The ALMA REBELS survey: the dust-obscured cosmic star formation rate density at redshift 7

Hiddo S.B. Algera; Hanae Inami; Pascal A. Oesch; Laura Sommovigo; Rychard J. Bouwens; Michael W. Topping; Sander Schouws; Mauro Stefanon; Daniel P. Stark; Manuel Aravena; Laia Barrufet; Elisabete da Cunha; Pratika Dayal; Ryan Endsley; Andrea Ferrara; Yoshinobu Fudamoto; Valentino Gonzalez; Luca Graziani; Jacqueline A. Hodge; Alexander P.S. Hygate; Ilse de Looze; Themiya Nanayakkara; Raffaella Schneider; Paul P. van der Werf

doi:10.1093/mnras/stac3195

The ALMA REBELS survey: the dust-obscured cosmic star formation rate density at redshift 7

Hiddo S.B. Algera, Hanae Inami, Pascal A. Oesch, Laura Sommovigo, Rychard J. Bouwens, Michael W. Topping, Sander Schouws, Mauro Stefanon, Daniel P. Stark, Manuel Aravena, Laia Barrufet, Elisabete da Cunha, Pratika Dayal, Ryan Endsley, Andrea Ferrara, Yoshinobu Fudamoto, Valentino Gonzalez, Luca Graziani, Jacqueline A. Hodge, Alexander P.S. HygateIlse de Looze, Themiya Nanayakkara, Raffaella Schneider, Paul P. van der Werf

International Centre for Radio Astronomy Research (ICRAR)

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Abstract

Cosmic dust is an essential component shaping both the evolution of galaxies and their observational signatures. How quickly dust builds up in the early Universe remains an open question that requires deep observations at (sub-)millimetre wavelengths to resolve. Here, we use Atacama Large Millimeter Array observations of 45 galaxies from the Reionization Era Bright Emission Line Survey (REBELS) and its pilot programs, designed to target [C II] and dust emission in UV-selected galaxies at z ∼ 7, to investigate the dust content of high-redshift galaxies through a stacking analysis. We find that the typical fraction of obscured star formation f_obs = SFR_IR/SFR_UV+_IR depends on stellar mass, similar to what is observed at lower redshift, and ranges from f_obs ≈ 0.3 − 0.6 for galaxies with log₁₀(M_*/M_☉) = 9.4–10.4. We further adopt the z ∼ 7 stellar mass function from the literature to extract the obscured cosmic star formation rate density (SFRD) from the REBELS survey. Our results suggest only a modest decrease in the SFRD between 3 ≲ z ≲ 7, with dust-obscured star formation still contributing ∼30 per cent at z ∼ 7. While we extensively discuss potential caveats, our analysis highlights the continued importance of dust-obscured star formation even well into the epoch of reionization.

Original language	English
Pages (from-to)	6142-6157
Number of pages	16
Journal	Monthly Notices of the Royal Astronomical Society
Volume	518
Issue number	4
DOIs	https://doi.org/10.1093/mnras/stac3195
Publication status	Published - 1 Feb 2023

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Full Text_Algera et al_2022_The ALMA REBELS survey
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Algera, H. S. B., Inami, H., Oesch, P. A., Sommovigo, L., Bouwens, R. J., Topping, M. W., Schouws, S., Stefanon, M., Stark, D. P., Aravena, M., Barrufet, L., da Cunha, E., Dayal, P., Endsley, R., Ferrara, A., Fudamoto, Y., Gonzalez, V., Graziani, L., Hodge, J. A., ... van der Werf, P. P. (2023). The ALMA REBELS survey: the dust-obscured cosmic star formation rate density at redshift 7. Monthly Notices of the Royal Astronomical Society, 518(4), 6142-6157. https://doi.org/10.1093/mnras/stac3195

@article{cbb2c16928ce4e698b9078cb8e763c5c,

title = "The ALMA REBELS survey: the dust-obscured cosmic star formation rate density at redshift 7",

abstract = "Cosmic dust is an essential component shaping both the evolution of galaxies and their observational signatures. How quickly dust builds up in the early Universe remains an open question that requires deep observations at (sub-)millimetre wavelengths to resolve. Here, we use Atacama Large Millimeter Array observations of 45 galaxies from the Reionization Era Bright Emission Line Survey (REBELS) and its pilot programs, designed to target [C II] and dust emission in UV-selected galaxies at z ∼ 7, to investigate the dust content of high-redshift galaxies through a stacking analysis. We find that the typical fraction of obscured star formation fobs = SFRIR/SFRUV+IR depends on stellar mass, similar to what is observed at lower redshift, and ranges from fobs ≈ 0.3 − 0.6 for galaxies with log10(M*/M☉) = 9.4–10.4. We further adopt the z ∼ 7 stellar mass function from the literature to extract the obscured cosmic star formation rate density (SFRD) from the REBELS survey. Our results suggest only a modest decrease in the SFRD between 3 ≲ z ≲ 7, with dust-obscured star formation still contributing ∼30 per cent at z ∼ 7. While we extensively discuss potential caveats, our analysis highlights the continued importance of dust-obscured star formation even well into the epoch of reionization.",

keywords = "galaxies: evolution, galaxies: high-redshift, submillimetre: galaxies",

author = "Algera, {Hiddo S.B.} and Hanae Inami and Oesch, {Pascal A.} and Laura Sommovigo and Bouwens, {Rychard J.} and Topping, {Michael W.} and Sander Schouws and Mauro Stefanon and Stark, {Daniel P.} and Manuel Aravena and Laia Barrufet and {da Cunha}, Elisabete and Pratika Dayal and Ryan Endsley and Andrea Ferrara and Yoshinobu Fudamoto and Valentino Gonzalez and Luca Graziani and Hodge, {Jacqueline A.} and Hygate, {Alexander P.S.} and {de Looze}, Ilse and Themiya Nanayakkara and Raffaella Schneider and {van der Werf}, {Paul P.}",

note = "Funding Information: We thank the anonymous reviewer for providing useful feedback that improved this manuscript. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2019.1.01634.L, ADS/JAO.ALMA#2017.1.01217.S, ADS/JAO.ALMA#2017.1.00604.S, ADS/JAO.ALMA#2018.1.00236.S, ADS/JAO.ALMA#2018.1.00085.S, ADS/JAO.ALMA#2018.A.00022.S. We acknowledge assistance from Allegro, the European ALMA Regional Center node in the Netherlands. This work was supported by NAOJ ALMA Scientific Research Grant Code 2021-19A (HSBA and HI). We acknowledge support from the Swiss National Science Foundation through project grant 200020 207349 (PAO, LB). The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. MS acknowledges support from the CIDEGENT/2021/059 grant, and from project PID2019-109592GBI00/AEI/10.13039/501100011033 from the Spanish Ministerio de Ciencia e Innovaci{\'o}n – Agencia Estatal de Investigaci{\'o}n. MA acknowledges support from FONDECYT grant 1211951, {\textquoteleft}ANID + PCI + INSTITUTO MAX PLANCK DE ASTRONOMIA MPG 190030{\textquoteright}, {\textquoteleft}ANID + PCI + REDES 190194{\textquoteright}, and ANID BASAL project FB210003. PD acknowledges support from the NWO grant 016.VIDI.189.162 ({\textquoteleft}ODIN{\textquoteright}) and the European Commission{\textquoteright}s and University of Groningen{\textquoteright}s CO-FUND Rosalind Franklin program. YF acknowledges support from NAOJ ALMA Scientific Research Grant number 2020-16B. IDL acknowledges support from ERC starting grant #851622 DustOrigin. Funding Information: We acknowledge assistance from Allegro, the European ALMA Regional Center node in the Netherlands. This work was supported by NAOJ ALMA Scientific Research Grant Code 2021-19A (HSBA and HI). We acknowledge support from the Swiss National Science Foundation through project grant 200020 207349 (PAO, LB). The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. MS acknowledges support from the CIDEGENT/2021/059 grant, and from project PID2019-109592GB-I00/AEI/10.13039/501100011033 from the Spanish Ministerio de Ciencia e Innovaci{\'o}n – Agencia Estatal de Investigaci{\'o}n. MA acknowledges support from FONDECYT grant 1211951, {\textquoteleft}ANID + PCI + INSTITUTO MAX PLANCK DE ASTRONOMIA MPG 190030{\textquoteright}, {\textquoteleft}ANID + PCI + REDES 190194{\textquoteright}, and ANID BASAL project FB210003. PD acknowledges support from the NWO grant 016.VIDI.189.162 ({\textquoteleft}ODIN{\textquoteright}) and the European Commission{\textquoteright}s and University of Groningen{\textquoteright}s CO-FUND Rosalind Franklin program. YF acknowledges support from NAOJ ALMA Scientific Research Grant number 2020-16B. IDL acknowledges support from ERC starting grant #851622 DustOrigin. Publisher Copyright: {\textcopyright} 2022 The Author(s).",

year = "2023",

month = feb,

day = "1",

doi = "10.1093/mnras/stac3195",

language = "English",

volume = "518",

pages = "6142--6157",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "4",

}

Algera, HSB, Inami, H, Oesch, PA, Sommovigo, L, Bouwens, RJ, Topping, MW, Schouws, S, Stefanon, M, Stark, DP, Aravena, M, Barrufet, L, da Cunha, E, Dayal, P, Endsley, R, Ferrara, A, Fudamoto, Y, Gonzalez, V, Graziani, L, Hodge, JA, Hygate, APS, de Looze, I, Nanayakkara, T, Schneider, R & van der Werf, PP 2023, 'The ALMA REBELS survey: the dust-obscured cosmic star formation rate density at redshift 7', Monthly Notices of the Royal Astronomical Society, vol. 518, no. 4, pp. 6142-6157. https://doi.org/10.1093/mnras/stac3195

TY - JOUR

T1 - The ALMA REBELS survey

T2 - the dust-obscured cosmic star formation rate density at redshift 7

AU - Algera, Hiddo S.B.

AU - Inami, Hanae

AU - Oesch, Pascal A.

AU - Sommovigo, Laura

AU - Bouwens, Rychard J.

AU - Topping, Michael W.

AU - Schouws, Sander

AU - Stefanon, Mauro

AU - Stark, Daniel P.

AU - Aravena, Manuel

AU - Barrufet, Laia

AU - da Cunha, Elisabete

AU - Dayal, Pratika

AU - Endsley, Ryan

AU - Ferrara, Andrea

AU - Fudamoto, Yoshinobu

AU - Gonzalez, Valentino

AU - Graziani, Luca

AU - Hodge, Jacqueline A.

AU - Hygate, Alexander P.S.

AU - de Looze, Ilse

AU - Nanayakkara, Themiya

AU - Schneider, Raffaella

AU - van der Werf, Paul P.

N1 - Funding Information: We thank the anonymous reviewer for providing useful feedback that improved this manuscript. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2019.1.01634.L, ADS/JAO.ALMA#2017.1.01217.S, ADS/JAO.ALMA#2017.1.00604.S, ADS/JAO.ALMA#2018.1.00236.S, ADS/JAO.ALMA#2018.1.00085.S, ADS/JAO.ALMA#2018.A.00022.S. We acknowledge assistance from Allegro, the European ALMA Regional Center node in the Netherlands. This work was supported by NAOJ ALMA Scientific Research Grant Code 2021-19A (HSBA and HI). We acknowledge support from the Swiss National Science Foundation through project grant 200020 207349 (PAO, LB). The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. MS acknowledges support from the CIDEGENT/2021/059 grant, and from project PID2019-109592GBI00/AEI/10.13039/501100011033 from the Spanish Ministerio de Ciencia e Innovación – Agencia Estatal de Investigación. MA acknowledges support from FONDECYT grant 1211951, ‘ANID + PCI + INSTITUTO MAX PLANCK DE ASTRONOMIA MPG 190030’, ‘ANID + PCI + REDES 190194’, and ANID BASAL project FB210003. PD acknowledges support from the NWO grant 016.VIDI.189.162 (‘ODIN’) and the European Commission’s and University of Groningen’s CO-FUND Rosalind Franklin program. YF acknowledges support from NAOJ ALMA Scientific Research Grant number 2020-16B. IDL acknowledges support from ERC starting grant #851622 DustOrigin. Funding Information: We acknowledge assistance from Allegro, the European ALMA Regional Center node in the Netherlands. This work was supported by NAOJ ALMA Scientific Research Grant Code 2021-19A (HSBA and HI). We acknowledge support from the Swiss National Science Foundation through project grant 200020 207349 (PAO, LB). The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. MS acknowledges support from the CIDEGENT/2021/059 grant, and from project PID2019-109592GB-I00/AEI/10.13039/501100011033 from the Spanish Ministerio de Ciencia e Innovación – Agencia Estatal de Investigación. MA acknowledges support from FONDECYT grant 1211951, ‘ANID + PCI + INSTITUTO MAX PLANCK DE ASTRONOMIA MPG 190030’, ‘ANID + PCI + REDES 190194’, and ANID BASAL project FB210003. PD acknowledges support from the NWO grant 016.VIDI.189.162 (‘ODIN’) and the European Commission’s and University of Groningen’s CO-FUND Rosalind Franklin program. YF acknowledges support from NAOJ ALMA Scientific Research Grant number 2020-16B. IDL acknowledges support from ERC starting grant #851622 DustOrigin. Publisher Copyright: © 2022 The Author(s).

PY - 2023/2/1

Y1 - 2023/2/1

N2 - Cosmic dust is an essential component shaping both the evolution of galaxies and their observational signatures. How quickly dust builds up in the early Universe remains an open question that requires deep observations at (sub-)millimetre wavelengths to resolve. Here, we use Atacama Large Millimeter Array observations of 45 galaxies from the Reionization Era Bright Emission Line Survey (REBELS) and its pilot programs, designed to target [C II] and dust emission in UV-selected galaxies at z ∼ 7, to investigate the dust content of high-redshift galaxies through a stacking analysis. We find that the typical fraction of obscured star formation fobs = SFRIR/SFRUV+IR depends on stellar mass, similar to what is observed at lower redshift, and ranges from fobs ≈ 0.3 − 0.6 for galaxies with log10(M*/M☉) = 9.4–10.4. We further adopt the z ∼ 7 stellar mass function from the literature to extract the obscured cosmic star formation rate density (SFRD) from the REBELS survey. Our results suggest only a modest decrease in the SFRD between 3 ≲ z ≲ 7, with dust-obscured star formation still contributing ∼30 per cent at z ∼ 7. While we extensively discuss potential caveats, our analysis highlights the continued importance of dust-obscured star formation even well into the epoch of reionization.

AB - Cosmic dust is an essential component shaping both the evolution of galaxies and their observational signatures. How quickly dust builds up in the early Universe remains an open question that requires deep observations at (sub-)millimetre wavelengths to resolve. Here, we use Atacama Large Millimeter Array observations of 45 galaxies from the Reionization Era Bright Emission Line Survey (REBELS) and its pilot programs, designed to target [C II] and dust emission in UV-selected galaxies at z ∼ 7, to investigate the dust content of high-redshift galaxies through a stacking analysis. We find that the typical fraction of obscured star formation fobs = SFRIR/SFRUV+IR depends on stellar mass, similar to what is observed at lower redshift, and ranges from fobs ≈ 0.3 − 0.6 for galaxies with log10(M*/M☉) = 9.4–10.4. We further adopt the z ∼ 7 stellar mass function from the literature to extract the obscured cosmic star formation rate density (SFRD) from the REBELS survey. Our results suggest only a modest decrease in the SFRD between 3 ≲ z ≲ 7, with dust-obscured star formation still contributing ∼30 per cent at z ∼ 7. While we extensively discuss potential caveats, our analysis highlights the continued importance of dust-obscured star formation even well into the epoch of reionization.

KW - galaxies: evolution

KW - galaxies: high-redshift

KW - submillimetre: galaxies

UR - http://www.scopus.com/inward/record.url?scp=85145962928&partnerID=8YFLogxK

U2 - 10.1093/mnras/stac3195

DO - 10.1093/mnras/stac3195

M3 - Article

AN - SCOPUS:85145962928

SN - 0035-8711

VL - 518

SP - 6142

EP - 6157

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

The ALMA REBELS survey: the dust-obscured cosmic star formation rate density at redshift 7

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