J/ApJ/765/9ivo://CDS.VizieR/J/ApJ/765/9doi:10.26093/cds/vizier.17650009CDSda Cunha E.Walter F.Decarli R.Bertoldi F.Carilli C.Daddi E.,Elbaz D.Ivison R.Maiolino R.Riechers D.Rix H.-W.Sargent M.,Smail I.Weiss A.2017-06-01T08:49:43Z2014-11-21T12:35:12ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frradio-galaxiesmillimeter-astronomysubmillimeter-astronomyredshiftedastronomical-modelsModern (sub-)millimeter/radio interferometers such as ALMA, JVLA, and the PdBI successor NOEMA will enable us to measure the dust and molecular gas emission from galaxies that have luminosities lower than the Milky Way, out to high redshifts and with unprecedented spatial resolution and sensitivity. This will provide new constraints on the star formation properties and gas reservoir in galaxies throughout cosmic times through dedicated deep field campaigns targeting the CO/[C II] lines and dust continuum emission in the (sub-)millimeter regime. In this paper, we present empirical predictions for such line and continuum deep fields. We base these predictions on the deepest available optical/near-infrared Advanced Camera for Surveys and NICMOS data on the Hubble Ultra Deep Field (over an area of about 12arcmin^2^). Using a physically motivated spectral energy distribution model, we fit the observed optical/near-infrared emission of 13099 galaxies with redshifts up to z=5, and obtain median-likelihood estimates of their stellar mass, star formation rate, dust attenuation, and dust luminosity. We combine the attenuated stellar spectra with a library of infrared emission models spanning a wide range of dust temperatures to derive statistical constraints on the dust emission in the infrared and (sub-)millimeter which are consistent with the observed optical/near-infrared emission in terms of energy balance. This allows us to estimate, for each galaxy, the (sub-)millimeter continuum flux densities in several ALMA, PdBI/NOEMA, and JVLA bands. As a consistency check, we verify that the 850{mu}m number counts and extragalactic background light derived using our predictions are consistent with previous observations. Using empirical relations between the observed CO/[C II] line luminosities and the infrared luminosity of star-forming galaxies, we infer the luminosity of the CO(1-0) and [C II] lines from the estimated infrared luminosity of each galaxy in our sample.2013ApJ...765....9Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/765/9CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toVI/139 : Herschel Observation Log (Herschel Science Centre, 2013)VIII/95 : Herschel Multi-tiered Extragalactic Survey (Oliver+, 2012)III/250 : The VIMOS VLT deep survey (VVDS-DEEP) (Le Fevre+ 2005)J/A+A/533/A119 : GOODS-Herschel North and South catalogs (Elbaz+, 2011)J/ApJ/707/1201 : LABOCA ECDFS Submillimeter Survey (LESS) (Weiss+, 2009)J/ApJ/682/985 : FIREWORKS photometry of GOODS CDF-S (Wuyts+, 2008)J/MNRAS/384/1611 : Submm observations in gravitational lenses (Knudsen+, 2008)J/ApJS/178/280 : Compendium of ISO far-IR extragalactic data (Brauher+, 2008)J/ApJS/172/70 : zCOSMOS-bright catalog (Lilly+, 2007)J/MNRAS/372/1621 : SCUBA Half-Degree Extragalactic Survey. II (Coppin+, 2006)J/MNRAS/370/1057 : Blank-field SCUBA surveys (Scott+ 2006)J/AJ/132/926 : Galaxies in the Hubble Ultra Deep Field (Coe+, 2006)J/MNRAS/358/149 : HDFN SCUBA Super-map. III (Pope+, 2005)J/MNRAS/344/887 : Sub-mm observations of the HDF (Serjeant+, 2003)J/ApJ/592/728 : Lyman break galaxies at redshift z~3 (Steidel+, 2003)J/ApJ/586/794 : Multiwavelength luminosities of galaxies (Bell, 2003)J/ApJ/554/803 : New VLA Sky Survey cat. of IRAS 2Jy Galaxies (Yun+ 2001)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/765/9https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/765/9http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/765/9https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/765/9https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/765/9http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/765/9GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/765/9/fluxes (Predicted continuum fluxes, and CO, [CII] line fluxes)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/765/9/fluxes?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/765/9/fluxes?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/765/9/fluxes?GETtext/xml+votable180.050000true53.1655-27.82848060.0055555555555555566/359352.5179064367170437e-23 1.2593110519984029e-21https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/765/9?format=asciiOpticalRadiodefaultJ/ApJ/765/9/fluxesPredicted continuum fluxes, and CO, [CII] line fluxes[CBS2006][1/60319] Coe et al. 2006(J/AJ/132/926) numbermeta.id;meta.mainintprimaryRAJ2000[3] Hour of Right Ascension (J2000)pos.eq.ra;meta.mainDEJ2000[27] Degree of Declination (J2000)pos.eq.dec;meta.mainzph[0.01/5] Photometric redshiftsrc.redshiftfloatlogF38Log of 38GHz flux density (1)log(Jy)phot.flux.density;em.mm.30-50GHzfloatE_logF38Upper limit uncertainty on logF38log(Jy)stat.error;stat.maxfloate_logF38Lower limit uncertainty on logF38log(Jy)stat.errorfloatlogF80Log of 80GHz flux density (1)log(Jy)phot.flux.density;em.mm.50-100GHzfloatE_logF80Upper limit uncertainty on logF80log(Jy)stat.error;stat.maxfloate_logF80Lower limit uncertainty on logF80log(Jy)stat.errorfloatlogF100Log of 100GHz flux density (1)log(Jy)phot.flux.density;em.mm.50-100GHzfloatE_logF100Upper limit uncertainty on logF100log(Jy)stat.error;stat.maxfloate_logF100Lower limit uncertainty on logF100log(Jy)stat.errorfloatlogF144Log of 144GHz flux density (1)log(Jy)phot.flux.density;em.mm.100-200GHzfloatE_logF144Upper limit uncertainty on logF144log(Jy)stat.error;stat.maxfloate_logF144Lower limit uncertainty on logF144log(Jy)stat.errorfloatlogF230Log of 230GHz flux density (1)log(Jy)phot.flux.density;em.mm.200-400GHzfloatE_logF230Upper limit uncertainty on logF230log(Jy)stat.error;stat.maxfloate_logF230Lower limit uncertainty on logF230log(Jy)stat.errorfloatlogF345Log of 345GHz flux density (1)log(Jy)phot.flux.density;em.mm.200-400GHzfloatE_logF345Upper limit uncertainty on logF345log(Jy)stat.error;stat.maxfloate_logF345Lower limit uncertainty on logF345log(Jy)stat.errorfloatlogF430Log of 430GHz flux density (1)log(Jy)phot.flux.density;em.mm.400-750GHzfloatE_logF430Upper limit uncertainty on logF430log(Jy)stat.error;stat.maxfloate_logF430Lower limit uncertainty on logF430log(Jy)stat.errorfloatlogF660Log of 660GHz flux density (1)log(Jy)phot.flux.density;em.mm.400-750GHzfloatE_logF660Upper limit uncertainty on logF660log(Jy)stat.error;stat.maxfloate_logF660Lower limit uncertainty on logF660log(Jy)stat.errorfloatlogF870Log of 870GHz flux density (1)log(Jy)phot.flux.density;em.mm.400-750GHzfloatE_logF870Upper limit uncertainty on logF870log(Jy)stat.error;stat.maxfloate_logF870Lower limit uncertainty on logF870log(Jy)stat.errorfloatlog(1-0)CO(1-0) flux density (115.27GHz)log(Jy)phot.flux;meta.modelleddoublelog(2-1)0CO(2-1) flux density (230.54GHz), MW model (2)log(Jy)phot.flux;meta.modelleddoublelog(2-1)1CO(2-1) flux density (230.54GHz), M82 model (2)log(Jy)phot.flux;meta.modelleddoublelog(3-2)0CO(3-2) flux density (345.80GHz), MW model (2)log(Jy)phot.flux;meta.modelleddoublelog(3-2)1CO(3-2) flux density (345.80GHz), M82 model (2)log(Jy)phot.flux;meta.modelleddoublelog(4-3)0CO(4-3) flux density (461.04GHz), MW model (2)log(Jy)phot.flux;meta.modelleddoublelog(4-3)1CO(4-3) flux density (461.04GHz), M82 model (2)log(Jy)phot.flux;meta.modelleddoublelog(5-4)0CO(5-4) flux density (576.27GHz), MW model (2)log(Jy)phot.flux;meta.modelleddoublelog(5-4)1CO(5-4) flux density (576.27GHz), M82 model (2)log(Jy)phot.flux;meta.modelleddoublelog(6-5)0CO(6-5) flux density (691.47GHz), MW model (2)log(Jy)phot.flux;meta.modelleddoublelog(6-5)1CO(6-5) flux density (691.47GHz), M82 model (2)log(Jy)phot.flux;meta.modelleddoublelog(7-6)0CO(7-6) flux density (806.65GHz), MW model (2)log(Jy)phot.flux;meta.modelleddoublelog(7-6)1CO(7-6) flux density (806.65GHz), M82 model (2)log(Jy)phot.flux;meta.modelleddoublelog[CII]Model flux density of [CII] line (1900.54GHz)log(Jy)phot.flux;meta.modelleddoubleNEDSimbad column added by the CDSmeta.ref.urlchar