Characterizing the contribution of dust-obscured star formation at $z \gtrsim$ 5 using 18 serendipitously identified [CII] emitters

Fuente: arXiv

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Autori principali:	van Leeuwen, I. F., Bouwens, R. J., van der Werf, P. P., Hodge, J. A., Schouws, S., Stefanon, M., Algera, H. S. B., Aravena, M., Boogaard, L. A., Bowler, R. A . A., da Cunha, E., Dayal, P., Decarli, R., Gonzalez, V., Inami, H., de Looze, I., Sommovigo, L., Venemans, B. P., Walter, F., Barrufet, L., Ferrara, A., Graziani, L., Hygate, A. P. S., Oesch, P., Palla, M., Rowland, L., Schneider, R.
Natura:	Preprint
Pubblicazione:	2024
Soggetti:	Astrophysics of Galaxies
Accesso online:	Acceder al recurso
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author	van Leeuwen, I. F. Bouwens, R. J. van der Werf, P. P. Hodge, J. A. Schouws, S. Stefanon, M. Algera, H. S. B. Aravena, M. Boogaard, L. A. Bowler, R. A . A. da Cunha, E. Dayal, P. Decarli, R. Gonzalez, V. Inami, H. de Looze, I. Sommovigo, L. Venemans, B. P. Walter, F. Barrufet, L. Ferrara, A. Graziani, L. Hygate, A. P. S. Oesch, P. Palla, M. Rowland, L. Schneider, R.
author_facet	van Leeuwen, I. F. Bouwens, R. J. van der Werf, P. P. Hodge, J. A. Schouws, S. Stefanon, M. Algera, H. S. B. Aravena, M. Boogaard, L. A. Bowler, R. A . A. da Cunha, E. Dayal, P. Decarli, R. Gonzalez, V. Inami, H. de Looze, I. Sommovigo, L. Venemans, B. P. Walter, F. Barrufet, L. Ferrara, A. Graziani, L. Hygate, A. P. S. Oesch, P. Palla, M. Rowland, L. Schneider, R.
contents	We present a new method to determine the star formation rate (SFR) density of the Universe at $z \gtrsim 5$ that includes the contribution of dust-obscured star formation. For this purpose, we use a [CII] (158 $μ$m) selected sample of galaxies serendipitously identified in the fields of known $z\gtrsim 4.5$ 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 $\gtrsim 30\ \text{M}_{\odot} \ \text{yr}^{-1}$. We find that [CII] emitters identified around SF galaxies have $\approx$63\% of their SFR obscured, while [CII] emitters around QSOs have $\approx$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 $z \sim 5$ and $z \sim 6$ based on our sample of companions galaxies near SFGs and QSOs, respectively. Our results suggest that dust obscuration is not negligible at $z\gtrsim 5$, further underlining the importance of far-IR observations of the $z\gtrsim 5$ Universe.
format	Preprint
id	arxiv_https___arxiv_org_abs_2409_11463
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	Characterizing the contribution of dust-obscured star formation at $z \gtrsim$ 5 using 18 serendipitously identified [CII] emitters van Leeuwen, I. F. Bouwens, R. J. van der Werf, P. P. Hodge, J. A. Schouws, S. Stefanon, M. Algera, H. S. B. Aravena, M. Boogaard, L. A. Bowler, R. A . A. da Cunha, E. Dayal, P. Decarli, R. Gonzalez, V. Inami, H. de Looze, I. Sommovigo, L. Venemans, B. P. Walter, F. Barrufet, L. Ferrara, A. Graziani, L. Hygate, A. P. S. Oesch, P. Palla, M. Rowland, L. Schneider, R. Astrophysics of Galaxies We present a new method to determine the star formation rate (SFR) density of the Universe at $z \gtrsim 5$ that includes the contribution of dust-obscured star formation. For this purpose, we use a [CII] (158 $μ$m) selected sample of galaxies serendipitously identified in the fields of known $z\gtrsim 4.5$ 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 $\gtrsim 30\ \text{M}_{\odot} \ \text{yr}^{-1}$. We find that [CII] emitters identified around SF galaxies have $\approx$63\% of their SFR obscured, while [CII] emitters around QSOs have $\approx$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 $z \sim 5$ and $z \sim 6$ based on our sample of companions galaxies near SFGs and QSOs, respectively. Our results suggest that dust obscuration is not negligible at $z\gtrsim 5$, further underlining the importance of far-IR observations of the $z\gtrsim 5$ Universe.
title	Characterizing the contribution of dust-obscured star formation at $z \gtrsim$ 5 using 18 serendipitously identified [CII] emitters
topic	Astrophysics of Galaxies
url	https://arxiv.org/abs/2409.11463