J/A+A/602/A96ivo://CDS.VizieR/J/A+A/602/A96doi:10.26093/cds/vizier.36020096CDSSchreiber C.Elbaz D.Pannella M.Merlin E.Castellano M.Fontana A.,Bourne N.Boutsia K.Cullen F.Dunlop J.Ferguson H.C.,Michalowski M.J.Okumura K.Santini P.Shu X.W.Wang T.White C.2017-07-17T11:39:08Z2017-06-21T08:26:27ZCDS support team

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

cds-question@unistra.frgalaxiesphotometryastronomical-modelsThis paper introduces egg, the Empirical Galaxy Generator, a tool designed within the ASTRODEEP collaboration to generate mock galaxy catalogs for deep fields with realistic fluxes and simple morphologies. The simulation procedure is based exclusively on empirical prescriptions - rather than first principles - to provide the most accurate match with current observations at 0<z<7. We considered that galaxies can be either quiescent or star-forming, and used their stellar mass (M*) and redshift (z) as the fundamental properties from which all the other observables can be statistically derived. Drawing z and M* from the observed galaxy stellar mass functions, a star-formation rate (SFR) is attributed to each galaxy from the tight SFR-M* main sequence, while dust attenuation, optical colors and simple disk plus bulge morphologies are obtained from empirical relations that we established from the high quality Hubble and Herschel observations from the CANDELS fields. Random scatter was introduced in each step to reproduce the observed distributions of each parameter. Based on these observables, an adequate panchromatic spectral energy distribution (SED) is selected for each galaxy and synthetic photometry is produced by integrating the redshifted SED in common broad-band filters. Finally, the mock galaxies are placed on the sky at random positions with a fixed angular two-point correlation function to implement basic clustering. The resulting flux catalogs reproduce accurately the observed number counts in all broad bands from the ultraviolet up to the sub-millimeter, and can be directly fed to image simulators such as SkyMaker. The images can then be used to test source extraction softwares and image-based techniques such as stacking. egg is open-source, and is made available to the community on behalf of the ASTRODEEP collaboration, together with a set of pre-generated catalogs and images.2017A&A...602A..96Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/602/A96CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/602/A96https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/602/A96http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/602/A96https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/602/A96https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/602/A96http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/602/A96GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/602/A96/tablec1The number countsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFluxCenter of flux bin (for differential counts) or flux lower limit (for cumulative counts)uJyphot.fluxdoubledUDifferential counts for the VIMOS U banddeg**-2phot.count;arith.diffdoublecUCumulative counts for the VIMOS U banddeg**-2phot.count;arith.diffdoubledBDifferential counts for the Hubble F435W banddeg**-2phot.count;arith.diffdoublecBCumulative counts for the Hubble F435W banddeg**-2phot.count;arith.diffdoubledVDifferential counts for the Hubble F606W banddeg**-2phot.count;arith.diffdoublecVCumulative counts for the Hubble F606W banddeg**-2phot.count;arith.diffdoubledIDifferential counts for the Hubble F775W banddeg**-2phot.count;arith.diffdoublecICumulative counts for the Hubble F775W banddeg**-2phot.count;arith.diffdoubledZDifferential counts for the Hubble F850LP banddeg**-2phot.count;arith.diffdoublecZCumulative counts for the Hubble F850LP banddeg**-2phot.count;arith.diffdoubledYDifferential counts for the Hubble F105W banddeg**-2phot.count;arith.diffdoublecYCumulative counts for the Hubble F105W banddeg**-2phot.count;arith.diffdoubledJDifferential counts for the Hubble F125W banddeg**-2phot.count;arith.diffdoublecJCumulative counts for the Hubble F125W banddeg**-2phot.count;arith.diffdoubledHDifferential counts for the Hubble F160W banddeg**-2phot.count;arith.diffdoublecHCumulative counts for the Hubble F160W banddeg**-2phot.count;arith.diffdoubledKsDifferential counts for the HAWK-I Ks banddeg**-2phot.count;arith.diffdoublecKsCumulative counts for the HAWK-I Ks banddeg**-2phot.count;arith.diffdoubled3p6Differential counts for the Spitzer 3.6um banddeg**-2phot.count;arith.diffdoublec3p6Cumulative counts for the Spitzer 3.6um banddeg**-2phot.count;arith.diffdoubled4p5Differential counts for the Spitzer 4.5um banddeg**-2phot.count;arith.diffdoublec4p5Cumulative counts for the Spitzer 4.5um banddeg**-2phot.count;arith.diffdoubled5p8Differential counts for the Spitzer 5.8um banddeg**-2phot.count;arith.diffdoublec5p8Cumulative counts for the Spitzer 5.8um banddeg**-2phot.count;arith.diffdoubled8p0Differential counts for the Spitzer 8um banddeg**-2phot.count;arith.diffdoublec8p0Cumulative counts for the Spitzer 8um banddeg**-2phot.count;arith.diffdoubled16Differential counts for the Spitzer 16um banddeg**-2phot.count;arith.diffdoublec16Cumulative counts for the Spitzer 16um banddeg**-2phot.count;arith.diffdoubled24Differential counts for the Spitzer 24um banddeg**-2phot.count;arith.diffdoublec24Cumulative counts for the Spitzer 24um banddeg**-2phot.count;arith.diffdoubled70Differential counts for the Herschel 70um banddeg**-2phot.count;arith.diffdoublec70Cumulative counts for the Herschel 70um banddeg**-2phot.count;arith.diffdoubled100Differential counts for the Herschel 100um banddeg**-2phot.count;arith.diffdoublec100Cumulative counts for the Herschel 100um banddeg**-2phot.count;arith.diffdoubled160Differential counts for the Herschel 160um banddeg**-2phot.count;arith.diffdoublec160Cumulative counts for the Herschel 160um banddeg**-2phot.count;arith.diffdoubled250Differential counts for the Herschel 250um banddeg**-2phot.count;arith.diffdoublec250Cumulative counts for the Herschel 250um banddeg**-2phot.count;arith.diffdoubled350Differential counts for the Herschel 350um banddeg**-2phot.count;arith.diffdoublec350Cumulative counts for the Herschel 350um banddeg**-2phot.count;arith.diffdoubled500Differential counts for the Herschel 500um banddeg**-2phot.count;arith.diffdoublec500Cumulative counts for the Herschel 500um banddeg**-2phot.count;arith.diffdoubled870Differential counts for the ALMA 870um banddeg**-2phot.count;arith.diffdoublec870Cumulative counts for the ALMA 870um banddeg**-2phot.count;arith.diffdoubled1200Differential counts for the ALMA 1.2mm banddeg**-2phot.count;arith.diffdoublec1200Cumulative counts for the ALMA 1.2mm banddeg**-2phot.count;arith.diffdoubled2000Differential counts for the ALMA 2mm banddeg**-2phot.count;arith.diffdoublec2000Cumulative counts for the ALMA 2mm banddeg**-2phot.count;arith.diffdouble