A panchromatic view of N2CLS GOODS-N: The evolution of the dust cosmic density since z ∼ 7
2 LAM - Laboratoire d'Astrophysique de Marseille
3 LAGRANGE - Joseph Louis LAGRANGE
4 Cardiff University
5 AIM (UMR_7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation
6 IRAM - Instituto de RadioAstronomía Milimétrica
7 NEEL - HELFA - Hélium : du fondamental aux applications
8 ObAS - Observatoire astronomique de Strasbourg
9 University of Sussex
10 LPSC - Laboratoire de Physique Subatomique et de Cosmologie
11 NEEL - Cryo - Cryogénie
12 UNIROMA - Università degli Studi di Roma "La Sapienza" = Sapienza University [Rome]
13 IPAG - Institut de Planétologie et d'Astrophysique de Grenoble
14 IPM - Institute for Research in Fundamental Sciences [Tehran]
15 Université Paris-Saclay
16 CAB - Centro de Astrobiologia [Madrid]
17 NOA - National Observatory of Athens
18 ANL - Argonne National Laboratory [Lemont]
19 LERMA - Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique
20 ICE-CSIC - Institute of Space Sciences [Barcelona]
21 JAO - Joint ALMA Observatory
22 IRAP - Institut de recherche en astrophysique et planétologie
23 University of Leeds
24 Università degli Studi di Roma Tor Vergata [Roma, Italia] = University of Rome Tor Vergata [Rome, Italy] = Université de Rome Tor Vergata [Rome, Italie]
25 IAP - Institut d'Astrophysique de Paris
26 IP2I Lyon - Institut de Physique des 2 Infinis de Lyon
27 UNIGE - Université de Genève = University of Geneva
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Résumé
To understand early star formation, it is essential to determine the dust mass budget of high-redshift galaxies. Sub-millimeter rest-frame emission, dominated by cold dust, is an unbiased tracer of dust mass. The New IRAM KID Arrays 2 (NIKA2) conducted a deep blank field survey at 1.2 and 2.0 mm in the GOODS-N field as part of the NIKA2 Cosmological Legacy Survey (N2CLS), detecting 65 sources with S/N ≥ 4.2. Thanks to a dedicated interferometric program with NOEMA and other high-angular resolution data, we identified the multi-wavelength counterparts of these sources and resolved them into 71 individual galaxies. We built detailed spectral energy distributions (SEDs) and assigned a redshift to 68 of them over the range 0.6 < z < 7.2. We fit these SEDs using modified blackbody and Draine & Li (2007, ApJ, 657, 810) models and the panchromatic approaches MAGPHYS, CIGALE, and SED3FIT, thus deriving their dust mass (Mdust), infrared luminosity (LIR), and stellar mass (M⋆). Eight galaxies require an active galactic nucleus torus component, and another six require an unextinguished young stellar population. A significant fraction of our galaxies are classified as starbursts based on their position on the M⋆ versus star formation rate plane or their depletion timescales. We computed the dust mass function in three redshift bins (1.6 < z ≤ 2.4, 2.4 < z ≤ 4.2 and 4.2 < z ≤ 7.2) and determined the Schechter function that best describes it. The dust cosmic density, ρdust, increases by at least an order of magnitude from z ∼ 7 to z ∼ 1.5, as predicted by theoretical works. At lower redshifts, the evolution flattens. Nonetheless, significant differences exist between results obtained with different selections and methods. The superb GOODS-N data set enabled a systematic investigation into the dust properties of distant galaxies. N2CLS holds promise for combining these deep field findings with the wide COSMOS field into a self-consistent analysis of dust in galaxies both near and far.
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