| Title | Modelling globular clusters in the TNG50 simulation: predictions from dwarfs to giant galaxies |
| Authors | Doppel, Jessica E. Sales, Laura, V Nelson, Dylan Pillepich, Annalisa Abadi, Mario G. Peng, Eric W. Marinacci, Federico Naiman, Jill Torrey, Paul Vogelsberger, Mark Weinberger, Rainer Hernquist, Lars |
| Affiliation | Univ Calif Riverside, 900 Univ Ave, Riverside, CA 92521 USA Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Baden Wurttembu, Germany Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany UNC, CONICET, Inst Astron Teor & Expt, Laprida 854,X5000BGR, Cordoba, Argentina Univ Nacl Cordoba, Observ Astron, Laprida 854,X5000BGR, Cordoba, Argentina Peking Univ, Dept Astron, Beijing 100871, Peoples R China Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China Univ Bologna, Dept Phys & Astron Augusto Righi, I-40129 Bologna, Italy Univ Illinois, Sch Informat Sci, 501 E Daniel St, Champaign, IL 61820 USA Univ Florida, Dept Astron, 211 Bryant Space Sci Ctr, Gainesville, FL 32611 USA MIT, Dept Phys, Cambridge, MA 02139 USA Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada Inst Theory & Computat, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA |
| Keywords | GENERATION VIRGO CLUSTER DARK-MATTER ILLUSTRISTNG SIMULATIONS COSMOLOGICAL SIMULATIONS FORMATION EFFICIENCIES QUENCHED FRACTIONS SPHERICAL GALAXIES STAR-FORMATION STELLAR HALOS LOCAL GROUP |
| Issue Date | 26-Nov-2022 |
| Publisher | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY |
| Abstract | We present a post-processing catalogue of globular clusters (GCs) for the 39 most massive groups and clusters in the TNG50 simulation of the Illlustris TNG project (virial masses M-200 = [5 x 10(12) -2 x 10(14)]M-circle dot). We tag GC particles to all galaxies with stellar mass M-* >= 5 x 10(6) M-circle dot, and we calibrate their masses to reproduce the observed power-law relation between GC mass and halo mass for galaxies with M-200 >= 10(11) M-circle dot (corresponding to M-* similar to 10(9) M-circle dot). Here, we explore whether an extrapolation of this M-GC-M-200 relation to lower mass dwarfs is consistent with current observations. We find a good agreement between our predicted number and specific frequency of GCs in dwarfs with M-* = [5 x 10(6) -10(9)] M-circle dot and observations. Moreover, we predict a steep decline in the GC occupation fraction for dwarfs with M-* < 10(9) M-circle dot that agrees well with current observational constraints. This declining occupation fraction is due to a combination of tidal stripping in all dwarfs plus a stochastic sampling of the GC mass function for dwarfs with M-* < 10(7.5) M-circle dot. Our simulations also reproduce available constraints on the abundance of intracluster GCs in Virgo and Centaurus A. These successes provide support to the hypothesis that the M-GC-M-200 relation holds, albeit with more scatter, all the way down to the regime of classical dwarf spheroidals in these environments. Our GC catalogues are publicly available as part of the IllustrisTNG data release. |
| URI | http://hdl.handle.net/20.500.11897/667621 |
| ISSN | 0035-8711 |
| DOI | 10.1093/mnras/stac2818 |
| Indexed | SCI(E) |
| Appears in Collections: | 物理学院 科维理天文与天体物理研究所 |
