20.500.12556/RUL-181939 The z = 9.625 Cosmic Gems galaxy was a compact “blue monster” propelled by massive star clusters The recent discovery of five massive stellar clusters at ▫$z =9.625$▫ in the Cosmic Gems galaxy has raised the question about the formation mechanism of star clusters in the first 500 Myr after the Big Bang. We inferred the total stellar mass in clusters by normalizing and integrating the stellar cluster mass function (SCMF, ▫$\text{d}n(M)/\text{d}M = n_0 M^{\beta}$▫), assuming three different slopes (▫$\beta = -1.5, -2.0$▫, and ▫$-2.5$▫) and different lower-mass limits between ▫$10^2$▫ and ▫$10^5$▫ ▫$\text{M}_{\odot}$▫. We compared the total integrated cluster stellar mass to the stellar mass inferred from the counter image of the Cosmic Gems, which provides the best modestly magnified (▫$\mu = 1.84 \pm 0.05$▫) representation of the entire galaxy. The delensed stellar mass of the Cosmic Gems galaxy was estimated as ▫$3.5_{-1.8}^{+3.3}\times10^7\ \text{M}_{\odot}$▫, with an effective radius of ▫$R_{\text{eff}} = 103_{-15}^{+13}$▫ parsecs and a stellar surface mass density of ▫$\Sigma_{\text{mass}} = 520_{-225}^{+340}\ \text{M}_{\odot}\ \text{pc}^{-2}$▫. Accounting for normalization uncertainties – including different lensing magnification scenarios for the arc – a modified SCMF, combined with a significantly high star cluster formation efficiency (approaching 100%), appears to be a necessary condition to explain the relatively short formation timescale of both the star clusters and the counter image, without exceeding the galaxy’s stellar mass. By extrapolating the physical properties at the peak of the burst, we found that in its recent past (▫$\lesssim$▫30 Myr) the Cosmic Gems galaxy likely experienced a specific star formation rate exceeding ▫$25\ \text{Gyr}^{-1}$▫ and luminosity approaching the “blue monster” regime (▫$M_{\text{UV}} < -20$▫). Our study provides insights into the extreme clustered nature of star formation in early galaxies and sheds light on the formation of bound star clusters that might survive to ▫$z = 0$▫ as globular clusters older than 13 Gyr. galaxies high-redshift star formation galaksije rdeči premik nastanek zvezd true false true Angleški jezik Slovenski jezik Članek v reviji 2026-04-20 12:55:49 2026-04-20 12:55:50 2026-04-22 15:05:40 0000-00-00 00:00:00 2026 0 0 11 str. art. no. A171 Vol. 705 Jan. 2026 0000-00-00 Zaloznikova Objavljeno NiDoloceno 0000-00-00 0000-00-00 0000-00-00 524.8 1432-0746 10.1051/0004-6361/202556570 275763971 https://www.aanda.org/articles/aa/full_html/2026/01/aa56570-25/aa56570-25.html 1 436590cf-3ca7-11f1-b0ab-0050569b8976 https://repozitorij.uni-lj.si/Dokument.php?lang=slv&id=232747 aa56570-25.pdf aa56570-25.pdf 1 9199424BE1E4BB7D8D765EEB9EDFCAAA 10cf2019caa21708575e8079374bf242973c4b7e2a309c41263b36b979d55aa2 7808cdfa-3ca7-11f1-b0ab-0050569b8976 https://repozitorij.uni-lj.si/Dokument.php?lang=slv&id=232748 Fakulteta za matematiko in fiziko 0 0 0