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|Title:||The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Search for [CII] Line and Dust Emission in 6||Authors:||Aravena, M.
Oesch, P. A.
Carilli, C. L.
Bauer, F. E.
Da Cunha, E.
Ivison, R. J.
Riechers, D. A.
Swinbank, A. M.
van der Werf, P.
|Issue Date:||2016||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||833||Issue:||1||First Page:||71||Abstract:||We present a search for [C II] line and dust continuum emission from optical dropout galaxies at z > 6 using ASPECS, our Atacama Large Millimeter submillimeter Array Spectroscopic Survey in the Hubble Ultra-deep Field (UDF). Our observations, which cover the frequency range of 212-272 GHz, encompass approximately the range of 6 < z < 8 for [C II] line emission and reach a limiting luminosity of L <SUB>[C II]</SUB> ∼ (1.6-2.5) × 10<SUP>8</SUP> L <SUB>☉</SUB>. We identify 14 [C II] line emitting candidates in this redshift range with significances >4.5σ, two of which correspond to blind detections with no optical counterparts. At this significance level, our statistical analysis shows that about 60% of our candidates are expected to be spurious. For one of our blindly selected [C II] line candidates, we tentatively detect the CO(6-5) line in our parallel 3 mm line scan. None of the line candidates are individually detected in the 1.2 mm continuum. A stack of all [C II] candidates results in a tentative detection with S <SUB>1.2 mm</SUB> = 14 ± 5 μJy. This implies a dust-obscured star-formation rate (SFR) of (3 ± 1) M <SUB>☉</SUB> yr<SUP>-1</SUP>. We find that the two highest-SFR objects have candidate [C II] lines with luminosities that are consistent with the low-redshift L <SUB>[C II]</SUB> versus SFR relation. The other candidates have significantly higher [C II] luminosities than expected from their UV-based SFR. At the current sensitivity, it is unclear whether the majority of these sources are intrinsically bright [C II] emitters, or spurious sources. If only one of our line candidates was real (a scenario greatly favored by our statistical analysis), we find a source density for [C II] emitters at 6 < z < 8 that is significantly higher than predicted by current models and some extrapolations from galaxies in the local universe.||URI:||http://hdl.handle.net/20.500.12386/26259||URL:||https://iopscience.iop.org/article/10.3847/1538-4357/833/1/71||ISSN:||0004-637X||DOI:||10.3847/1538-4357/833/1/71||Bibcode ADS:||2016ApJ...833...71A||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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