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AN ALMA SURVEY of SUB-MILLIMETER GALAXIES in the EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED from ULTRAVIOLET-TO-RADIO MODELING

da Cunha, Elisabete; Walter, F.; Smail, Ian; Swinbank, A M; Simpson, J M; Decarli, Roberto; Hodge, J. A.; Weiss, A; Van der Werf, P.; Bertoldi, Frank; Chapman, Scott C.

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The ALESS survey has followed up on a sample of 122 sub-millimeter sources in the Extended Chandra Deep Field South at 870 μm with the Atacama Large Millimeter Array (ALMA), allowing us to pinpoint the positions of sub-millimeter galaxies (SMGs) to ~0.3 arcsec and to find their precise counterparts at different wavelengths. This enabled the first compilation of the multi-wavelength spectral energy distributions (SEDs) of a statistically reliable survey of SMGs. In this paper, we present a new...[Show more]

dc.contributor.authorda Cunha, Elisabete
dc.contributor.authorWalter, F.
dc.contributor.authorSmail, Ian
dc.contributor.authorSwinbank, A M
dc.contributor.authorSimpson, J M
dc.contributor.authorDecarli, Roberto
dc.contributor.authorHodge, J. A.
dc.contributor.authorWeiss, A
dc.contributor.authorVan der Werf, P.
dc.contributor.authorBertoldi, Frank
dc.contributor.authorChapman, Scott C.
dc.date.accessioned2018-11-29T22:52:28Z
dc.date.available2018-11-29T22:52:28Z
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1885/152185
dc.description.abstractThe ALESS survey has followed up on a sample of 122 sub-millimeter sources in the Extended Chandra Deep Field South at 870 μm with the Atacama Large Millimeter Array (ALMA), allowing us to pinpoint the positions of sub-millimeter galaxies (SMGs) to ~0.3 arcsec and to find their precise counterparts at different wavelengths. This enabled the first compilation of the multi-wavelength spectral energy distributions (SEDs) of a statistically reliable survey of SMGs. In this paper, we present a new calibration of the magphys SED modeling code that is optimized to fit these ultraviolet-to-radio SEDs of $z\gt 1$ star-forming galaxies using an energy balance technique to connect the emission from stellar populations, dust attenuation, and dust emission in a physically consistent way. We derive statistically and physically robust estimates of the photometric redshifts and physical parameters (such as stellar masses, dust attenuation, star formation rates (SFRs), and dust masses) for the ALESS SMGs. We find that the ALESS SMGs have median stellar mass ${M}_{*}=8.9\pm 0.1\times {10}^{10}\;{M}_{\odot }$, median SFR $=\;280\pm 70\;{M}_{\odot }\;{\mathrm{yr}}^{-1}$, median overall V-band dust attenuation ${A}_{V}=1.9\pm 0.2$ mag, median dust mass ${M}_{\mathrm{dust}}=(5.6\pm 1.0)\times {10}^{8}\;{M}_{\odot }$, and median average dust temperature ${T}_{\mathrm{dust}}\simeq 40$ K. We find that the average intrinsic SED of the ALESS SMGs resembles that of local ultra-luminous infrared galaxies in the infrared range, but the stellar emission of our average SMG is brighter and bluer, indicating lower dust attenuation, possibly because they are more extended. We explore how the average SEDs vary with different parameters (redshift, sub-millimeter flux, dust attenuation, and total infrared luminosity), and we provide a new set of SMG templates that can be used to interpret other SMG observations. To put the ALESS SMGs into context, we compare their stellar masses and SFRs with those of less actively star-forming galaxies at the same redshifts. We find that at $z\simeq 2$, about half of the SMGs lie above the star-forming main sequence (with SFRs three times larger than normal galaxies of the same stellar mass), while half are consistent with being at the high-mass end of the main sequence. At higher redshifts ($z\simeq 3.5$), the SMGs tend to have higher SFRs and stellar masses, but the fraction of SMGs that lie significantly above the main sequence decreases to less than a third.
dc.format.mimetypeapplication/pdf
dc.publisherIOP Publishing
dc.sourceThe Astrophysical Journal
dc.titleAN ALMA SURVEY of SUB-MILLIMETER GALAXIES in the EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED from ULTRAVIOLET-TO-RADIO MODELING
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume806
dc.date.issued2015
local.identifier.absfor020104 - Galactic Astronomy
local.identifier.ariespublicationa383154xPUB8677
local.type.statusPublished Version
local.contributor.affiliationda Cunha, Elisabete, College of Science, ANU
local.contributor.affiliationWalter, F., Max Planck Institut fur Astronomie
local.contributor.affiliationSmail, Ian, Durham University
local.contributor.affiliationSwinbank, A M, Durham University
local.contributor.affiliationSimpson, J M, Durham University
local.contributor.affiliationDecarli, Roberto, Max-Planck Institut fur Astronomie
local.contributor.affiliationHodge, J. A., National Radio Astronomy Observatory
local.contributor.affiliationWeiss, A, Max-Planck Institut für Radioastronomie
local.contributor.affiliationVan der Werf, P., Leiden Observatory, Leiden University
local.contributor.affiliationBertoldi, Frank, Argelander Institute for Astronomy
local.contributor.affiliationChapman, Scott C., Dalhousie University
local.bibliographicCitation.issue1
local.identifier.doi10.1088/0004-637X/806/1/110
dc.date.updated2018-11-29T07:46:16Z
local.identifier.scopusID2-s2.0-84934987010
local.identifier.thomsonID000356810300110
dcterms.accessRightsOpen Access
CollectionsANU Research Publications

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