The ALPINE-ALMA [C II] Survey: [C II] 158 mu m Emission Line Luminosity Functions at z similar to 4-6
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The ALPINE-ALMA [C II] Survey : [C II] 158 mu m Emission Line Luminosity Functions at z similar to 4-6. / Yan, Lin; Sajina, A.; Loiacono, F.; Lagache, G.; Bethermin, M.; Faisst, A.; Ginolfi, M.; Fevre, 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.
In: Astrophysical Journal, Vol. 905, No. 2, 147, 01.12.2020.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - The ALPINE-ALMA [C II] Survey
T2 - [C II] 158 mu m Emission Line Luminosity Functions at z similar to 4-6
AU - Yan, Lin
AU - Sajina, A.
AU - Loiacono, F.
AU - Lagache, G.
AU - Bethermin, M.
AU - Faisst, A.
AU - Ginolfi, M.
AU - Fevre, O. Le
AU - Gruppioni, C.
AU - Capak, P. L.
AU - Cassata, P.
AU - Schaerer, D.
AU - Silverman, J. D.
AU - Bardelli, S.
AU - Dessauges-Zavadsky, M.
AU - Cimatti, A.
AU - Hathi, N. P.
AU - Lemaux, B. C.
AU - Ibar, E.
AU - Jones, G. C.
AU - Koekemoer, Anton M.
AU - Oesch, P. A.
AU - Talia, M.
AU - Pozzi, F.
AU - Riechers, D. A.
AU - Tasca, L. A. M.
AU - Toft, Sune
AU - Vallini, L.
AU - Vergani, D.
AU - Zamorani, G.
AU - Zucca, E.
PY - 2020/12/1
Y1 - 2020/12/1
N2 - We present the [C II] 158 mu m line luminosity functions (LFs) at z similar to 4-6 using the ALMA observations of 118 sources, which are selected to have UV luminosity M-1500A < -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 similar to 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 similar to 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 similar to 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 similar to 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 similar to 4-6. Finally, we set a constraint on the molecular gas mass density at z similar to 4-6, with rho(mol) similar to (2-7) x 10(7)M Mpc(-3). This is broadly consistent with previous studies.
AB - We present the [C II] 158 mu m line luminosity functions (LFs) at z similar to 4-6 using the ALMA observations of 118 sources, which are selected to have UV luminosity M-1500A < -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 similar to 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 similar to 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 similar to 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 similar to 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 similar to 4-6. Finally, we set a constraint on the molecular gas mass density at z similar to 4-6, with rho(mol) similar to (2-7) x 10(7)M Mpc(-3). This is broadly consistent with previous studies.
KW - High-redshift galaxies
KW - Emission line galaxies
KW - Luminosity function
KW - Warm ionized medium
KW - Warm neutral medium
KW - Molecular gas
KW - STAR-FORMATION
KW - GALAXIES
KW - EPOCH
KW - DEEP
KW - GAS
U2 - 10.3847/1538-4357/abc41c
DO - 10.3847/1538-4357/abc41c
M3 - Journal article
VL - 905
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 147
ER -
ID: 271825679