The Galaxy Origins and Young Assembly (goya) survey is designed to
study the formation and evolution of 1 < z < 3 galaxies with the aim of learning on
the epoch and the mechanisms by which galaxies assembled the bulk of their stars
and acquired their present structure and dynamics. In 1998 goya proposed, and
has since been guiding, the construction of the most ambitious of the common-user
instruments for GranTeCan —the emir near-infrared multi-object spectrograph. In
preparation for the exploitation of emir, we have conducted a deep near-infrared
photometric survey, for sample selection and characterisation. Now that this research
has reached its final stages, we provide here details on its current status
and its finalisation plans. Overall, this survey has images of 0.5 square degrees of
high-latitude sky to limiting ab magnitude Ks = 23.7 (5-¾, 100 aperture) and corresponding
depths at U,B, V,R, I and J. The sample of sources obtained is being
extended to include fields available to Gemini-S, since a recent collaboration with
the Flamingos-2 Early Science Survey Team grants goya privileged access to this
pioneering near-infrared multi-object spectrograph.Peer ReviewedPostprint (published version

Abreu Rodríguez, David

Balcells, Marc

Barro, Guillermo

Cristóbal Hornillos, David

Domínguez, Lilian

Eliche Morral, Maria del Carmen

Gallego Maestro, Jesús

López, C.

Prieto Muñoz, Mercedes

Vallbé Mumbrú, Marc

Villar, Vïctor

English

UPCommons. Portal del coneixement obert de la UPC

Completion of the GOYA Photometric SurveyM. Vallbe´ i Mumbru´1, M. Balcells1, D. Abreu1, G. Barro2, D. Cristo´bal3,L. Domı´nguez1, C. Eliche1, J. Gallego2, C. Lo´pez1, M. Prieto1, V. Villar21 Instituto de Astrof´ısica de Canarias, E-38205 La Laguna, Tenerife, SpainMarc.Vallbe@iac.es2 Universidad Complutense de Madrid, Madrid, Spain3 Instituto de Astrof´ısica de Andaluc´ıa, Granada, SpainSummary. The Galaxy Origins and Young Assembly (goya) survey is designed tostudy the formation and evolution of 1 < z < 3 galaxies with the aim of learning onthe epoch and the mechanisms by which galaxies assembled the bulk of their starsand acquired their present structure and dynamics. In 1998 goya proposed, andhas since been guiding, the construction of the most ambitious of the common-userinstruments for GranTeCan —the emir near-infrared multi-object spectrograph. Inpreparation for the exploitation of emir, we have conducted a deep near-infraredphotometric survey, for sample selection and characterisation. Now that this re-search has reached its final stages, we provide here details on its current statusand its finalisation plans. Overall, this survey has images of 0.5 square degrees ofhigh-latitude sky to limiting ab magnitude Ks = 23.7 (5-σ, 1′′ aperture) and cor-responding depths at U,B, V,R, I and J . The sample of sources obtained is beingextended to include fields available to Gemini-S, since a recent collaboration withthe Flamingos-2 Early Science Survey Team grants goya privileged access to thispioneering near-infrared multi-object spectrograph.1 IntroductionThe search for the origins of the massive spiral and elliptical galaxies thatpopulate the Universe today, and the understanding of the physical processesthat drove their formation and evolution, will be a central theme in observa-tional cosmology for the next decade. The evolution with redshift of quantitiessuch as the dynamical mass, the stellar content of galaxies, the metallicity,the star formation rate density, and the super-massive black-hole accretionrates in the 1 < z < 3 range will be prime drivers of progress. This comesas the natural continuation of the observations undertaken in the last decadewith hst and 8-m class telescopes, which have shown that high-z galaxieswere sensibly different to the present-day ones: they were smaller ([13]), lessmassive ([5]), of bluer colours ([8]), and formed stars at much superior rates2 Vallbe´ i Mumbru´ et goya teamFig. 1. Close-up images of the same field on goods-n. The image on the left is anear-infrared Ks-band picture obtained with liris on the wht, while the image onthe right was taken with the hst under blue light.([11]). However pioneering studies in the infrared domain have unveiled thatthe statistics obtained from optical samples, which map the uv spectrumof galaxies, are biased towards galaxies with high star-formation rates butwith low masses ([9, 4, 1]). Hence, given the importance of massive galaxiesas discriminants amongst different hierarchical structure-formation scenarios,mapping the rest-frame optical spectrum, which cosmological expansion shiftsto the nir, is the prime driver of the next generation of near-infrared, multi-object spectrographs on 10m-class telescopes.With the Gran Telescopio Canarias (gtc), Spain has ensured a privilegedaccess to first-class observational means in the optical and infrared astronomi-cal ranges. In 1998 goya, led by four main nodes at iac, ucm, laomp (Europe)and ufl (usa), proposed to Grantecan the commissioning of a multi-objectspectrograph for the near-infrared range (0.9-2.5 microns), that has becomeknown as emir. The instrument was then unique in its class, and today it keepsbeing so in many regards. Amongst the most relevant features we single out arobotic reconfigurable cryogenic multi-slit mask acting as field selector, and aset of dispersive elements formed by the combination of high quality diffrac-tion grating and conventional prisms which allow resolutions of R > 4000 inZJHK (see [10] for further details). That the goya scientific aims drove thedesign of emir guarantees an immediate scientific production right at the on-set of the spectrograph’s operations. This return is granted by employing halfof the emir Guaranteed Time during the initial years of emir operations.In recent months, goya has established a close collaboration with theFlamingos-2 Early Science Survey team of the University of Florida and willbenefit from a minimum of 7 nights of guaranteed time during 2007-08 withFlamingos-2. This is a fully cryogenic, 1 to 2.5 micron multi-object spectrom-eter and wide field imager for the Gemini-S, to start commissioning in 2007([6]). Apart from boosting the international promotion and visibility of theGOYA Photometric Survey 3Table 1. Extent of the goya Photometric Survey. Note that the limit-ing magnitude is the Ks band measured in the AB photometric systemat S/N=3 and a fwhm=1′′. Also that the area is given in squared arc-minutes. The fields targeted for the “deep” slice are the Groth Strip(175 arcsec2), Groth O2k (750 arcsec2), goods-n (250 arcsec2; see Fig-ure 1), and SA-68 (150 arcsec2)Survey Bands Limiting Magnitude AreaUltra Deep (WHT / Groth-Westfall) UBVIJK 23.7 20Deep (WHT) UBVRIJK 22.7 1300Shallow (CAHA / Groth Flanking Fields) (J),K ∼21.7 1000gtc community, the Flamingos time will be highly valuable for it will allowto accelerate the generation of results for goya and polish the observationalstrategies for a more efficient exploitation of emir. Also, with ∼ 500 nir spec-tra of galaxies, we will be able to produce the first results as a proto-studyfor the complete goya Spectroscopic Survey to undertake with emir.2 GOYA Photometric Survey: 2000-2007All in all, goya has over 40 nights of guaranteed time with the top nirmos spectrographs. In preparation for a fruitful scientific exploitation, thegoya Photometric Survey was undertaken to create a database of sourceswith near-infrared and optical photometry, photometric redshifts, and as muchinformation as possible collected at other wavelengths, which could then beobserved and characterised with emir and Flamingos-2.Most of the effort of the Photometric Survey has been devoted to conducta deep infrared imaging program (bands J,K) with correspondingly deepoptical data. Undertaken by the goya nodes at iac and ucm, it has usedsubstantial allocations of observational resources at the ORM and Calar Alto.Due to bad weather throughout, the original plans to cover 1 square degreewere downsized by a factor of two. We organised thet survey area into “ultradeep”, “deep” and “shallow” levels of sensibility, roughly at decreasing stepsof 1 magnitude starting at Ks(AB) ' 22.7 for the “ultra deep” slice (seeTable 1 for details). As of today, the data-acquisition campaign is at a stageof being 80% complete, while the data reduction is completed at the 70%level. In terms of data-reduction we are currently reducing wht and cahainfrared data.We are committed to publishing standardised photometric database cat-alogs of sources for public access. We are working in a timeline where abeta version of the photometric survey catalogs including all observed datain fields Groth-Westfall, Groth Strip, Groth Flanking Fields, goods-n, plusdatamined info on cdfs and virmos-2h, will be available by Jan 2007. This4 Vallbe´ i Mumbru´ et goya teamFig. 2. The goya Photometric Survey has become a valuable scientific tool. Spawn-ing from K < 21.4 and correspondingly deep UBV IJK photometry over 175 sq.arc-min. on the Groth strip, several studies on early-type galaxy formation have beenpursued: SED-based stellar mass estimates ([2]); B− and K−band population syn-thesis evolutionary models (Prieto et al 2006); bulge/disk relationships (Dominguezet al. in prep.); galaxy fusion rate vs. z; extremely red objects; K-band luminosityfunction; photo-z distributions (depicted in picture); census of mergers; obscuredX-ray agn ([12]); etc.catalogs will be debugged in the following months and an alpha version forinternal use is planned for Jul 2007. Keeping on schedule, a public release ofthe data should follow as early as Jan 2008.The goya photometric catalog combines data taken by our team withother data available in public databases, as well as through collaborations. Theevolving calendars for the completion of GTC and the start of the goya spec-troscopic survey with emirmean that we can now take advantage of public nirsurveys carried out with efficient, wide-field imagers such as ukirt/wfcamand cfht/wircam, for securing large datasets of nir photometry of galaxies.Among those are space platforms of special interest for high-z galaxy studies,such as galex, and Spitzer. The goods and swire surveys provide rest-frameK-band luminosities for galaxies at z up to ∼3, giving us ideal informationfor the selection of galaxy samples that avoid biases in star formation activity(see Perez-Gonza´lez’s talk in these proceedings).3 Pre-EMIR scienceWe are exploiting the goya Photometric Survey in a wide range of scientificprojects. We have obtained galaxy number counts in the nir ([3]), and in bluebands ([7]). Using number count models that simultaneously fit blue and nircounts we obtained constraints on the epoch of formation of galaxies in the redsequence (Prieto et al. 2006, these proceedings). We have obtained estimatesGOYA Photometric Survey 5Fig. 3. The goya Data Flow specifies routines and algorithms for all the proceduresinvolved in the acquisition of data, including data reduction pipelines, which are thenstored in the Archive.of the stellar mass in galaxies through SED-fitting methods ([2]). Currentlyongoing projects include: the determination of the K-band luminosity func-tion of galaxies and its evolution to z = 1.5; photometric and morphologicalcharacterisation of the sample of merger galaxies in the Groth and goods-n fields; evolution of the rate of mergers to z = 1.5; analysis of the ages ofgalactic bulges to z 0.8, in Groth and goods-n (Science with the GTC IIIProceedings, in prep.).4 GOYA Data SystemIn order to manage the large amount of data produced in the survey, we haveestablished the goya Data System (gds), a prescription for a comprehensiveorganisation of information in the goya project (Figure 3). The gds specifieswhat information is stored and how, specifies data formats, and provides forways to access the data. Information consists of: the products of the goyaData Flow; data gathered from external sources; the documentation generatedin the project; and, the software packages developed for the project. Thesecomponents are organised into the goya Archive, which provides the rela-tional functionality that fulfils the scientific needs of the project. User accessinterfaces to the archive include web interfaces as well as direct and ftp access.The development of the gds has been guided by the principles of: Stan-dardisation, Integration, Modularity, Maintainability, Accessibility, Deploya-bility. This shall make it easy to adapt to other surveys, and we will be happyto share this work with any interested parties. As Virtual Observatory (vo)standards become more unified, the gds has the commitment to follow them.6 Vallbe´ i Mumbru´ et goya team5 SummaryThe goya team has acknowledged the importance of measuring the dynamicand stellar mass, the star-formation rate, the abundances of heavy elementsand the super-massive black-hole accretion rates in distant galaxies as thefour main functions which will tell us how galaxies form and evolve. For thesestudies it has gathered over 40 nights of guaranteed time on two of the world’smost advanced nir spectrographs, emir on gtc (2008-10) and Flamingos-2on Gemini-S (2007-08), and it is estimated that 104 near-infrared spectra willbe obtained. In preparation for the exploitation of emir, the goya team hasconducted a deep nir photometric survey, for sample selection and character-isation, which covers over 0.5 deg2 at typical magnitudes of Ks < 22.5 (AB).This survey is proving good for 0.5 < z < 2 science and several lines of re-search have stemmed from it. Recently our source catalogs are being expandedto include sources available to Flamingos-2 and Spitzer infrared data.We anticipate to release a working version of our catalogs for internal usearound 2007 summer. A public release is planned for 2008, in the frame of thegoya Archive. More information on the project can be obtained by contactingthe authors or at http://www.iac.es/project/GOYAiac/GOYAiac.html.References1. A. Cimatti et al. The K20 survey. I. A&A, 381:L68–L72, Jan. 2002.2. D. Cristo´bal. PhD thesis, Instituto de Astrof´ısica de Canarias, 2005.3. D. Cristo´bal, M. Prieto, M. Balcell, R. Guzma´n, N. Cardiel, A´. Serrano, J. Gal-lego, and R. Pello´. K[s] number counts in the Groth and Coppi fields. In J. M.Rodriguez Espinoza, F. Garzon Lopez, and V. Melo Martin, editors, RevistaMexicana de Astronomia y Astrofisica Conference Series, pages 267–268, 2003.4. M. Dickinson et al. In Bulletin of the American Astronomical Society, pages1367–+, Dec. 1998.5. M. Dickinson et al. ApJ, 587:25–40, Apr. 2003.6. S. Eikenberry et al. FLAMINGOS-2. In Proceedings of the SPIE, Volume 6269,pp. (2006)., July 2006.7. M. C. Eliche-Moral, M. Balcells, M. Prieto, C. E. Garc´ıa-Dabo´, P. Erwin, andD. Cristo´bal-Hornillos. GOYA Survey: U and B Number Counts in the Groth-Westphal Strip. ApJ, 639:644–671, Mar. 2006.8. R. S. Ellis. Faint Blue Galaxies. ARA&A, 35:389–443, 1997.9. R. Elston, G. H. Rieke, and M. J. Rieke. ApJ, 331:L77–L80, Aug. 1988.10. F. Garzo´n, D. Abreu, S. Barrera, S. Becerril, L. M. Cairo´s, J. J. Dı´az, A. B.Fragoso, F. Gago, R. Grange, C. Gonza´lez, P. Lo´pez, J. Patro´n, J. Pe´rez, J. L.Rasilla, P. Redondo, R. Restrepo, P. Saavedra, V. Sa´nchez, F. Tenegi, andM. Vallbe´. EMIR: the GTC NIR multi-object imager-spectrograph. In Pro-ceedings of the SPIE, Volume 6269, pp. (2006)., July 2006.11. P. Madau et al. MNRAS, 283:1388–1404, Dec. 1996.12. T. Miyaji et al. Multiwavelength Properties of the X-Ray Sources in the Groth-Westphal Strip Field. AJ, 127:3180–3191, June 2004.13. I. Trujillo et al. ApJ, 604:521–533, Apr. 2004.

Completion of the GOYA photometric survey

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Completion of the GOYA photometric survey

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