THE GOULD's BELT DISTANCE SURVEY Revista Mexicana De Astronomía Y Astrofísica, Vol

Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México

Loinard, L.; Mioduszewski, A. J.; Torres, R. M.; Dzib, S.; Rodríguez, L. F.; Boden, A. F. THE GOULD'S BELT DISTANCE SURVEY Revista Mexicana de Astronomía y Astrofísica, vol. 40, 2011, pp. 205-210 Instituto de Astronomía Distrito Federal, México

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Torres-Peimbert e Words: Key observations. usd fteSlrsse,btte r icl to difficult are they objects but to system, distances Solar gauging the of of outside way direct only the ob- with predictions results. our theoretical servational limit compare and study, to of under ability age) objects or stellar mass young luminosity, the the derived as the (such on parameters uncertainties large larger Such even imply star-formation. even uncertaintieserrors active to of distances large sites the nearest affecting fairly the 50%) the to 20 (typically been has formation itneSurvey Distance nenlsrcueadknmtc.W ilte reydsrb ag rjc (cal project large a describe briefly then will to started We m have the and kinematics. to Because distance etc.) and percent. the Orion, structure few constrained Ophiuchus, a internal already (Taurus, detectabl than have star-formation emission observations better of radio VLBI to compact regions how Sun with show the trigonometr associated will the of often we measure pc are to 500 stars sufficient young within is active, object This any micro-arcseconds. of 50 motions posi order the of provide accuracy can observations an (VLBI) Interferometry Baseline Long obser Very usando Solar, vecindad la en formación estelar la de detallada vista una proveer nen.Leo eciieo nga ryco(llamado forma proyecto de gran estructura regiones un su revelar describiremos las a Luego, a empezado han distancia y interna. Orión, la etc.) Ofiuco, (Tauro, restringido estudiadas han frecuentemente ya ser Por VLBI movimi técnicas porcientos. cómo micro usando VL observaciones los unos detectable trigonométrica precisión que 50 y emisión compacta una mejor emiten radio paralaje de con jóvenes menudo Sol la estrellas a orden del medir precisión (VLBI pc del 500 para una base hasta suficiente localizado con de l´ınea es compactas Esto larga radiofuentes muy arco. posición de la interferometr´ıa de proveer la pueden utilizan que Observaciones eMxA(ei eConferencias) de (Serie RevMexAA ainlAtooad ´xc,Ad.Psa -2 58090, 3-72, Postal ([email protected]). Michoacán, Mexico Morelia, México, Apdo. Autónoma de Nacional neOeain etr 03Lpzil od oor,NM Socorro, Road, Lopezville USA. 87801, 1003 Center, Operations ence u e ¨gl7,511Bn,Germany. Bonn, 53121 Hügel 71, dem Auf ttt fTcnlg,10 aionaBv. aaeaCA Pasadena Blvd., California USA. E 91125, 1200 Technology, of stitute 1 2 3 4 rgnmti aalxmaueet provide measurements parallax Trigonometric star- of study the in obstacle recurrent An etod aiatooáyAto´sc,Universidad Astrof´ısica, y Radioastronom´ıa de Centro ainlRdoAtooyOsraoy oeiiSci- Domenici Observatory, Astronomy Radio National readrIsiu ¨rAtooi,Uiesta Bonn, Universität Astronomie, für Argelander-Institut iiino hsc,Mt,adAtooy aionaIn- California Astronomy, and Math, Physics, of Division .Loinard, L. srmty—rdainmcaim:nnteml—rdocnium stars continuum: radio interferometric — techniques: non–thermal — mechanisms: radiation — astrometry .INTRODUCTION 1. eindt rvd ealdve fsa-omto nteSlrneighborho Solar the in star-formation of view detailed a provide to designed ) 1 .J Mioduszewski, J. A. H OL’ ETDSAC SURVEY DISTANCE BELT GOULD’S THE , 40 0–1 (2011) 205–210 , 2 .M Torres, M. R. ABSTRACT RESUMEN 3 .Dzib, S. atee ntenaetsa-omn ein (at regions star-forming com- nearest very the radii remain in stellar therefore even few and a pact stars, only con- the extending normally around regions is instru- emission to This VLBI fined with 1985). (Dulk detectable pro- mag- ments stars emission strong young radio the low-mass duce in surrounding gy- fields electrons The netic relativistic active. of low-mass magnetically ration often because are regions, stars star-forming young all in exist fsffiin rgtes( brightness sufficient of ol eur srmti bevtosacrt to case accurate 40 this observations about in a astrometric 2% obtain require To to would par- accurate (mas). trigonometric measurement milli-arcseconds the 2 parallax ob- instance, only an for is For pc, allax 500 neighborhood. at Solar ject the in even obtain n ehiu htcnraiypoieastrometric provide 50 readily order observ- of can an accuracies that is 2001) technique Swenson ing & Moran, accuracy. of Thompson, level a such reach not did Perryman 1997) Hipparcos; al. as et (such astrometry to icated h ol’ etDsac Survey Distance Belt Gould’s The eyLn aeieItreoer VB;e.g. (VLBI; Interferometry Baseline Long Very 1 .F Rodr´ıguez, F. L. µ s vnepniesaemsin ded- missions space expensive Even as. ino opc ai ore with sources radio compact of tion no rpo ecaqirobjeto cualquier de propios entos sn LItcnqe.Here techniques. VLBI using e µ rvd nomto ntheir on information provide s o opc ai sources radio compact for as, magnéticamente las activas, T 1 io sea ecnsmás cercanas ción estelar b tr:pemi sequence pre-main stars: — o u ilse inglés) en siglas sus por n .F Boden F. A. and s fe tde nearby studied often ost ≈ ainsVLBI. vaciones I Aqu´ı, mostraremos BI. cprla n proper and parallax ic hyaemagnetically are they led 10 7 h ol’ Belt Gould’s The ) uhsources Such K). diseñado para ) ucinemática su y duigVLBI using od sgno de -segundos 4 205 © 2011: Instituto de Astronomía, UNAM - XIII Latin American Regional IAU Meeting Ed. W. J. Henney & S. Torres-Peimbert n ics oepnigissues. pending some results, discuss these In summarize and concentrated. will we is sections, Sun coming the the of the parsecs hundred Belt, few within Gould’s a star-formation most to where and belong structure ring-like regions Serpens, These Perseus, re- Orion). star-forming Taurus, nearby (Ophiuchus, prominent most gions five the mas. in 10 about only entire is the figure that the the Note of towards case. size oriented specific – com- this the source in the and south-east, the is component of trajectory parallax motion elliptic That proper an details). of et for bination Loinard characterized 2007 (see as observations Tauri compan- al. southern T VLBI the multi-epoch object of famous by one of the Sb, plane of Tau the ions T on by described sky show trajectory the we the example, 1 an Figure multi- As in using observations. stars VLBI young epoch nearby several to distance variable. strongly often and rare use are limited they mass of are because intermediate masers and where low regions with star-forming here results primar- concerned few be ily a will we mention observations, maser will from low- we obtained Although active an stars. magnetically offer mass to and alternative common, detectable are interesting also instruments) are VLBI (which with masers methanol and ter rdce ytebs ta h wleeoh seLiade l 07f 2007 al. multi-e d et prop by Loinard and (see measured parallax epochs as twelve of sky the combination ellip at a the as fit with shown of best fit are plane the and best by 2005, the the July predicted shows on to curve 2003 Sb dotted September Tau from The T epochs 12 of at Trajectory collected 1. Fig. 206 ea 6 c(hn 91.Mr eety however, recently, More 1981). (Chini pc 165 at be ≈ h on tr osdrds a r l located all are far so considered stars young The the measured have we years, five last the Over uigmn er,Ohuhswstogtto thought was Ophiuchus years, many During 0 c.I ihms trfrigrgos wa- regions, star-forming mass high In pc). 100 2.1 .RESULTS 2. Ophiuchus . ONR TAL. ET LOINARD eGu ta.(99 on enphotometric mean a found (1989) 125 of al. distance et example, For Geus preferred. de been have distances shorter h picu oe(1adDA2) n on a found and 120 of DoAr21), value and in mean (S1 stars core two Ophiuchus of the parallax trigonometric core. the Ophiuchus measured the for pc 120 a about Using reported of also distance (2008) a Ophiuchus. al. of et in Lombardi distance method, component the similar pc dust to 120 main corresponds at this the jump Hipparcos that extinction their agued clear of and direc- a function the found a in distances, as stars Ophiuchus of of reddening Hög (1998), tion the & examined Knude who Ophiuchus. with associated hudb sue ob 120 be to assumed core (2008), Ophiuchus be the al. should to distance et the Loinard that to conclude by pc and reported 2 To errors quadratically order. formal add that we the of effect, be that to for expected account are core depth Ophiuchus its the to the in due on region objects errors the individual systematic of to so depth a similar, distance The be to to pc. corresponding expected 2 is across, about of degrees radius 2 linear about only is ntne obrie l 20)fudsm indica- some For found several case. (2008) are the al. There be et Lombardi indeed sky). instance, might the this of that plane indications physical the their pc, on 10 at extent about be (within therefore associated distances should the physically similar and from be core, pc Ophiuchus to the 10 thought with about are to They extend core. and 1709, 1729) 1689, Lynds or as 1712, correspond (such streamers clouds The dust prominent 2008). to al. the et as Wikling known (see structures filamentary eral sn LIosrain,Liade l (2008) al. et Loinard observations, VLBI Using nadto oiscr,Ohuhscnan sev- contains Ophiuchus core, its to addition In rdetails). or rmto.Tesursaetepositions the are squares The motion. er e hs ie ersn h ro bars. error the represent sizes whose ses ± . 5p o h tla population stellar the for pc 25 ohosrain.Tedt were data The observations. poch 0 ± 4 . c h picu core Ophiuchus The pc. 5 ± pc. 5 streamers © 2011: Instituto de Astronomía, UNAM - XIII Latin American Regional IAU Meeting Ed. W. J. Henney & S. Torres-Peimbert itneo 178 a of determine they distance 16293–2422, masers IRAS water with of observations associated of VLBI stel- streamer on eastern (2007) young Based the very L1689. in 16293–2422 the al. IRAS system of et lar parallax Imai trigonometric by the determination the from twudceryb eyipratt bana in- L1689. an to obtain distance the to of important farther. confirmation very pc dependent be of clearly tens east- several would the be It with would associated L1689 region cloud the ern while be pc, would 120 streamers, associated at north-eastern region, and core One the with Ophiuchus. toward two line sight the least along of (2007) at coexist that Thus, regions al. indicate star-forming et deep. unrelated would pc Imai it 60 of confirmed, of be determination were plane to distance the unlikely the on very if across is pc it sky, 10 the about only is complex n fsa-omto seKno ta.20 for 2008 al. et Kenyon (see star-formation understand- of our ing of development the to instrumental iayyugselrojc ao11c oae in located 111 (2008) the 1–14c, of to streamer, Haro north-eastern modeling) al. object the orbit stellar et on young Schaefer (based binary nearer Similarly, distance pc a 10 to found core. 5 the be might t than streamers of location the The that (2001). tions al. et Dame from indicated. line are CO(1-0) the motions in proper Taurus their of Image 2. Fig. oehtpzln euti htrsetcomes respect that in result puzzling somewhat A arsi ehp h einta a enmost been has that region the perhaps is Taurus − +18 37 c ic h nieOphiuchus entire the Since pc. 2.2 Taurus . H OL’ ETDSAC UVY207 SURVEY DISTANCE BELT GOULD’S THE − +19 18 pc. on ob tasmlrdsac (132 distance similar a are at stars three be prominent all to Interestingly, the found same with L1495. the cloud associated toward and dark Taurus, located 283572, are of HDE 2) portion Figure 4, – (Hubble Tau stars V773 complex. these Taurus of the reported five Three across have of distributed we parallax stars 2011), trigonometric young 2009, the of 2007, measurements al. et Torres pc 25 about side. be far might its filament that than conceivable each closer quite of is side it near sight, the of those line perpendic- Since the orientated to be thick. ularly to degrees reason no filaments 2 have parallel filaments about speak- the three each Roughly of of 2) pc). plane (Figure composed 25 the is (or Taurus on degrees ing, 10 region about the and is 1994), of been sky al. extent long et (Kenyon total has pc distance the 140 about mean be Its to known review). recent a 128 oto fTuu.Tedseso bu htmean that about dispersion specific that The to Taurus. distance of the of portion estimate the pro- good clearly of a pc) vides mean (131.4 weighted measurements distance The spatio- three coherent a structure. to belong kinematical by to 2), appear measured (Figure therefore velocities as and radial kinematics and motions same proper the their share to pear . nasre fppr Liade l 05 2007; 2005, al. et (Loinard papers of series a In 5 ± 0 . c n 132 and pc, 6 efiesasi h ope,and complex, the in stars five he . 9 ± 2 . c.Te loap- also They pc). 4 . 8 ± 0 . pc, 5 © 2011: Instituto de Astronomía, UNAM - XIII Latin American Regional IAU Meeting Ed. W. J. Henney & S. Torres-Peimbert eune o u nesadn fstar-formation. con- of important understanding have our would for This sequences associ- Taurus. population the with stellar ated and the re- of structure to kinematics three-dimensional potential internal the the both have would veal complex across distributed entire stars young the of tens several for here edge. eastern that edge the from near western different stars the significantly the are of near complex 2009). stars the of of velocity al. space et The center-Galactic (Ballesteros-Paredes Galactic axis the anticenter along be would almost Taurus oriented in In filaments side. the eastern side configuration, the western that to the corresponding pc), edge (25–30 with far wide the associated and is edge it near clearly as the deep Taurus as with about made. be to be appears can conclusions pre- few liminary a but Taurus, the of regarding structure conclusions three-dimensional definite reach to needed be line-of- the along resolving complex clearly Taurus are the sight. we of Thus, depth farthest the sample. and nearest our separa- the in the between stars than pc) smaller 30 times (a (about 10 measurements tion about distance are (Fig- our pc) on L1495 few errors with The motions associated 2). stars proper ure the Their different of significantly those but from 2009). another, one to similar al. are et Torres 2007; hl PTui t161 at is Tau HP while o G 33 n a bandfo nanalysis later, an Somewhat from measurements. obtained was previous was distance several Her- and of this following as 1333, Specifically, pc, Perseus NGC 350 to (1983). for be Jones distance to & the assumed big time, was 2008; long whole a a al. For et ac- Walawender particularly instance tive. is 348; star-formation (for where IC 2008) Herbst sub-regions and important 1333 NGC of number a Fgr ) ar a on ob t146 at be to found was Tauri complex T Taurus 2). the to (Figure of respectively, Sb north-east Tauri located, and are south-east T the They are Tau/G3. measured HP been and have parallaxes ric wide. is it as deep to as the appears about region; L1495 that be with for associated pc population 2.5 to stellar about corresponds of This radius physical across. a degrees 2 popu- complex. about stellar Taurus is good associated the lation of its of provide and depth L1495 must local Interestingly, hand, the other of the estimate on pc), (2.4 208 lal,osrain iia otoedescribed those to similar observations Clearly, will measurements distance accurate Additional h esu lu Blye l 08 contains 2008) al. et (Bally cloud Perseus The h te w tr o hc LItrigonomet- VLBI which for stars two other The 2.3 Perseus . . 9 ± 0 . c(onr tal. et (Loinard pc 9 . 7 ± ONR TAL. ET LOINARD 0 . pc, 6 rn deo h lu a t255 at was the cloud that the concluded area of and an edge degrees, covering front square stars 50 more about their many of extended include (2003) to al. work et Straizys recently, More e C5i h epn oergo.Te obtain They region. 414 core of sys- Serpens distance binary a the the in of EC95 parallax tem trigonometric the sured be- association physical two. a of the that suggests tween and Rift coworkers, Aquila Serpens and the Straizys the by to found pc. distance 200 cloud the about of between et distance a similarity Prato at The 1985; be to Thaddeus believed 2008) called & al. clouds (Dame Rift molecular Aquila of located the is complex Serpens larger projection, a In toward pc. 80 about depth ntels 5yasi htrpre ySriy tal. et Straizys photometry: by stellar reported on that based 2010 is (1996) years authors al. 15 most et last by Dzib used the and distance in 2008 The pc al. discussion). et a 250 Eiroa for from (see controversy ranging pc some 650 estimates to of with matter years, a the sky.over been the star-formation has of of plane distance the region Its on important degrees several an for extending is 2008) al. complete region. a important that enable of eastern would structure the the 348) of of IC description and and B1) (B5 part with portions central the (associated determina- in Perseus VLBI stars young of to at Sun. distance located the the of be from tion to pc western assumed 230–235 the be sources about can that two Perseus 1.5 the indicates of about that distances portion result is similar Their 2011) at (2008, are pc. 6 al. The or con- et degrees, sources Hirota complex. two by Perseus the sidered the between of separation 1448 edge projected L western cloud the dark the at with associated source stellar V 3i G 33 n 232 and 1333, NGC in 13 SVS hyoti itneo 235 of distance using masers. a water Perseus obtain associated They in their objects of observations stellar VLBI young two to tance to (corresponding across entire degrees pc). the 6 25–30 could because about there spread is are, distance region they significant phys- if a are even be sub-regions and not different is associated, it the ically Indeed, if pc. clear to 350 entirely and continued 300 have between distance however, values measure- use shorter authors, extinction Many on a based for pc) ments. argued (220 1333 (1990) NGC to al. et Cernis sn LIosrain,Di ta.(00 mea- (2010) al. et Dzib observations, VLBI Using h epn oeua lu ope Eraet (Eiroa complex cloud molecular Serpens The ioae l 20,21)hv esrdtedis- the measured have 2011) (2008, al. et Hirota . 9 ± 2.4 4 . c infiatylre than larger significantly pc, 4 Serpens . ± ± 8p o h source the for pc 18 8p o young a for pc 18 ± d 5p,adits and pc, 55 259 = ± 7pc. 37 © 2011: Instituto de Astronomía, UNAM - XIII Latin American Regional IAU Meeting Ed. W. J. Henney & S. Torres-Peimbert 21)adcaiyterlto ewe epn and Serpens Rift. al. between Aquila et relation the Dzib the of clarify Serpens measurement and of (2010) distance direction the the confirm in to It stars mea- other parallax plane. VLBI of Galactic obtain surements sight to the important of of very This direction be line will the that sight. in since of roughly unexpected is line not same certainly but the is associated, along physically located be Ser- merely not Aquila of would and those clouds Serpens the than Rift interpretation, rather that In Rift the Aquila pens. with associated the natu- be in might would clouds which along 2003) contribution sight, dust of (1996, first line method the the to the al. sensitive that be et is rally Straizys conclusion by Their Dzib used (2010). in given al. is di- parallax et obtained trigonometric that a and from years, 15 rectly last the in used Serpens distance for popular most the between discrepancy enpbihd ioae l 20)otie dis- a obtained (2007) 437 al. of tance et Hirota years, have published. five measurements been last parallax the VLBI In al. several (1981). et however, Muench al. pc et 480 by was Genzel given distance following accepted is the decades, Orion For history to 2008). the distance (an of the region account of Nebula entertaining largely Orion and have the interesting Orion on to concentrated distance been ef- the The measure star-formation. to of forts region studied often most l 20)fud389 et found Sandstrom (2007) whereas region, al. BN/KL the in masers easmdt e415 can be distance to that and assumed limited, be very core be Serpens to the expected to is distance depth the of of contribution uncertainty the the to consequence, a As sky. the ndaee.Tedsac otecoda whole a 415 as 25 be cloud or to the taken across, to be degrees therefore distance 3 should The about is diameter. hand in other the on netn fol bu 5 with about cloud, only Serpens of the extent of Serpens sub-region an The dense a Serpens. is for core adopted usually value the yMne ta.(07 n i ta.(08 who (2008) measure- al. (414 consistent et ments Kim highly and settled obtained (2007) was independently issue al. The et Menten star. by flaring a of observations ieetdsacs nadto,teeaeanumber a are at there certainly addition, most In so are across, distances. complex different pc the region. 100 of Nebula about parts Orion is different complex the cloud for Orion only The are far so quoted ealdaayi ftepsil esn o the for reasons possible the of analysis detailed A oehrwt ars ro sudutdythe undoubtedly is Orion Taurus, with Together tsol oe,hwvr httedistances the that however, noted, should It ± ± 9p sn LIosrain fwater of observations VLBI using pc 19 cad418 and pc 7 2.5 ± ± 3p rmVB continuum VLBI from pc 23 Orion . c h epn cloud, Serpens The pc. 5 ′ ± 06p)o h ln of plane the on pc) (0.6 c respectively). pc, 6 H OL’ ETDSAC UVY209 SURVEY DISTANCE BELT GOULD’S THE ± 5pc. 25 eetprso h ro n urudn lusap- necessary. clouds dif- be surrounding to the and pears to Orion the pro- distance of the VLBI parts ferent establishing comprehensive at the a aimed than Thus, gram closer significantly of Nebula. some be Orion that might indications themselves clouds some clouds are these Orion There complex, the unclear. Orion to is the relation of whose vicinity the but al. et in Reipurth L1622; located and 2008) L1617 (e.g. clouds dark of fta osblt,w aeiiitdalreproject large a initiated have advantage(the we Taking possibility, that stars. feasible of young become hundred will several here for presented observations those upgrade, fac- that to a to similar by Thanks several. sensitivity) of its its tor therefore increase will (and which bandwidth upgrade, currently is major VLBA) a - undergoing Array Baseline Long Very (the three-dimensional regions. the these of of indications structure provided direct of have first regions they the nearest different cases, several the our dozen In to refined star-formation. a distance significantly the about of already knowledge only have but of objects, total a targeted h te ad ilsati h al21 n last and 2011 years. fall 4 about the of in total on start a observations, will for VLBA hand, sum- The other the year. the until that continue of will started mer/fall and have observations time 2011, observations February astrometric VLBA EVLA in the of The hours to 2000 themselves. dedicated first about be that of Following will total (EVLA) a Array targets. stage, Large adequate observing Very identify of Expanded hours to the 120 about on use time will stage project first the The of Orion). and Serpens Perseus, Taurus, costefiergosdsrbdin described regions distributed five stars the young 200 across about to distance the ing enlknmtc ftefiergosdsrbdin described regions five the in- of and kinematics structure ternal three-dimensional distance, mean vey ore nnab ein fsa-omto aebeen have star-formation of regions nearby in sources very the Belt. on particu- light Gould’s In new of Way. shed origin Milky will observations the our of understanding lar, structure our local for the the and of for star-formation, both of consequences study important have will This .TEGUDSBL ITNESURVEY DISTANCE BELT GOULD’S THE 3. n ftewrdspeirVB instruments VLBI premier world’s the of One have far so described observations VLBI The h nlga fthe of goal final The ut-pc LIatoer fyugstellar young of astrometry VLBI Multi-epoch st siaewt nrcdne cuaythe accuracy unprecedented with estimate to is ol’ etDsac Survey Distance Belt Gould’s .CONCLUSIONS 4. ol’ etDsac Sur- Distance Belt Gould’s ie tmeasur- at aimed ) § (Ophiuchus, 2 § 2. © 2011: Instituto de Astronomía, UNAM - XIII Latin American Regional IAU Meeting Ed. 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Astronomy version of to dio digital map grateful a CO(1-0) are us grated We sending for 61/3-1. Dame VL grant Re- search Noether Emmy Forschungs- the through Deutsche R.F.H. (DFG) gemeinschaft the and by V.H.T., and support R.M.T., acknowledges UNAM DGAPA, of Mexico. acknowl- support CONACyT, L.F.R. financial and the S.D., edge L.L., Foundation. heim Ser- of regions Perseus, Orion. and nearby Taurus, pens, prominent Ophiuchus, most star-formation: five dis- distributed the accurate stars young across 200 providing about to by estimates tance knowledge Survey that Distance called prove Belt project com- VLBA the Gould’s on-going star- In large The of a years, neighborhood. kinematics few Solar ing and the distribution in formation space These knowledge the our unprece- percent. of improved an few already a with have than observations distance better their accuracy dented measure to used 210 o.I d .Riut SnFacso S) 372 ASP), Francisco: (San Reipurth B. ed. 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