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The Atacama Large Millimeter/submillimeter Array Spectroscopic Survey in the Hubble Ultra Deep Field : co emission lines and 3 mm continuum sources.

González-López, Jorge and Decarli, Roberto and Pavesi, Riccardo and Walter, Fabian and Aravena, Manuel and Carilli, Chris and Boogaard, Leindert and Popping, Gergö and Weiss, Axel and Assef, Roberto J. and Bauer, Franz Erik and Bertoldi, Frank and Bouwens, Richard and Contini, Thierry and Cortes, Paulo C. and Cox, Pierre and da Cunha, Elisabete and Daddi, Emanuele and Díaz-Santos, Tanio and Inami, Hanae and Hodge, Jacqueline and Ivison, Rob and Le Fèvre, Olivier and Magnelli, Benjamin and Oesch, Pascal and Riechers, Dominik and Rix, Hans-Walter and Smail, Ian and Swinbank, A. M. and Somerville, Rachel S. and Uzgil, Bade and van der Werf, Paul (2019) 'The Atacama Large Millimeter/submillimeter Array Spectroscopic Survey in the Hubble Ultra Deep Field : co emission lines and 3 mm continuum sources.', Astrophysical journal., 882 (2). p. 139.

Abstract

The Atacama Large Millimeter/submillimeter Array (ALMA) SPECtroscopic Survey in the Hubble Ultra Deep Field (HUDF) is an ALMA large program that obtained a frequency scan in the 3 mm band to detect emission lines from the molecular gas in distant galaxies. Here we present our search strategy for emission lines and continuum sources in the HUDF. We compare several line search algorithms used in the literature, and critically account for the line widths of the emission line candidates when assessing significance. We identify 16 emission lines at high fidelity in our search. Comparing these sources to multiwavelength data we find that all sources have optical/ infrared counterparts. Our search also recovers candidates of lower significance that can be used statistically to derive, e.g., the CO luminosity function. We apply the same detection algorithm to obtain a sample of six 3 mm continuum sources. All of these are also detected in the 1.2 mm continuum with optical/near-infrared counterparts. We use the continuum sources to compute 3 mm number counts in the sub-millijansky regime, and find them to be higher by an order of magnitude than expected for synchrotron-dominated sources. However, the number counts are consistent with those derived at shorter wavelengths (0.85–1.3 mm) once extrapolating to 3 mm with a dust emissivity index of β = 1.5, dust temperature of 35 K, and an average redshift of z = 2.5. These results represent the best constraints to date on the faint end of the 3 mm number counts.

Item Type:Article
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Status:Peer-reviewed
Publisher Web site:https://doi.org/10.3847/1538-4357/ab3105
Publisher statement:© 2019. The American Astronomical Society. All rights reserved.
Date accepted:17 March 2019
Date deposited:08 October 2019
Date of first online publication:11 September 2019
Date first made open access:08 October 2019

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