin formation host develop and galaxies a with extractwide a pure range factor AGN of of emissions, ionization 2 states which accuracy, and are andto (3) that crucial characterize to motivates to AGN subtract us characterize power emission to over AGNs. line introduce a fluxes Wein a wide find massive new range that of parameter, galaxies, AGNs AGN a (b) activities. show sum the a of Basedblack AGN [OII] on hole power and these growth increases new [OIII] rate developments, with luminosities, (Eddington we increasing parameter)that find SFRs increases is, (a) of with black AGNs the holes increasing reside grow galaxy host in growth galaxies,formation growing rate and and galaxies. (specific the most This star down-sizing importantly, result formation in (c) may rate) AGN provide the – activities. a physical link between the down-sizing in galaxy star 6.21 Growing black holes in growing galaxies Abstract We present the current status offor KMOS, the the ESO first VLT. multi-object KMOS near-infrareddiscuss is integral the design in field drivers spectrograph an for under advanced KMOS and construction integrationtime some phase observations. of the and key commissioning science programmes is that predicted will be to undertaken start during the in guaranteed Spring 2012. We 6.20 KMOS: A New Observational Tool for Studies of Galaxy Evolution Galaxy Formation, Durham, Poster Programme ) with the 2 . 0 (accompanied 9 . 0 z < ∼ Uppsala Universitet z 60 have associated archival ∼ Northwestern University - CIERA ) maps of the CO(3-2) gas taken at the ′′ 4 . (for which 0 1 . 0 ∼ Ms Beatriz Villarroel [email protected] ∼ Harvard-Smithsonian Center for Astrophysics z Dr Laura Trouille [email protected] 175 Miss Vivian U [email protected] 1”, or 500pc, apart) in gravitating towards the dynamical center of the ∼ 3000 SDSS DR8 post-starbursts at ∼ 200 post-starbursts from the DEEP2, zCOSMOS, and OPTX surveys at ∼ by deep Chandra imaging). A keypopulation benefit synthesis modeling of provides studying an post-starburst estimate galaxies of the isthe time following that since questions: they the 1) peak are Does star-formation natural a event. chronometers; visuala In detailed inspection this for trend study near-neighbors we with and address tidal post-starburst disruptions age? inand our low-redshift 2) what sample show Do does post-starbursts this move tellproperties across us (for optical about individually emission-line the diagnostic detected time-delay diagramsformation sources between activity? as and starburst We they will activity on age discuss and average theof AGN implications via recent of fueling? AGN-starburst our X-ray simulations. results stacking) 3) on galaxy Are correlated evolution post-starburst with studies X-ray and time place them since in peak the context in star most statistically complete sample toquasar-galaxy associations date with using spectroscopically the measured seventh redshiftsstar-formation rates, data to oxygen calculate release abundances, how dust of extinction surface and the densitiesWe ionization Sloan changes of also as Digital identify galaxies, a and colors, function Sky of exclude Survey. the theOur distance AGN to results We from the suggest quasars. our have that main used there galaxychanges is sample of a and ionization, significant calculate surface dust increase density of extinction of the and different galaxy metallicity, galaxy surface but types. density might around observe quasars. a slight We see change no in significant color and star-formation rate. Abstract The impact of quasars on their galaxyThe neighbors aim is of an important this factor work in the is understanding to of the characterize galaxy for evolution the models. first time the environments of quasars at low redshift ( 6.25 In the Neighbourhood of Tame Monsters Chandra data) and the Abstract NGC 6240 is a late-stagegas precedes advance its merger stellar harboring component two counterparts AGNs ( that have yet to coalesce, but its central dense molecular 6.24 High-Resolution Molecular Gas Dynamics in the Center of NGC 6240 system. Building on previous submillimeter work, we present high-resolution ( Abstract Post-starburst galaxies have recently undergoneexceptional an and rare abrupt stage cessation in of galaxyinto evolution active early-types. is star thought While formation to it occur (within is duringthat 20–500 poorly the galaxy-galaxy understood Myr). transition tidal what from causes interactions gas-rich, This the star-forming ortriggering galaxies abrupt mergers intensive end trigger star of the formation their starburst star may inevolution formation, also many of there cause the of is strong properties strong these fuelling of evidence galaxies. onto post-starbursts,connection. a we This The obtain central same use insights supermassive of mechanism into black post-starbursts the for hole. as originHere probes of By we is the studying compare only red-sequence the results now and feasible from the with AGN-starburst the the advent of large optical spectroscopic surveys. 6.23 Building Up the Red-Sequence: The AGN-Starburst Connection Submillimeter Array. At this spatial scale,the we turbulent resolve nature asymmetric gas of fluxalong the peaks with molecular lying local disturbances. inward gas. of A the simple A geometry-basedhydrodynamic two scenario galaxy-merger AGNs general is simulation and proposed velocity models, confirm to gradient the explain the continual alonggas observed development behavior gas the of dynamics at axis which based these will on in small shed scales. between light on the the two physics nuclei behind is noted Galaxy Formation, Durham, Poster Programme Yale University Ghent University University of Trieste [email protected] Mr Pedro R. Capelo [email protected] Dr Weiguang Cui . Over the GIMIC halo mass range we resolve best, Miss Annelies Cloet-Osselaer [email protected] sun M 1 − h 14 176 10 − 13 10 relation), and of the Tully-Fisher relation. star M , the central galaxies in the fossil groups show similar properties as those in ordinary vs. sun halo M 1 M − h 13 10 × 0 . 4 ∼ 12 10 × 0 . 9 groups, in terms of age, metallicity,fossil color, groups concentration, as and transient mass-to-light phases ratio. in Theseobjects. the results evolution support of an ordinary interpretation galaxy of groups rather than forming a physically distinct class of we here investigate fossil groups identified in theulations hydrodynamical of simulations five of regions the GIMIC in project, the whichfrom Millennium consists a Simulation of deep resim- (MS) that void are to characterizedas a by well proto-cluster different as region. large-scale a densities, conditional For ranging luminosity comparison,use function we a approach. also spectral We consider synthesis identify semi-analytic code galaxies models in tothe built the derive thermal GIMIC on bremsstrahlung their simulations top emission optical as of of properties. groups the the ofproperties The gas MS, stars in of X-ray and the luminosity fossil host of groups halos, the in neglecting groupsand the metallicity is trying effects. theoretical estimated to We models in focus identify and terms on observational possible of that comparing results, dependencies the the highlighting on optical the environment fossil differences for fraction betweenis which shows them, evidence our no for approach clear a is environmental weakgroups particularly dependence effect in well in GIMIC in set-up. also either the shows of GIMIC We angions. the hydrodynamic find environmental Combining simulations. semi-analytic effect, the making models, optical X-ray Interestingly, but and bright the X-raya there groups X-ray selection function disproportionally criteria of luminosity rare for halo in distribution mass, fossil low-density of at groups, re- a we mass find scale that of the around fossil fraction exhibits a peak as Abstract models 7.3 Properties of fossil groups in cosmological simulations and galaxy formation We show results based onDM a halos, set as of well Nbody-SPH as simulations DM-onlycooling of simulations. and dwarf metal Our enrichment. galaxies, Nbody-SPH both For simulations the withprofile include cusped initially is star halo used. cusped formation, we and stellar Both employ feedback, initially the dark radiative NFWagreement cored matter profile; with, halos for observations have the of been cored dwarf proven halo galaxies togas a be in dynamics Kuz’min stable. the and Kutuzov Local star (KK) Our Group formation simulations and reveal aretion, in a compared unlike nearby our gradual with, clusters. DM-only transition and control from are The simulations. in a NFWwithout The good cusped simulations KK gas density including simulations dynamics distribution on and to the other star aon hand cored formation. remain the density relatively baryonic Besides distribu- stable, component. differences both The with in simulations and circular the with evolution velocity NFW halos of than have DM the a distributions simulations lowertions we star with in can formation a close rate, also agreement KK lower see with metallicity, halo effects and detailed(particularly of lower the observations comparable slope of mass of dwarf the and galaxy scalelength. stellar populations, This of the brings dark-matter our halo NFW occupancy simula- Abstract 7.2 The dwarf galaxy dark-matter halo occupancy Abstract We report on the investigation ofusing the 3D effects mesh-refined of simulations, AGN and incorporatingand SN physics heating, feedback and such on injection as the of momentum. evolution gravity of Wethe (from power, explore the dark several the ISM duration, feedback matter of scenarios, the and early-type location studying and galaxies, a stars),time the parameter by and radiative geometry space radius, of where cooling by the we studying outflows. vary the We fateinto study of X-ray the the energy observables ISM, deposition, and its both temperature compare as and those a pressure to function profiles. of current We observations. also translate physical properties 7.1 Feedback in Early-Type Galaxies Galaxy Formation, Durham, Poster Programme MPE kpc scales and the ∼ Fermilab, UChicago Dr Fabrice Durier [email protected] Dr Robert Feldmann [email protected] Universidad Complutense de Madrid (Spain) 177 Dr M. Carmen Eliche-Moral mceliche@fis.ucm.es H2-CO conversion factor. Cosmological simulations often use a fixed densityformation threshold is criterion in observed the to sub-grid modeling takedepend of place on star the within formation. presence molecular Since of star molecular clouds hydrogen.on a the In potentially metallicity this and more way, the the physical interstellar modeling UVcosmological approach of radiation simulations star is field formation of of to acquires galaxies. the an let ISM. explicit In I star dependence will particular, formation present I some will implications discuss of such the an star approach formation for laws on 100 pc to Abstract 7.6 Star formation in cosmological simulations of galaxies Abstract Recent observations show that inner discs andpoints rings to (IDs the and IRs) relevance are of notminor other preferentially mergers formation found in in mechanisms barred the besides galaxies, formation the ainvestigated of traditional fact the these that capability bar-origin inner of scenario. minor components mergers (ICs), In to triggerbody while contrast, the simulations, often the formation analysing of invoked, role IDs the is of and remnants IRs still in resultingand poorly spiral from galaxies understood. primary minor through galaxy collisionless We merger N- models experiments have run (Sabsatellite with material. or different A Sc). orbits, wide mass morphological zoo ratios, Allbars, of the and ICs combinations has simulated of been minor them), obtained (including all mergersbe IDs, with develop IRs, structural deduced pseudo-rings, thin and through nested kinematical rotationally-supported IDs, the properties nuclear ICs similar featuresin to out that observations. many of they real Their imprint existence cases. can toefficient The the orbital realistic isophotal circularization density profiles and ratios disruption and between than kinemetricencounter, in the maps these previous merging of processes studies. galaxies the give Combined used final place with makemodels the remnant, to prove the disc as highly that satellites resonances aligned minor to induced co- mergers by experiencewithout the and are more requiring counter-rotating an strong efficient ICs dissipation mechanism in or to themuch noticeable form more remnant bars, complex rotationally-supported and centres. than stellar suggest just The ICs that bar their in present triggering. role spiral in galaxies, the formation of ICs must have been mergers 7.5 Formation of stellar inner discs and rings in spiral galaxies through minor Abstract We perform simulations of feedback fromtime supernovae that, with in smoothed the particle absence hydrodynamicspropriate (SPH). of time We radiative integration. show cooling, for concordance In the of order first scheme, thermal to we and implemented preserve in kinetic a the feedback high GADGET-2(2009). is level code achieved We of a apply when energy the modified using conservation limiter version to an when ofalso general ap- using the to test enforce the cases, time-step a and limiter hierarchical prompt find response proposed time-step necessary, of by the notback system Saitoh only events to to & the enables ensure energy Makino a us perturbation. fast to The information achieve methodinto propagation, proposed energy but only here conservation to one at handle strong particle. percent feed- level Finally,high in all we resolution, tests, show simulations even that, of if even an allconcordance. if individual the Animations cooling available supernovae available energy processes explosion at: is are with http://www.mpe.mpg.de/ injected taken fdurier/Concordance/ the into different account feedback and methods providing are a still sufficiently reaching 7.4 Implementation of feedback in SPH: towards concordance of methods Galaxy Formation, Durham, Poster Programme Observatoire de Paris University of California, Santa Cruz University of California Santa Barbara [email protected] Miss Anaelle Halle Miss Javiera Guedes [email protected] 178 fi[email protected] Dr Kristian Finlator Abstract Nucleosynthesis and the CMB predict baryons representsare 4% not of observed. the Dark matter-energy content baryons ofulations are the and therefore universe, their an but comparisons interesting 90% to lead of observed to them form galaxy address properties. a some Molecular problems significant hydrogen encountered gas, part in difficultinfluence of numerical to of sim- observe, these dark could dark baryons especially on baryons. galaxy evolution. We use simulations using the TreeSPH N-body code Gadget to study the 7.9 Galaxies and the Missing Baryons Abstract The successful formation of Milkybaryonic Way-sized physics disks at in sub-grid cosmological scales, simulationsbriefly requires particularly review the gas some correct cooling, of treatment star theresults of formation, challenges complex of and that the supernovae have Eris feedback. plagueddetailed simulation, comparison numerical In between state-of-the-art three simulations this similar cosmological of talk, simulations simulation with flat I varyingthreshold. of resolution, will galactic star the I disks, formation efficiency, will formation and and focus star of will formation evolution on a present of the the the late-type effect baryon spiral these fraction galaxy, with parameters redshift, on and the the properties star of the formation satellites, history, and the the formation distribution of of metals. bar instabilities, the 7.8 Forming Massive Disk Galaxies in LCDM Abstract The last decade has producedfer an explosion a in wealth observational of constraints insightprocesses on into that galaxy fundamental regulate growth questions their at such stellar highperiod, mass as redshifts. advances growth the These in while form data coupling computing in of- their have whichtreatments gas enabled for gas reservoirs cosmological galaxy accretes to hydrodynamic growth onto their and simulations galaxies surroundings.outflows, feedback to and and in Over incorporate the mergers representative the remarkably feedback have same cosmological detailed reached volumes.self-consistent maturity, treatments Simulations and for that state-of-the-art photoionization account efforts feedback. for arestrong support Broad inflows, beginning for agreement to smooth between gas incorporate accretion predictions spatially-resolved, as andfor the improvement dominant observations in gas-delivery provides our mechanism, understanding but of lingering feedback. discrepanciesdominate indicate I galaxy room will growth discuss through current and comparisons future betweentributions efforts numerical to such predictions understand as and the processes observations the that of luminosityrelationship, fundamental and and galaxy mass dis- their functions, evolution the inaccretion ”main time. versus sequence” mergers of I in star-forming driving will stellarhistories. galaxies, illustrate mass how the In growth, the these mass-metallicity emphasizing near measurements the future, constrain needment JWST the for for will statistical photoionization trace relative constraints feedback. these roles trends on of To into staroutflows this smooth and the formation photoionization end, reionization feedback I in epoch, regulating will necessitating star use a formationhave within a self-consistent dominated the new treat- cosmological low-mass reionization. generation halos whose of Finally, stellar I calculations populationsfronts. will may to comment consider on future the progress relative on roles both of theoretical and observational 7.7 Numerical Simulations of High-Redshift Galaxy Populations Galaxy Formation, Durham, Poster Programme Durham University Columbia University UCL / Mullard Space Sci. Lab. Mr Jiaxin Han [email protected] Mr Cameron Hummels [email protected] [email protected] Dr Shigeki Inoue 179 Among nearby disk galaxies, theponents. galaxies have However, a in clean-cut the and high-zgalaxies beautiful universe, are shape: disk called they galaxies ‘clump have clusters’, in aN-body/SPH its which disk simulation have formation and how some stage a the star appear bulge clump forming shapeless as clustersconclusions clumps and main evolve in in into com- clumpy. this the its study. These current disk Clumps infant disk region. formednally galaxies in merge In like the into the this a clump Milky study, single clusters Way. bulge. I area sucked I investigate As group into found the by of galactic first two conclusion, center pseudobulges. main I by Properties found dynamicalbulges that of friction have this the an and bulge exponential clump-origin fi- (clump-origin surface bulge density bulge) resemble profile, shouldclump-origin an to be bulge oblate classified that forms shape into with of and thick significant pseudobulges disk rotation. closely. by However,as non-secular The on observationally evolution. the clump-origin suggested, The other the bulge hand, bulge stars the of areresult the as old Milky suggests as Way that the also The thick seems disk. Milky to Interestingly, the Way’s be clumps. a bulge pseudobulge, In may but the be stars formation the in stageinto clump-origin the of bulge bulge. disk disk are region, galaxies, Second, old. the while I This clumps growing found arewreckage that via disrupted of by a clumps mergers galactic disrupted thick with by disk other and the is spread clumps. tide. made out In from their As my own simulation, a stars nearly result, 80% the mass disk of thick is disk made was up made from from clumps. the stars which are Abstract 7.12 Thick disk and pseudobulge formation in a clump cluster Abstract Cosmological hydrodynamical simulations of galaxy formationmentum have in long the been baryonic plagued component byficient of the resolution disk spurious and loss galaxies. of incorrect The angular prescriptionsconduct culprits mo- for several of star high-resolution, this grid-based formation angular AMR and momentum simulationsproblem problem stellar using by appear feedback the systematically to in enzo modifying be code. the various insuf- simulations.and We simulation criteria, investigate parameters In the supernovae including angular feedback, this spatial momentum and work, resolution,quite the star we complex baryonic formation and equation efficiency there of is state. no single Our parameter results responsible indicate for that this the effect. problem appears to be 7.11 Investigating the Angular Momentum Problem in Disk Galaxy Formation Abstract We introduce a new codesimulations. based Here dark on matter the subhalos are mergermerger defined hierarchy hierarchy as of of self-bound subhalos remnant dark and of allow mattermerger dark growth hierarchy matter halos hence of halos. allowing satellite to mergers We subhalos among find keep satellites. through and fullof accretion Local record accretion stripped from trace of of mass its background dark the is subordinate mass is matter allowed. subhalos omitted in subhalos while Theand re-accretion the justification by in the of success these in treatments finding is theresolution provided complete of by subhalo simulation case output catalogue. has study Dependence also of of been the theshow examined. life that result We this of of compare Hierarchical this individual our Bound-Tracing tracing result subhalos (HBT) algorithm to code on thestrict is popular the able physical subhalo time to finder track well SUBFIND resolve of and subhalos subhalos’ inspatial high merger density searching history. environment when and constructing keep HBT source subhalos, also andwith features because the fast it author. is speed fully as parallelized. it This does code is not available need upon density request interpolation or 7.10 Resolving Subhalos’ Lives with the Hierarchical Bound-Tracing Algorithm Galaxy Formation, Durham, Poster Programme at = 6 35 . z 2 − to = M = 9 α z ) as sources of ener- and 6 Observatoire de Paris 15 . University of Leicester 2 z > − = L University of Nevada Las Vegas α Max Planck Institute for Astronomy [email protected] Miss Gillian James [email protected] Mr Benjamin L’Huillier [email protected] Mr Jason Jaacks [email protected] Mr Rahul Kannan 180 Galaxies in Cosmological SPH Simulations 6 . Our results suggest a significant population of small faint galaxies which are currently beyond z > 6 z > erg/s) high-mass X-ray binaries (HMXBs). We investigate the contribution of these HMXBs to the heating of 38 10 and steeper for ≈ X = 6 L Abstract According to the hierarchical model, small galaxiesassemble form their first mass and through merge accretion together from to form cosmicsimulations bigger filaments. have objects. Recently, emphasised In the parallel, increased that galaxies spatial a resolutionthe large of two the fraction cosmological phenomena, of we cold detect gasby baryonic can building and be merger dark trees. accreted matter by We structuresmerger galaxies. study in fraction the multi-zoom as In baryonic a numerical order function mass simulations, of to history the and compare ofthe environment track mass and galaxies the of them assembly, detected role the in in galaxy of particular the mass. at simulation, Wedense high and find environments. mass. that the the At accretion smooth smaller and accretion masses, mode gas dominates stripping is frequent, and quenches further growth in 7.16 Galaxy Mass Assembly: Mergers versus smooth accretion getic, neutral hydrogen ionising UV photons.( The remnants of these stars could continuethe to intergalactic be medium, important and as discuss X-ray a luminous simple method for including this effect in the modelling of galaxy formation. Abstract We investigate the idea ofshells DM found sub-halo in interaction the with HI regions thesub-halo of is gaseous not galaxies. disc able We as to particularly the produceamount concentrate holes, origin of on but of the on gas the the disc in recently contrary galaxy them it observed ICseem are gives to 2574. holes able rise be and to We to dependent on high push find the density that the gasa regions a gas mass, in small pure gas from the percentage density DM the disc. and of disc impact Halos the and velocity withnot observed of form a the the holes small holes major sub-halo. are and channel In predicted through shells. the by which cosmological The the framework, simulations. only size holes This are and formed leads lifetime or us of alternatively. to the conclude holes that either DM impact is 7.15 Interaction between dark matter sub-halos & galactic gaseous discs Abstract Massive stars may have played an important role during the epoch of cosmological reionisation ( Intergalactic Medium 7.14 The Contribution of High-Mass X-ray Binaries to the Heating of the z Abstract Using cosmological hydrodynamic simulations, we examine the photometric and physical properties of 7.13 Properties of our observational limits. Examinationlarge of numbers the they star are formation a primary rate contributor densities to of reionization. these faint galaxies suggest that due to their galaxies, such as the color-color diagrams, rest-frameing UV a luminosity fit function to and the galaxy Schechter stellar function mass we function. find By an perform- evolving faint-end luminosity/mass slope of Galaxy Formation, Durham, Poster Programme at 9 . 0 ∼ ) galaxies γ 2 . 0 using a high- and ⊙ 6 . M 0 T < / 15 ∼ Durham University B 10 γ km/s) bulgeless ( Max Planck Institute for Astrophysics CDM Model 150 Λ Mr Benjamin Lowing [email protected] > Max Planck Institute for Astronomy, Heidelberg . Cylindrical (2D) and spherical (3D) mass profiles circ V to present in a galaxy cluster of = 0 z = 3 z 181 Mr Chervin Laporte [email protected] kpc. The central slope of the dark matter density profile reduces to 5 Dr Andrea Maccio’ [email protected] at 1 − kms 300 ∼ . The system was then re-simulated to due to the interaction between the stars and dark matter. It reaches values of = 3 1 z kpc. This is in contrast to the uncontracted model run, where the stars dominate over the dark matter up 5 at dlnr < 1 / − kms dlnρ − 350 = Recent observations have pointed out a large population of massive ( Abstract 7.19 Formation of Bulgeless Massive Galaxies in the in the local environment aroundquestion our of the how Milky can Way.for the This merger-built CDM implies bulges. hierarchical that formation pure-disk Combininginvestigate scenario galaxies semi-analytical if are make models the far so presence of from many of galaxy rareCDM giant, these formation and model. bulges pure-disk raises with galaxies galaxies the high around with resolution the no SPH Local Group evidence simulation is we a true challenge for the otherwise successful I will present my recentexplore work the using heating the of Aquarius the simulations, Milkyin a Way disk set the via of solar substructure six bombardment. neighbourhood high-resolution TheWhile is dark origin the matter thought of only heating the to age-velocity simulations, is be dispersion to thought relation spiral a to waves, result the be importance of dominated of the interactions by withthere intrinsic Milky dark are processes matter Way enough substructures such disk is substructures as uncertain. present being scattering Itfraction in heated to is by haloes, the still through molecular observed and an heating. dynamic if clouds open I question the mechanisms. and attempt whether extracted interactions to transient answer deliver from this enough question simulations. by energy, using a to cosmologicallysimplified Reconstruction contribute realistic disk population a of interaction of significant subhaloes model their enable orbits us to as obtain they an upper pass limit to through the the level of centre heating of that substructure the could halo generate. and the use of a Abstract 7.18 Disk Heating by Substructure Bombardment to 18 kpc, in better agreementvelocity with dispersion, recent with observations a by value Newman et of al.. Moreover, it also matches their measured rising for the total, dark matter anddark stellar matter components dominates are the presented. mass Theof budget contracted the model in BCG run the is produced central too a galaxy∼ cluster high across in compared all which to the radii. observational measurements Moreover, in the galaxies projected of velocity similar dispersion masses, reaching a central valueγ of the innermost resolved radius for themodels uncontracted is and significantly contracted shallower runs than respectively. that forcombined The the kinematic central Navarro lensing slope -Frenk-White and of profile, X-ray the and observations it uncontracted of is in Newman excellent et agreement al., with thus recent alleviating the cluster core-cusp problem. Abstract We investigate the stellar and dark matter components from problem 7.17 Brightest cluster galaxies and the impact of dry mergers on the core-cusp resolution collisionless simulations presented bythe Ruszkowski cluster were & populated Springel. withdark spherical Dark matter model matter halo galaxies halos at with dominating and the without assembly accounting of for the adiabatic contraction of the Galaxy Formation, Durham, Poster Programme spirals were . We study the = 0 MPA-Garching z = 0 z Msun at 12 Swinburne University, Australia 10 , which is also when bars begin to form. and 5 Dr Benjamin Moster [email protected] . 11 10 = 0 remaining as central bulges. The first hints of a z 1 z > Dr Marie Martig [email protected] 182 progenitors is however complicated: half of these = 1 z , and are usually well in place by = 1 are less prone to bar formation. This suggests the possibility of using bar properties for z = 1 z galaxies with their . We study the interplay between bulge and bar formation, finding in particular that spiral galaxies properties and the merger and accretion histories. Unsurprisingly, the most disk-dominated cases = 0 = 1 z z = 0 z I present a novel approach tocosmological study merger galaxy trees evolution extracted combining from numericalgalaxy merger simulations an trees with N-body which semi-analytic provide simulation the models. and initialthe conditions We a galaxy for in use multi-merger semi-analytic the hydrodynamic main model simulations. branch of of Specifically, thewhen we merger galaxy tree evolve the in formation satellite a to simulation enters and create the include the largerexploit satellite halo the galaxies in using advantages this the of simulation at satellite merger the simulations properties time models (high predicted (cosmological resolution by background and the and detailed semi-analytic low treatment model.allows of computational In us the cost), this to gas and way physics) study integrate we and themass them semi-analytic dynamical resolution to evolution than create of standard a galaxies zoomed novelwe in hydrodynamical tool. find detail cosmological with good This simulations. a approach agreement lower Focusing withfurther computational on observations investigate, time Milky-Way for whether sized and the accreted systems a evolutioncentral satellite higher galaxy, of spatial stars and the and find can total that be this stellaran distinguished is accreted masses only satellite, kinematically and possible it from galaxy for is a not stars scale fraction possible parameters. formed of to ‘in determine the We in disrupted situ’ which satellites. in satellite Even the the if star a was star born. can be attributed to Abstract 7.21 Simulated Galaxy Merger Trees: A new numerical tool Abstract Cosmological simulations have unveiled twoof main cold modes gas from of cosmic galaxy filaments. growth:govern However, internal these hierarchical evolution simulations growth struggle and by to are take mergers aa into and key account new accretion ingredient small-scale simulation to mechanisms, which understand technique, galaxysimulation which formation and consists and performing evolution. in a We extracting re-simulation havetechnique the of thus makes merger developed this it possible and history to at accretion performgathered high history statistical a resolution studies of sample (150 and a of to pc). galaxy 30 explore the simulated The in parameter spiral low a space galaxies computational of cosmological with cost galaxy halo of formation. masses this We between have 7.20 Spiral Galaxy Formation in a Cosmological Context galactic archaeology. that were bulge-dominated at spiral structure begin to appearAn at identification of bulge-dominated at correspond to quiet merger histories. Inangular addition, momentum we varies find that with the time, angularusually are momentum very crucial of efficient the factors at accreted for building gas, disks, disk and with building. the the way The spheroids this formed accretion at of gas from filaments is however link between the Galaxy Formation, Durham, Poster Programme ) those 2 z < University of Nottingham . At lower redshifts ( 1 University of California, Santa Cruz − . At the end of an rapid early phase of = 2 z 262 kms ≈ [email protected] Mr Stuart Muldrew [email protected] Ms Lauren Porter Max Planck Institut fuer Astrophysik, Garching, Germany 183 [email protected] Mr Ludwig Oser kpc and central line-of-sight velocity dispersions of 1 < galaxies grow predominantly by the accretion ofmass-velocity smaller dispersion stellar relations. systems and We evolve find towards that the themergers observed evolution which local of is mass-size massive the and galaxies dominant can mode be explained of by accretion frequent for minor our stellar simulated galaxies. High-resolution simulations have suggested that someies, elliptical with galaxies are the formed dissipation through associated majoris with mergers essential star of in formation spiral reproducing producing galax- the a slopeSubsequent compact and minor spheroid scatter remnant. mergers of can, Including the in this observedcals turn, dissipation into size-mass preserve the and these large, Fundamental scaling diffuse Plane relations objects relationssimulations seen while for within in transforming ellipticals. semi-analytic the high-redshift models local compact to universe. ellipti- ing predict I the major will effective discuss and radius my minor work and mergers. torelations velocity include dispersion as Using the of a these results elliptical function of results, galaxies of high-resolution Iface follow- redshift. will brightness ’thickness’ I examine of will the the also evolutionFundamental Fundamental look of Plane Plane. at the allows correlations size-mass Looking us between at and to stellar thesurface Fundamental determine age merger brightnesses, Plane whether and histories do metallicity galaxies of so and that elliptical becausetheir the galaxies lie of mass-to-light residual throughout above ratios their sur- the the and more central Fundamental recent dark Plane,analysis mergers matter with fractions. of and relatively star By the higher comparing formation, Sloan the or Digitalelliptical results because galaxies. of Sky semi-analytic of Survey, models intrinsic with we variations a can in recent determine the efficacy of major and minor mergers in creating realistic Abstract star-formation, where stars are createdmass from infalling radii cold of gas, our simulated galaxies are all compact with projected half- 7.24 Simulating Elliptical Galaxies Throughout the Fundamental Plane We use a large sampleincrease of in cosmological re-simulations sizes of and individual weak massive decrease galaxies of to the investigate stellar the velocity origin dispersions of since the strong Abstract 7.23 Cosmological SPH Simulations: Formation and Evolution of massive Galaxies Abstract Environment and supernova feedback play importanttween roles implementations. in galaxy For formation modellers, yet environment thesimulation. can meaning be Observers of measured on these in the terms other 3D can hand spacial varyproperty, do be- coordinates such not as as have velocity given dispersion, this by is luxury then the andhow measured outputs are from well of limited a these galaxy by different to the constrain methods 2D the converge projectionsbeing third on dimension. as compared. the to It Similarly, sky. is unify supernova interesting Usually observations feedback to a is and ask Supernovae implemented simulations are in not one only many needs responsible models, for to but clearing agree different theimplementations ISM on recipes can through are what a lead used is Sedov construct blast, to actually but it. different canconstrain also star trigger these formation star effects, formation. rates we Different based present onferent results techniques the from used. same two The physical projects first event, is thatenvironment which an parameters use should in environment known use. project not solutions that The occur. second uses to is thehow compare To a the Millennium series the feedback Simulation of models accuracy to supernova work blasts of investigate on conducted the the the inthe different same different dif- different initial environments techniques conditions. to compared is Through investigated, these improving two comparison our projects understanding convergence of between models of galaxy formation. 7.22 Measuring Environment and Feedback Galaxy Formation, Durham, Poster Programme dex. 2 . 0 ≤ Ghent University Stanford University Leiden Observatory Mr Joeri Schroyen [email protected] Mr Alireza Rahmati [email protected] while having enough volume to make precise Miss Rachel Reddick [email protected] 18 − = r M 184 (after galaxy mass as the dominant parameter) in dwarf galaxy evolution. second parameter We show results based onrotating a [Schroyen large et suite al.]. of The N-Body/SPH mainstellar simulations goal metallicity of is profiles isolated, to of flat investigate dwarf dwarf possible galaxies:flat galaxies, mechanisms dwarf metallicity to both irregulars profiles, explain rotating (dIrr) while the and and rounder observed non- flat, and dichotomyshow rotating non-rotating in that dwarf dEs radial ellipticals flattening show (dE) by strong generally rotation negative posess particularly metallicity is efficient gradients. key in to These producing simulations reproducing flatable the metallicity to observed do profiles, characteristics this. while of The non-rotating flat additionthe dEs of dwarf low-level angular in star galaxies. momentum formation flattened causes and Rotation dark-matter a the “centrifugal accompanying proves haloesprevents barrier” feedback large-scale are which are oscillations not slows not centrally down in concentrated the the but infalllow occur SFR, of density galaxy-wide. gas, turning holes so This a to also that so-called be “breathing” createdtime proves in SFH to the into be gas, the a which principal more reason is“fountain for continuous observed mechanism”. the SFH, in flat We metallicity and dIrrs. therefore profiles propose causes of This our dIrrs mechanism “centrifugalOur and barrier of general flat mechanism” conclusion smearing dEs, which is instead out is that of able the rotation the to SF previously hassuggest explain suggested a in angular the significant momentum space observations. influence as and on a the evolution and appearance of dwarf galaxies, and we Abstract 7.27 Angular momentum as a second parameter in dwarf galaxy evolution Angular momentum differentiates between SF modes,does making not our seem fast possible without rotating rotation. models qualitatively resemble dIrrs, which While cosmological dark matter simulationswith have the consistently dark improved matter over in time, orderdance to it matching make remains to comparisons necessary dark with to matter observation.subhalo relate halos To abundance galaxies in examine matching this the (SHAM) relationship, Bolshoi for we simulation. objects have dimmer applied The than abun- Bolshoi simulation has sufficient resolution to allow DR7 Galaxies Abstract 7.26 Subhalo Abundance Matching in the Bolshoi Simulation Tested Against SDSS statements about their statistical properties.two-point correlation We function, the apply conditional several luminosityare different function then and SHAM compared the prescriptions, against conditional stellar and the mass same measureand function. measures the the drawn These projected conditional results from luminosity the SDSS functionvelocity DR7 found before galaxy in accretion catalog. the and SHAM SDSS using reproduces a when the fixed performing clustering scatter abundance in matching luminosity. with the This peak scatter is circular constrained to be nonzero and Abstract We study different properties ofredshift the zero. neutral Our method and is ionized basedsimulations, gas on using post in TRAPHIC, processing a in the zoomed order snapshots at to simulationof different investigate which redshifts neutral the with is gas effect a inside of similar set the different to of galaxy. physical full the processes radiative Milky which transfer change Way the at distribution shaping neutral gas structures in Milky-Way-like galaxies 7.25 The interplay between background and local ionizing radiation sources in Galaxy Formation, Durham, Poster Programme and are initially ⊙ M Durham University Universität Potsdam 13 University of Toronto 10 − 10 10 × 3 [email protected] Mr Dan Taranu Dr Martin Stringer [email protected] [email protected] Dr Thorsten Tepper García 185 100 groups spanning a range of masses from ∼ composed of 3 to 50 spiralTully-Fisher galaxies. relation. The These input simulations galaxies are are designed selecteding to from known test an scaling observed whether relations luminosity hierarchical can function multipleof and produce mergers the scaled of elliptical largest by spiral remnants samples the galaxies on of obey- the galaxyone group observed dimensional simulations profile fundamental to fitting plane. techniques, date. as The Thephotometric well simulations resulting as and galaxies are two kinematic are dimensional one analysed fits observations using using ofsatellites. GALFIT a and the variety The GALMORPH. of resulting groups, We traditional morphologies, create using kinematics mock GALFITcal and galaxies. scaling to relations fit We are focus the compared on profiles toare the published of systematic best analyses effects the fit of from Sersic central local seeing, index ellipti- galaxy signal-to-noise and and and bulge fitting nearby fractions method. in addition to the fundamental plane. Also discussed Abstract Using high-resolution, hydrodynamical simulationsLyman-Alpha of Absorbers structure (BLA). formation In (OWLS),conditions particular, of we we the gas analyse investigate and the the the structuressome mechanisms nature where predictions responsible they about of arise. for what Broad We should their compare be our widths, expected results from and to data observations the obtained where physical with possible, and e.g. make COS. 7.30 What are Broad Lyman-Alpha Absorbers? Abstract We present a large samplenants. of collisionless The simulations simulations of consist galaxy group of mergers designed to produce elliptical galaxy rem- 7.29 The Fundamental Plane of Galaxy Group Mergers Abstract Twenty years have passed sinceishing the advances first numerical in simulations computational of facilities.keeping supernova faith feedback Yet with in our the galaxies, analytic results years treatment ofply marked of is these by indeed this simple aston- simple pioneering process – experiments. seems underpinnedTo to by Is face robust this have this energy conviction lingered, question, conservation because apparently we arguments the have –tempting net or run to effect are controlled understanding on we simulations the gas turning of to physical sup- disknumerical outdated reason galaxies, technique. conclusions? for exploring However, the the by dependence differing extrapolation on beyond results.to resolution, the support highest and This a achievable at- modified exercise resolution, version reveals it of is aaccuracy the possible traditional of lack to treatment both of use of analytic convergence these supernovae models feedback. results in and the This resolution-limited can simulations. be used to improve the physical the wrong reasons? 7.28 Numerical and analytic treatment of supernova feedback: The right answer for Galaxy Formation, Durham, Poster Programme α % at 1 ∼ (Barnes, 3 LAEs. It is ∼ 7 . CEA - Saclay z 5 ∼ z % or better for scales 1 MPA/Leiden Observatory Dr Edoardo Tescari [email protected] photons. For this purpose, a Monte Carlo Ly α Mr Marcel van Daalen [email protected] Center for Astronomy and Astrophysics, Yale University emission, are becoming an important probe of galaxy forma- α 186 Dr Zheng Zheng [email protected] . We have employed the large suite of simulations from the OWLS project to inves- 1 − emission and the circumgalactic and intergalactic environments induced by the reso- α Mpc h 10 halos around star-forming galaxies, including LAEs and LBGs. The study leads to a completely ≤ α k photons. Such an environment-dependent radiative transfer effect alone is able to explain an array ≤ α 1 . already. It will thus be necessary to improve our understanding of feedback processes in galaxy formation, 0 1 − Mpc h 3 . = 0 Lyman Alpha Emitters (LAEs), galaxies selected by their Ly Abstract Galaxy Clustering corresponding to tigate the effects of various baryonicprocesses processes are on capable the of changing matter the powerk power spectrum. spectrum In by this up talk, toor I several at will tens least show of to that constrain per them single cent, through baryonic and auxiliary can observations, before even we change can it fulfil by the goals of upcoming weak lensing surveys. 7.33 Radiative Transfer Modeling of Lyman Alpha Emitters and New Effects in tion, cosmic reionization, and cosmology.into full Correct consideration interpretations the of radiativeradiative the transfer growing transfer (resonant observations code scattering) of is LAEs of applied require Ly to us a to state-of-the-art take cosmological reionization simulation to study Upcoming weak lensing surveys, suchtrum as those with with unprecedented LSST, accuracy. EUCLID,set and In WFIRST, of order aim cosmological to to parameters, interpret measure can the these matter predict observations, power the theoretical spec- non-linear models are matter needed power that, spectrum given at a the level of Abstract 7.32 The effects of baryons on the matter power spectrum Haehnelt, Tescari & Viel 2011,a suite arXiv: of 1101.3319, cosmological submitted galaxyof to formation observed MNRAS). simulations properties The (run of radiative with Dampedsome transfer the Lya preliminary simulations SPH absorption results code are systems on GADGET-2) based (TescariRomain the which on et Teyssier, same reproduce al. using a topic, the wide Eulerian 2009, fromtriply range AMR MNRAS, the ionized code Carbon 397, work RAMSES. (CIV) 411). I I in high-resolution will am hydrodynamicinvestigate Then, conclude doing simulations’ the by I (Tescari properties in discussing et will of al. the Saclay CIV present paper 2011, (Paris), insimulations MNRAS, ‘Cosmic the of 411, under evolution intergalactic 826), a of the medium where LambdaCDM the using we supervision model. a of set of Prof. high-resolution and large box-size cosmological the first time that realistic radiativecoupling transfer between modeling the of observed LAEs Ly isnant performed scattering in of a Ly cosmological volume. The study reveals a Abstract I will discuss results from different worksmedium which at explore high the effect redshift. of First feedback I processesof will on the the present Lya galaxies 3D radiation and resonant the from radiative intergalactic a transfer central simulations source of in the the spatial host and galaxies spectral of diffusion high column density absorption systems at circumgalactic medium of high redshift galaxies. 7.31 The impact of different feedback processes on the Lya emission and the of observed properties of LAEs.also predicts In extended addition, Ly it gives rise to interesting new features in the clustering of LAEs. The model new framework for understanding LAEs, with important implications for using LAEs to study reionization and cosmology. 7.34 Self-Similar Secondary Infall: Trying to Understand Halo Formation Mr Phillip Zukin MIT [email protected]

Abstract

N-body simulations have revealed a wealth of information about dark matter halos, but their results are largely empirical. Using analytic means, we attempt to shed light on simulation results by generalizing the self-similar secondary infall model to include tidal torque. Imposing self-similarity allows us to analytically calculate the structure of the the halo in different radial regimes and numerically compute the profiles of the halo without being limited by resolution effects inherent to N- body codes. I will describe this simplified halo formation model and compare our results to mass and velocity profiles from recent N-body simulations. We find that angular momentum plays an important role in determining the structure of the halo at small radii.

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