Details

Autor(en) / Beteiligte

• Yan, Lin
• Sajina, A.
• Loiacono, F.
• Lagache, G.
• Béthermin, M.
• Faisst, A.
• Ginolfi, M.
• Fèvre, O. Le
• Gruppioni, C.
• Capak, P. L.
• Cassata, P.
• Schaerer, D.
• Silverman, J. D.
• Bardelli, S.
• Dessauges-Zavadsky, M.
• Cimatti, A.
• Hathi, N. P.
• Lemaux, B. C.
• Ibar, E.
• Jones, G. C.
• Koekemoer, Anton M.
• Oesch, P. A.
• Talia, M.
• Pozzi, F.
• Riechers, D. A.
• Tasca, L. A. M.
• Toft, Sune
• Vallini, L.
• Vergani, D.
• Zamorani, G.
• Zucca, E.

Titel

The ALPINE-ALMA [C II] Survey: [C II] 158 μm Emission Line Luminosity Functions at z ∼ 4–6

Ist Teil von

• The Astrophysical journal, 2020-12, Vol.905 (2), p.147

Ort / Verlag

Philadelphia: IOP Publishing

Erscheinungsjahr

2020

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• Abstract We present the [C II] 158 μ m line luminosity functions (LFs) at z  ∼ 4–6 using the ALMA observations of 118 sources, which are selected to have UV luminosity M 1500Å  < −20.2 and optical spectroscopic redshifts in COSMOS and ECDF-S. Of the 118 targets, 75 have significant [C II] detections and 43 are upper limits. This is by far the largest sample of [C II] detections, which allows us to set constraints on the volume density of [C II] emitters at z  ∼ 4–6. But because this is a UV-selected sample, we are missing [C II]-bright but UV-faint sources, making our constraints strict lower limits. Our derived LFs are statistically consistent with the z  ∼ 0 [C II] LF at 10 8.25 –10 9.75 L ⊙ . We compare our results with the upper limits of the [C II] LF derived from serendipitous sources in the ALPINE maps. We also infer the [C II] LFs based on published far-IR and CO LFs at z  ∼ 4–6. Combining our robust lower limits with these additional estimates, we set further constraints on the true number density of [C II] emitters at z  ∼ 4–6. These additional LF estimates are largely above our LF at L [CII]  > 10 9 L ⊙ , suggesting that UV-faint but [C II]-bright sources likely make significant contributions to the [C II] emitter volume density. When we include all the LF estimates, we find that available model predictions underestimate the number densities of [C II] emitters at z  ∼ 4–6. Finally, we set a constraint on the molecular gas mass density at z  ∼ 4–6, with ρ mol  ∼ (2–7) × 10 7 M ⊙ Mpc −3 . This is broadly consistent with previous studies.