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http://hdl.handle.net/20.500.12386/26259
Title: | The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Search for [CII] Line and Dust Emission in 6 | Authors: | Aravena, M. DECARLI, ROBERTO Walter, F. Bouwens, R. Oesch, P. A. Carilli, C. L. Bauer, F. E. Da Cunha, E. Daddi, E. Gónzalez-López, J. Ivison, R. J. Riechers, D. A. Smail, I. Swinbank, A. M. Weiss, A. Anguita, T. Bacon, R. Bell, E. Bertoldi, F. Cortes, P. Cox, P. Hodge, J. Ibar, E. Inami, H. Infante, L. Karim, A. Magnelli, B. Ota, K. Popping, G. van der Werf, P. Wagg, J. Fudamoto, Y. |
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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Aravena_2016_ApJ_833_71.pdf | Pdf editoriale | 4.42 MB | Adobe PDF | View/Open |
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