ALMA Frontier Fields Survey. V.J/A+A/633/A160ivo://CDS.VizieR/J/A+A/633/A160doi:10.26093/cds/vizier.36330160CDSCarvajal R.Bauer F.E.Bouwens R.J.Oesch P.A.Gonzalez-Lopez J.,Anguita T.Aravena M.Demarco R.Guaita L.Infante L.Kim S.,Kneissl R.Koekemoer A.M.Messias H.Treister E.Villard E.Zitrin A.,Troncoso P.2020-04-28T07:40:47Z2020-01-28T07:56:51ZCDS support teamCDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, Francecds-question@unistra.frradio-galaxiesinterferometryradio-continuum-emissionThe Hubble Frontier Fields offer an exceptionally deep window into the high-redshift universe, covering a substantially larger area than the Hubble Ultra-Deep field at low magnification and probing 1-2mags deeper in exceptional high-magnification regions. This unique parameter space, coupled with the exceptional multi-wavelength ancillary data, can facilitate for useful insights into distant galaxy populations. We aim to leverage Atacama Large Millimetre Array (ALMA) band 6 (~263GHz) mosaics in the central portions of five Frontier Fields to characterize the infrared (IR) properties of 1582 ultraviolet (UV)-selected Lyman-Break Galaxies (LBGs) at redshifts of z~2-8. We investigated individual and stacked fluxes and IR excess (IRX) values of the LBG sample as functions of stellar mass (M_star), redshift, UV luminosity and slope {beta}, and lensing magnification. LBG samples were derived from color-selection and photometric redshift estimation with Hubble Space Telescope photometry. Spectral energy distributions (SED)-templates were fit to obtain luminosities, stellar masses, and star formation rates for the LBG candidates. We obtained individual IR flux and IRX estimates, as well as stacked averages, using both ALMA images and u-v visibilities. Two (2) LBG candidates were individually detected above a significance of 4.1-sigma, while stacked samples of the remaining LBG candidates yielded no significant detections. We investigated our detections and upper limits in the context of the IRX-M_star and IRX-{beta} relations, probing at least one dex lower in stellar mass than past studies have done. Our upper limits exclude substantial portions of parameter space and they are sufficiently deep in a handful of cases to create mild tension with the typically assumed attenuation and consensus relations. We observe a clear and smooth trend between M* and {beta}, which extends to low masses and blue (low) {beta} values, consistent with expectations from previous works.2020A&A...633A.160Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/633/A160CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/633/A160https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/633/A160http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/633/A160https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/633/A160https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/633/A160http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/633/A160GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/633/A160/tablec1 (HST photometry)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/633/A160/tablec1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/633/A160/tablec1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/633/A160/tablec1?GETtext/xml+votable180.050000true3.598375-30.41480.005555555555555556Cone search capability for table J/A+A/633/A160/tablec2 (ALMA properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/633/A160/tablec2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/633/A160/tablec2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/633/A160/tablec2?GETtext/xml+votable180.050000true3.5983333-30.414750.0055555555555555566/16486 17741 28448 34793 46474 464961.0590977079788917e-19 1.3189343879298211e-18https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/633/A160?format=asciiRadiodefault
J/A+A/633/A160/tablec2ALMA propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSource IDmeta.id;meta.mainintRAJ2000ALMA Right ascension (J2000) (1)pos.eq.ra;meta.mainDEJ2000ALMA Declination (J2000)pos.eq.dec;meta.mainClusterCandidate home clustermeta.id.parentcharFpeakALMA peak 1mm flux (pb-corrected)uJyphot.flux.density;em.mm.200-400GHzintrmspeakALMA peak 1mm rms (pb-corrected) (2)uJystat.stdev;instr.det.noiseintB_FpeakUpper 3-sigma limit in FpeakuJyphot.flux.density;em.mm.200-400GHz;stat.maxintS/NPeak 1mm signal to noise ratiostat.snrfloatpbcorPeak primary beam correction factorarith.factorfloat
J/A+A/633/A160/tablec3UV-slope, magnification and distancerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSource IDmeta.id;meta.mainintbetaUV-slopespect.indexfloatb_betaLower 1-sigma (68%) limit in betameta.notefloatB_betaUpper 1-sigma (68%) limit in betameta.notefloatmagnifMagnification factor (1)phot.flux;arith.ratiodoubleb_magnifLower 1-sigma (68%) limit in magnif (2)meta.notefloatB_magnifUpper 1-sigma (68%) limit in magnif (2)meta.notedoublee_magnifMagnification factor standard deviation (3)stat.errorfloatDlLuminosity distance (4)Mpcpos.distanceintb_DlLower 1-sigma (68%) limit in DlMpcpos.distance;stat.minintB_DlUpper 1-sigma (68%) limit in DlMpcpos.distance;stat.maxint
J/A+A/633/A160/tablec4Properties from FAST++ and graybodyrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSource IDmeta.id;meta.mainintlog(M*)Log of stellar mass (1)log(solMass)phys.massfloatb_log(M*)Lower 1-sigma (68%) limit in log(M*) (1)log(solMass)phys.mass;stat.minfloatB_log(M*)Upper 1-sigma (68%) limit in log(M*) (1)log(solMass)phys.mass;stat.maxfloatlog(SFR)Log of star formation rate (1)log(solMass.yr**-1)phys.SFRfloatb_log(SFR)Lower 1-sigma (68%) limit in log(SFR) (1)log(solMass.yr**-1)phys.SFR;stat.minfloatB_log(SFR)Upper 1-sigma (68%) limit in log(SFR) (1)log(solMass.yr**-1)phys.SFR;stat.maxfloatlog(sSFR)Log of specific star formation ratelog(yr**-1)phys.SFRfloatb_log(sSFR)Lower 1-sigma (68%) limit in log(sSFR)log(yr**-1)phys.SFR;stat.minfloatB_log(sSFR)Upper 1-sigma (68%) limit in log(sSFR)log(yr**-1)phys.SFR;stat.maxfloat
J/A+A/633/A160/tablec5HST photometry and graybody luminositiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSource IDmeta.id;meta.mainintlog(LUV)Log of ultraviolet luminositylog(solLum)phys.luminosity;em.UVfloatb_log(LUV)Lower 1-sigma (68%) limit in log(LUV)log(solLum)phys.luminosity;em.UV;stat.minfloatB_log(LUV)Upper 1-sigma (68%) limit in log(LUV)log(solLum)phys.luminosity;em.UV;stat.maxfloatB_log(LIR)? Upper 3-sigma limit in log of infrared luminositylog(solLum)phys.luminosity;em.IR;stat.maxfloatnullableB_log(LIR/LUV)? Upper 3-sigma limit in log of LIR/LUVmeta.notefloatnullablelog(FUV)Log of ultraviolet flux densitylog(uJy)phot.flux.density;em.UVfloatb_log(FUV)Upper 1-sigma (68%) limit in log(FUV)log(uJy)arith.zp;stat.maxfloatB_log(FUV)Lower 1-sigma (68%) limit in log(FUV)log(uJy)arith.zp;stat.minfloatB_log(FIR)? Upper 3-sigma limit in log of infrared fluxlog(uJy)phot.flux.density;em.IR;stat.maxfloatnullable