ALMA IMAGING AND GRAVITATIONAL LENS MODELS OF SOUTH POLE TELESCOPE—SELECTED DUSTY, STAR-FORMING GALAXIES AT HIGH REDSHIFTS
AuthorSpilker, J. S.
Marrone, Daniel P.
Bothwell, M. S.
Carlstrom, J. E.
Chapman, S. C.
Crawford, T. M.
de Breuck, C.
Fassnacht, C. D.
Gonzalez, Anthony H.
Greve, T. R.
Rotermund, K. M.
Strandet, M. L.
Vieira, J. D.
AffiliationUniv Arizona, Steward Observ
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationALMA IMAGING AND GRAVITATIONAL LENS MODELS OF SOUTH POLE TELESCOPE—SELECTED DUSTY, STAR-FORMING GALAXIES AT HIGH REDSHIFTS 2016, 826 (2):112 The Astrophysical Journal
JournalThe Astrophysical Journal
Rights© 2016. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractThe South Pole Telescope has discovered 100 gravitationally lensed, high-redshift, dusty, star-forming galaxies (DSFGs). We present 0."5 resolution 870 mu m. Atacama Large Millimeter/submillimeter Array imaging of a sample of 47 DSFGs spanning z = 1.9-5.7, and construct gravitational lens models of these sources. Our visibility-based lens modeling incorporates several sources of residual interferometric calibration uncertainty, allowing us to properly account for noise in the observations. At least 70% of the sources are strongly lensed by foreground galaxies (mu(870) (mu m) > 2), with a median magnification of mu(870) (mu m) = 6.3, extending to mu(870) (mu m) > 30. We compare the intrinsic size distribution of the strongly lensed sources to a similar number of unlensed DSFGs and find no significant differences in spite of a bias between the magnification and intrinsic source size. This may indicate that the true size distribution of DSFGs is relatively narrow. We use the source sizes to constrain the wavelength at which the dust optical depth is unity and find this wavelength to be correlated with the dust temperature. This correlation leads to discrepancies in dust mass estimates of a factor of two compared to estimates using a single value for this wavelength. We investigate the relationship between the [C II] line and the far-infrared luminosity and find that the same correlation between the [C II]/L-FIR. ratio and Sigma(FIR). found for low-redshift star-forming galaxies applies to high-redshift galaxies and extends at least two orders of magnitude higher in SFIR. This lends further credence to the claim that the compactness of the IR-emitting region is the controlling parameter in establishing the "[C II] deficit."
VersionFinal published version
SponsorsU.S. National Science Foundation from the NRAO [AST-1312950, SOSPA2-012]; FONDECYT ; US National Science Foundation ; National Science Foundation [PLR-1248097, PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation; ; ; [085. A-0608]; [086.A-0797]; [088.A0902]; [090.A-0503]; [092.A-0480]; [284.A-5029]; [285.A-5034]; [GS-2013B-Q-5]; [GS-2013A-Q-33]