학술논문
Life beyond 30: probing the -20
Astrophysics - Astrophysics of Galaxies
Document Type
Working Paper
Author
Pérez-González, Pablo G.; Costantin, Luca; Langeroodi, Danial; Rinaldi, Pierluigi; Annunziatella, Marianna; Ilbert, Olivier; Colina, Luis; Noorgaard-Nielsen, Hans Ulrik; Greve, Thomas; Ostlin, Göran; Wright, Gillian; Alonso-Herrero, Almudena; Álvarez-Márquez, Javier; Caputi, Karina I.; Eckart, Andreas; Fèvre, Olivier Le; Labiano, Álvaro; García-Marín, Macarena; Hjorth, Jens; Kendrew, Sarah; Pye, John P.; Tikkanen, Tuomo; van der Werf, Paul; Walter, Fabian; Ward, Martin; Bik, Arjan; Boogaard, Leindert; Bosman, Sarah E. I.; Gómez, Alejandro Crespo; Gillman, Steven; Iani, Edoardo; Jermann, Iris; Melinder, Jens; Meyer, Romain A.; Moutard, Thibaud; van Dishoek, Ewine; Henning, Thomas; Lagage, Pierre-Olivier; Guedel, Manuel; Peissker, Florian; Ray, Tom; Vandenbussche, Bart; García-Argumánez, Ángela; Mérida, Rosa María
Source
Subject
Language
Abstract
We present the ultraviolet luminosity function and an estimate of the cosmic star formation rate density at $88$ galaxy candidates based on their dropout nature in the F115W and/or F150W filters, a high probability for their photometric redshifts, estimated with three different codes, being at $z>8$, good fits based on $\chi^2$ calculations, and predominant solutions compared to $z<8$ alternatives. We find mild evolution in the luminosity function from $z\sim13$ to $z\sim8$, i.e., only a small increase in the average number density of $\sim$0.2 dex, while the faint-end slope and absolute magnitude of the knee remain approximately constant, with values $\alpha=-2.2\pm0.1$ and $M^*=-20.8\pm0.2$ mag. Comparing our results with the predictions of state-of-the-art galaxy evolution models, we find two main results: (1) a slower increase with time in the cosmic star formation rate density compared to a steeper rise predicted by models; (2) nearly a factor of 10 higher star formation activity concentrated in scales around 2 kpc in galaxies with stellar masses $\sim10^8$ M$_\odot$ during the first 350 Myr of the Universe, $z\sim12$, with models matching better the luminosity density observational estimations $\sim$150 Myr later, by $z\sim9$.
Comment: Accepted for publication in ApJL, in memoriam Hans Ulrik Noorgaard-Nielsen and Olivier Le F\`evre
Comment: Accepted for publication in ApJL, in memoriam Hans Ulrik Noorgaard-Nielsen and Olivier Le F\`evre