Contributors: Department of Astronomy, Yonsei University, 50 Yonsei-ro Seodaemun-gu, Seoul 03722, Republic of Korea; NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab); NRC Herzberg Astronomy and Astrophysics; Conseil National de Recherches Canada (CNRC); Department of Physics and Astronomy Shanghai; Shanghai Jiao Tong University Shanghai; Institute of Astrophysics, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile; Institute of Astronomy Cambridge; University of Cambridge UK (CAM); Observatoire astronomique de Strasbourg (ObAS); Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS); Department of Physics and Astronomy Riverside; University of California Riverside (UC Riverside); University of California (UC)-University of California (UC); Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)); Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité); Department of Physics, Astronomy, Geology and Environmental Sciences, Youngstown State University, One University Plaza, Youngstown, OH 44555, USA; European Southern Observatory (ESO); Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstraße 25/8, Innsbruck A-6020, Austria; Department of Astronomy, Case Western Reserve University, Cleveland, OH 44106, USA; EPFL Laboratoire d’astrophysique; Ecole Polytechnique Fédérale de Lausanne (EPFL); STFC UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK; Sejong Science,Programme de bourses de la Fondation nationale pour la recherche de Subvention coréenne (NRF) financée par le gouvernement coréen (MSIT; N° NRF-2021R1C1C2006790); Fondation nationale des sciences naturelles de Chine (NSFC, subventions nos 12173025, 11833005, 11933003), 111 projet (n° B20019); ANID/CONICYT , FONDECYT Projet de bourse postdoctorale n° 3200959; Fonds national suisse, subvention n° PZ00P2_202104; L'IRAF a été distribué par la National Optical Astronomy Observatoire, géré par l'Association des Universités de Recherche en Astronomie (AURA) sous un accord de coopération avec la National Science Foundation. Sur la base des observations obtenues avec MegaPrime/MegaCam, un projet conjoint du CFHT et du CEA/DAPNIA; Le Télescope France-Hawaï (CFHT), exploité par le Conseil national de recherches (CNRC) du Canada, l'Institut National des Sciences de l'Univers (INSU) du Centre National de la Recherche Scientifique (CNRS) de France et l'Université d'Hawaï.; Le télescope spatial Hubble NASA/ESA obtenu depuis l'espace Telescope Science Institute, qui est géré par l'Association des universités de recherche en astronomie, Inc., sous Contrat NASA NAS 5-26555. Ces observations sont associé au programme GO-9401.; ANR-19-CE31-0022,POPSYCLE,Synthèse de populations pour les amas stellaires et les galaxies -atteindre la précision des relevés spectrophotométriques modernes par une physique stellaire renouvelée(2019)
نبذة مختصرة : International audience ; We present an analysis of the spatial distribution of globular cluster (GC) systems of 118 nearby early-type galaxies in the Next Generation Virgo Cluster Survey and Mass Assembly of early-Type GaLAxies with their fine Structures survey programs, which both used MegaCam on the Canada-France-Hawaii Telescope. We describe the procedure used to select GC candidates and fit the spatial distributions of GCs to a two-dimensional Sérsic function, which provides effective radii (half number radii) and Sérsic indices, and estimate background contamination by adding a constant term to the Sérsic function. In cases where a neighboring galaxy affects the estimation of the GC spatial distribution in the target galaxy, we fit two two-dimensional Sérsic functions, simultaneously. We also investigate the color distributions of GCs in our sample by using Gaussian mixture modeling. For GC systems with bimodal color distributions, we divide the GCs into blue and red subgroups and fit their respective spatial distributions with Sérsic functions. Finally, we measure the total number of GCs based on our fitted Sérsic function, and calculate the GC specific frequency. Unified Astronomy Thesaurus concepts: Early-type galaxies (429); Virgo Cluster (1772); Globular star clusters (656); Field galaxies (533); Galaxy evolution (594) Materials only available in the online version of record: figure sets Introduction Globular clusters (GCs) have long been used as probes of galaxy formation and evolution. While studies of GCs belonging to individual galaxies have provided many insights into galaxy evolution, it is the systematic study of GCs in large surveys (e.g.
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