J/ApJ/850/83ivo://CDS.VizieR/J/ApJ/850/83doi:10.26093/cds/vizier.18500083CDSFujimoto S.Ouchi M.Shibuya T.Nagai H.2018-08-24T07:53:51Z2018-07-23T08:38:13ZCDS support team

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

cds-question@unistra.frmillimeter-astronomysubmillimeter-astronomyinfrared-photometryredshiftedWe present the large statistics of the galaxy effective radius Re in the rest-frame far-infrared (FIR) wavelength R_e(FIR)_ obtained from 1627 Atacama Large Millimeter/submillimeter Array (ALMA) 1mm band maps that become public by 2017 July. Our ALMA sample consists of 1034 sources with the star formation rate ~100-1000M_{sun}_/yr and the stellar mass ~10^10^-10^11.5^M_{sun}_ at z=0-6. We homogeneously derive R_e(FIR)_ and FIR luminosity LFIR of our ALMA sources via the uv-visibility method with the exponential disk model, carefully evaluating selection and measurement incompletenesses by realistic Monte-Carlo simulations. We find that there is a positive correlation between R_e(FIR)_ and LFIR at the >99% significance level. The best-fit power-law function, R_e(FIR)_{propto}L_FIR_^{alpha}^, provides {alpha}=0.28+/-0.07, and shows that R_e(FIR)_ at a fixed LFIR decreases toward high redshifts. The best-fit {alpha} and the redshift evolution of R_e(FIR)_ are similar to those of Re in the rest-frame UV (optical) wavelength R_e(UV)_ (R_e(Opt)_) revealed by Hubble Space Telescope (HST) studies. We identify that our ALMA sources have significant trends of R_e(FIR)_<~R_e(UV)_ and R_e(Opt)_, which suggests that the dusty starbursts take place in compact regions. Moreover, R_e(FIR)_ of our ALMA sources is comparable to R_e(Opt)_ of quiescent galaxies at z~1-3 as a function of stellar mass, supporting the evolutionary connection between these two galaxy populations. We also investigate rest- frame UV and optical morphologies of our ALMA sources with deep HST images, and find that ~30%-40% of our ALMA sources are classified as major mergers. This indicates that dusty starbursts are triggered by not only the major mergers but also the other mechanism(s).2017ApJ...850...83Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/850/83CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/284 : COSMOS Multi-Wavelength Photometry Catalog (Capak+, 2007)J/ApJ/622/772 : Redshift survey of submillimeter galaxies (Chapman+, 2005)J/A+A/434/53 : GOODS-South Field redshifts (Vanzella+, 2005)J/ApJS/176/1 : Subaru/XMM-Newton deep survey (SXDS). II. (Furusawa+, 2008)J/ApJS/179/124 : Subaru/XMM-Newton deep survey (SXDS) III. (Ueda+, 2008)J/ApJ/690/1236 : COSMOS photometric redshift catalog (Ilbert+, 2009)J/ApJS/195/10 : The CDF-S survey: 4Ms source catalogs (Xue+, 2011)J/ApJS/201/30 : The Chandra COSMOS survey. III. (Civano+, 2012)J/ApJS/203/24 : Structural param. of galaxies in CANDELS (van der Wel+, 2012)J/ApJ/769/80 : Spitzer/IRAC observations of five deep fields (Ashby+, 2013)J/A+A/556/A55 : Multi-color photom. of star-forming galaxies (Ilbert+, 2013)J/ApJ/788/125 : An ALMA survey of ECDFS submm galaxies (Simpson+, 2014)J/ApJ/806/110 : ALESS survey: SMGs in the ECDF-S data (da Cunha+, 2015)J/ApJ/801/97 : GOODS-S & UDS stellar mass cat. from CANDELS (Santini+, 2015)J/ApJS/219/15 : Morphologies of z=0-10 galaxies with HST data (Shibuya+, 2015)J/ApJS/222/1 : Faint ALMA 1.2mm sources down to ~0.02mJy (Fujimoto+, 2016)J/A+A/591/A136 : Galaxies & QSOs FIR size and surface brightness (Lutz+, 2016)J/A+A/597/A41 : ALMA Frontier Fields Survey. I. (Gonzalez-Lopez+, 2017)J/ApJ/839/58 : ALMA submm galaxies multi-wavelength data (Simpson+, 2017)http://almascience.eso.org/aq/ : ALMA science archivehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/850/83https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/850/83http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/850/83https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/850/83https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/850/83http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/850/83GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/850/83/table4 (5{sigma}-peak catalog (ALL5S))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/850/83/table4?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/850/83/table4?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/850/83/table4?GETtext/xml+votable180.050000true150.2038882.501070.0055555555555555565/6814 6/9272 16486 17677 17679 17688 17690 19682 27245 27247 27344 28448 33943 33948 33949 34793 35935 35957https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/850/83?format=asciiRadioInfrareddefaultJ/ApJ/850/83/table2ALMA mapsMID[1/1627] Map IDmeta.id;obs.fieldintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPrIDALMA project code IDmeta.id;obscharTargetTarget name in the initial ALMA observationsmeta.id;phys.atmol.initial;obscharlambda[0.8/1.4] Wavelength in the observed framemmem.wlfloatnu[221/354] Frequency in the observed frameGHzem.freqintBand[6/7] ALMA Bandmeta.code;instr.filterintMin[15/43] Minimum baseline of the antenna configurationminstr.baselineintMax[134/2270] Maximum baseline of the antenna configurationminstr.baselineintsigma[0.01/1.4] One sigma noise level measured after the CLEAN process (Section 2.2)mJy/beaminstr.det.noisefloatamaj[0.1/4.1] Major axis of the synthesized beam (weight = 'natural')arcsecphys.angSize;instr.beamfloatbmin[0.1/1.3] Minor axis of the synthesized beam (weight = 'natural')arcsecphys.angSize;instr.beamfloatBeam[0.1/2.1] Circularized beam sizearcsecphys.angSize;instr.beamfloatsSetClassification of the sub-dataset (1)meta.idcharType[1/2] map type: 1=single field; 2=mosaic (2)meta.codeintJ/ApJ/850/83/table45{sigma}-peak catalog (ALL5S)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[1/1034] Source ID of ALL5Smeta.id;meta.mainintRAJ2000Right Ascension, decimal degrees (J2000)degpos.eq.ra;meta.mainDEJ2000Declination, decimal degrees (J2000)degpos.eq.dec;meta.mainlambda[0.8/19.2] Observed wavelengthmmem.wlfloatSNpeak[5/69] Peak signal-to-noise ratiostat.snr;stat.maxfloatSpeak[0.08/10.2] Peak flux density per beam obtained from the peak pixel value before primary beam correctionmJy/beamphot.flux.density;em.mm.200-400GHzfloate_Speak[0.01/1.1]? Standard deviation of the pixel values before primary beam correction, corresponding to the uncertainty of the peak pixel valuesmJystat.errorfloatnullableSimf[0.06/30.4]? Total flux density measured by IMFIT after primary beam correctionmJyphot.flux.density;em.mm.200-400GHzfloatnullablee_Simf[0.01/1.1]? Uncertainty in Simf (1)mJystat.errorfloatnullableSuvf[0.05/35]? Total flux density measured by UVMULTIFIT after primary beam correction for ALL10SmJyphot.flux.density;em.mm.200-400GHzfloatnullablee_Suvf[0.01/425]? Uncertainty in Suvf (2)mJystat.errorfloatnullableSuvfcrr[0.05/27]? Total flux density measured by UVMULTIFIT after primary beam Monte-Carlo simulation (Section 3.3) corrections for ALL10S (2)mJyphot.flux.density;em.mm.200-400GHzfloatnullablee_Suvfcrr[0.01/483]? Uncertainty in Suvfcrr (2)mJystat.errorfloatnullableRuvf[0.04/0.9]? Effective Radius measured by UVMULTIFIT for ALL10S (2)arcsecphys.angSizefloatnullablee_Ruvf[0/133]? Uncertainty in Ruvf (2)arcsecstat.errorfloatnullableRuvfcrr[0.01/0.9]? Effective Radius measured by UVMULTIFIT after Monte-Carlo simulation correction (Section 3.3) for ALL10S (2)arcsecarith.factor;phys.angSizefloatnullablee_Ruvfcrr[0/111]? Uncertainty in Ruvfcrr (2)arcsecstat.errorfloatnullablef_uvf? Reliability of UVMULTIFIT result (0=reliable) (2)(3)meta.codeintnullableoffset[0.01/1]? Offset between centers of the ALMA source and the optical-NIR counterpart for OC5S (4)arcsecmeta.id.assoc;pos.angDistancefloatnullablezphot[0.01/10]? Photometric redshift of the optical-NIR counterpart obtained from the optical-NIR source catalog for OC5S (4)src.redshiftfloatnullableHmag[1.4/28.3]? H-band AB magnitude for OC5S (4)magphot.mag;em.IR.HfloatnullableCOSMOSDisplay COSMOS data (II/284 and Ilbert+, 2013, J/A+A/556/A55) within 0.3"meta.ref.urlintnullable