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Early Results from GLASS-JWST. XI. Stellar Masses and Mass-to-light Ratio of z > 7 Galaxies

Santini, P. and Fontana, A. and Castellano, M. and Leethochawalit, N. and Trenti, M. and Treu, T. and Belfiori, D. and Birrer, S. and Bonchi, A. and Merlin, E. and Mason, C. and Morishita, T. and Nonino, M. and Paris, D. and Polenta, G. and Rosati, P. and Yang, L. and Boyett, K. and Bradac, M. and Calabrò, A. and Dressler, A. and Glazebrook, K. and Marchesini, D. and Mascia, S. and Nanayakkara, T. and Pentericci, L. and Roberts-Borsani, G. and Scarlata, C. and Vulcani, B. and Wang, Xin (2023) Early Results from GLASS-JWST. XI. Stellar Masses and Mass-to-light Ratio of z > 7 Galaxies. Astrophysical Journal Letters, 942 (2). Art. No. L27. ISSN 2041-8205. doi:10.3847/2041-8213/ac9586.

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We exploit James Webb Space Telescope (JWST) NIRCam observations from the GLASS-JWST-Early Release Science program to investigate galaxy stellar masses at z > 7. We first show that JWST observations reduce the uncertainties on the stellar mass by a factor of at least 5–10, when compared with the highest-quality data sets available to date. We then study the UV mass-to-light ratio, finding that galaxies exhibit a a two orders of magnitude range of M/L_(UV) values for a given luminosity, indicative of a broad variety of physical conditions and star formation histories. As a consequence, previous estimates of the cosmic stellar-mass density — based on an average correlation between UV luminosity and stellar mass — can be biased by as much as a factor of ∼6. Our first exploration demonstrates that JWST represents a new era in our understanding of stellar masses at z > 7 and, therefore, of the growth of galaxies prior to cosmic reionization.

Item Type:Article
Related URLs:
URLURL TypeDescription
Santini, P.0000-0002-9334-8705
Fontana, A.0000-0003-3820-2823
Castellano, M.0000-0001-9875-8263
Leethochawalit, N.0000-0003-4570-3159
Trenti, M.0000-0001-9391-305X
Treu, T.0000-0002-8460-0390
Birrer, S.0000-0003-3195-5507
Bonchi, A.0000-0002-2667-5482
Merlin, E.0000-0001-6870-8900
Mason, C.0000-0002-3407-1785
Morishita, T.0000-0002-8512-1404
Nonino, M.0000-0001-6342-9662
Paris, D.0000-0002-7409-8114
Polenta, G.0000-0003-4067-9196
Rosati, P.0000-0002-6813-0632
Yang, L.0000-0002-8434-880X
Boyett, K.0000-0003-4109-304X
Bradac, M.0000-0001-5984-0395
Calabrò, A.0000-0003-2536-1614
Dressler, A.0000-0002-6317-0037
Glazebrook, K.0000-0002-3254-9044
Marchesini, D.0000-0001-9002-3502
Mascia, S.0000-0002-9572-7813
Nanayakkara, T.0000-0003-2804-0648
Pentericci, L.0000-0001-8940-6768
Roberts-Borsani, G.0000-0002-4140-1367
Scarlata, C.0000-0002-9136-8876
Vulcani, B.0000-0003-0980-1499
Wang, Xin0000-0002-9373-3865
Additional Information:This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program JWST-ERS-1324. The JWST data used in this paper can be found on MAST:10.17909/fqaq-p393. We acknowledge financial support from NASA through grant JWST-ERS-1324. K.G. and T.N. acknowledge support from Australian Research Council Laureate Fellowship FL180100060. M.B. acknowledges support from the Slovenian national research agency ARRS through grant N1-0238. P.R. acknowledges financial support through grants PRIN-MIUR 2017WSCC32 and 2020SKSTHZ. M.N. acknowledges INAF Mainstream P.S., M.C., and E.M. acknowledge INAF Mini-Grant "The evolution of passive galaxies through cosmic time."
Funding AgencyGrant Number
Australian Research CouncilFL180100060
Slovenian National Research AgencyN1-0238
Ministero dell’Istruzione, dell’Università e della Ricerca (MIUR)2017WSCC32
Ministero dell’Istruzione, dell’Università e della Ricerca (MIUR)2020SKSTHZ
NASANAS 5-03127
Istituto Nazionale di Astrofisica (INAF)
Issue or Number:2
Record Number:CaltechAUTHORS:20230203-893712500.44
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:119036
Deposited By: Research Services Depository
Deposited On:01 Mar 2023 01:37
Last Modified:01 Mar 2023 01:37

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