Publication details for Professor Ian SmailAravena, M., Decarli, R., 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. (2016). The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Search for [CII] Line and Dust Emission in 6 < z < 8 Galaxies. The Astrophysical Journal 833(1): 71.
- Publication type: Journal Article
- ISSN/ISBN: 0004-637X, 1538-4357
- DOI: 10.3847/1538-4357/833/1/71
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Author(s) from Durham
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 [C ii] ~ (1.6–2.5) × 108 L ⊙. 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 1.2 mm = 14 ± 5 μJy. This implies a dust-obscured star-formation rate (SFR) of (3 ± 1) M ⊙ yr−1. We find that the two highest-SFR objects have candidate [C ii] lines with luminosities that are consistent with the low-redshift L [C ii] 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.