TY - JOUR
T1 - The ALPINE-ALMA [CII] survey
T2 - Dust attenuation properties and obscured star formation at z ∼4.4-5.8
AU - Fudamoto, Y.
AU - Oesch, P. A.
AU - Faisst, A.
AU - Béthermin, M.
AU - Ginolfi, M.
AU - Khusanova, Y.
AU - Loiacono, F.
AU - Le Fèvre, O.
AU - Capak, P.
AU - Schaerer, D.
AU - Silverman, J. D.
AU - Cassata, P.
AU - Yan, L.
AU - Amorin, R.
AU - Bardelli, S.
AU - Boquien, M.
AU - Cimatti, A.
AU - Dessauges-Zavadsky, M.
AU - Fujimoto, S.
AU - Gruppioni, C.
AU - Hathi, N. P.
AU - Ibar, E.
AU - Jones, G. C.
AU - Koekemoer, A. M.
AU - Lagache, G.
AU - Lemaux, B. C.
AU - Maiolino, R.
AU - Narayanan, D.
AU - Pozzi, F.
AU - Riechers, D. A.
AU - Rodighiero, G.
AU - Talia, M.
AU - Toft, S.
AU - Vallini, L.
AU - Vergani, D.
AU - Zamorani, G.
AU - Zucca, E.
N1 - Funding Information:
Acknowledgements. This paper is dedicated to the memory of Olivier Le Fèvre, PI of the ALPINE survey. We thank the anonymous referee for insightful comments that improved the quality of this manuscript. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.00428.L. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and 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. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TER-APIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. This work was supported by the Swiss National Science Foundation through the SNSF Professorship grant 157567 “Galaxy Build-up at Cosmic Dawn”. G.C.J. acknowledges ERC Advanced Grant 695671 “QUENCH” and support by the Science and Technology Facilities Council (STFC). D.R. acknowledges support from the National Science Foundation under grant number AST-1614213 and from the Alexander von Humboldt Foundation through a Humboldt Research Fellowship for Experienced Researchers. A.C., F.P. and M.T. acknowledge the grant MIUR PRIN2017. LV acknowledges funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie Grant agreement No. 746119. S.F. is supported by and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under then grant No. 140. R.A. acknowledges support from FONDE-CYT Regular Grant 1202007.
Publisher Copyright:
© 2020 ESO.
PY - 2020/11/1
Y1 - 2020/11/1
N2 - We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ∼4.4 - 5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158 μm obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope (β), stellar mass (M∗), and infrared excess (IRX = LIR/LUV). Twenty-three galaxies are individually detected in the continuum at > 3.5σ significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z ∼ 4.4 - 5.8. The individual detections and stacks show that the IRX-β relation at z ∼ 5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z < 4). The attenuation curve is similar to or even steeper than that of the extinction curve of the Small Magellanic Cloud. This systematic change of the IRX-β relation as a function of redshift suggests an evolution of dust attenuation properties at z > 4. Similarly, we find that our galaxies have lower IRX values, up to 1 dex on average, at a fixed mass compared to previously studied IRX-M∗ relations at z 4, albeit with significant scatter. This implies a lower obscured fraction of star formation than at lower redshifts. Our results suggest that dust properties of UV-selected star forming galaxies at z 4 are characterised by (i) a steeper attenuation curve than at z 4, and (ii) a rapidly decreasing dust obscured fraction of star formation as a function of redshift. Nevertheless, even among this UV-selected sample, massive galaxies (log M∗/M· > 10) at z ∼ 5 - 6 already exhibit an obscured fraction of star formation of ∼45%, indicating a rapid build-up of dust during the epoch of reionization.
AB - We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ∼4.4 - 5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158 μm obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope (β), stellar mass (M∗), and infrared excess (IRX = LIR/LUV). Twenty-three galaxies are individually detected in the continuum at > 3.5σ significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z ∼ 4.4 - 5.8. The individual detections and stacks show that the IRX-β relation at z ∼ 5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z < 4). The attenuation curve is similar to or even steeper than that of the extinction curve of the Small Magellanic Cloud. This systematic change of the IRX-β relation as a function of redshift suggests an evolution of dust attenuation properties at z > 4. Similarly, we find that our galaxies have lower IRX values, up to 1 dex on average, at a fixed mass compared to previously studied IRX-M∗ relations at z 4, albeit with significant scatter. This implies a lower obscured fraction of star formation than at lower redshifts. Our results suggest that dust properties of UV-selected star forming galaxies at z 4 are characterised by (i) a steeper attenuation curve than at z 4, and (ii) a rapidly decreasing dust obscured fraction of star formation as a function of redshift. Nevertheless, even among this UV-selected sample, massive galaxies (log M∗/M· > 10) at z ∼ 5 - 6 already exhibit an obscured fraction of star formation of ∼45%, indicating a rapid build-up of dust during the epoch of reionization.
KW - Dust
KW - Extinction
KW - Galaxies: ISM
KW - Galaxies: high-redshift
UR - http://www.scopus.com/inward/record.url?scp=85095114868&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85095114868&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202038163
DO - 10.1051/0004-6361/202038163
M3 - Review article
AN - SCOPUS:85095114868
SN - 0004-6361
VL - 643
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A4
ER -