Papers › Characterizing the contribution of dust-obscured star formation at z ≳ 5 using 18...
Characterizing the contribution of dust-obscured star formation at z ≳ 5 using 18 serendipitously identified [CII] emitters
I. F. van Leeuwen, R. J. Bouwens, P. P. van der Werf, J. A. Hodge, S. Schouws, M. Stefanon, H. S. B. Algera, M. Aravena, L. A. Boogaard, R. A . A. Bowler, E. da Cunha, P. Dayal, R. Decarli, V. Gonzalez, H. Inami, I. de Looze, L. Sommovigo, B. P. Venemans, F. Walter, L. Barrufet, A. Ferrara, L. Graziani, A. P. S. Hygate, P. Oesch, M. Palla, L. Rowland, R. Schneider
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We present a new method to determine the star formation rate (SFR) density of the Universe at z ≳5 that includes the contribution of dust-obscured star formation. For this purpose, we use a [CII] (158 μm) selected sample of galaxies serendipitously identified in the fields of known z≳4.5 objects to characterize the fraction of obscured SFR. The advantage of a [CII] selection is that our sample is SFR-selected, in contrast to a UV-selection that would be biased towards unobscured star formation. We obtain a sample of 23 [CII] emitters near star-forming (SF) galaxies and QSOs -- three of which we identify for the first time -- using previous literature and archival ALMA data. 18 of these serendipitously identified galaxies have sufficiently deep rest-UV data and are used to characterize the obscured fraction of the star formation in galaxies with SFRs ≳30 M_⊙ yr⁻¹. We find that [CII] emitters identified around SF galaxies have ≈63\% of their SFR obscured, while [CII] emitters around QSOs have ≈93\% of their SFR obscured. By forward modeling existing wide-area UV luminosity function (LF) determinations, we derive the intrinsic UV LF using our characterization of the obscured SFR. Integrating the intrinsic LF to M_(UV) = $-$20 we find that the obscured SFRD contributes to $>3\%$ and $>10\%$ of the total SFRD at z ∼5 and z ∼6 based on our sample of companions galaxies near SFGs and QSOs, respectively. Our results suggest that dust obscuration is not negligible at z≳5, further underlining the importance of far-IR observations of the z≳5 Universe.
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