Alma imaging and gravitational lens models of south pole telescope—selected dusty, star-forming galaxies at high redshifts
- Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States)
- Núcleo de Astronomía, Facultad de Ingeniería, Universidad Diego Portales, Av. Ejército 441, Santiago (Chile)
- European Southern Observatory, Karl Schwarzschild Straße 2, D-85748 Garching (Germany)
- Cavendish Laboratory, University of Cambridge, JJ Thompson Avenue, Cambridge CB3 0HA (United Kingdom)
- Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States)
- Dalhousie University, Halifax, Nova Scotia (Canada)
- Department of Physics, University of California, One Shields Avenue, Davis, CA 95616 (United States)
- Department of Astronomy, University of Florida, Gainesville, FL 32611 (United States)
- Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT (United Kingdom)
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305 (United States)
- Department of Physics and Astronomy, University of California, Los Angeles, CA 90095-1547 (United States)
- Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69 D-53121 Bonn (Germany)
The South Pole Telescope has discovered 100 gravitationally lensed, high-redshift, dusty, star-forming galaxies (DSFGs). We present 0.″5 resolution 870 μm 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 (μ{sub 870μm}>2), with a median magnification of μ{sub 870μm}=6.3, extending to μ{sub 870μm}>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{sub FIR} ratio and Σ{sub FIR} found for low-redshift star-forming galaxies applies to high-redshift galaxies and extends at least two orders of magnitude higher in Σ{sub FIR}. 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.”.
- OSTI ID:
- 22868863
- Journal Information:
- Astrophysical Journal, Vol. 826, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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