TY - JOUR
T1 - The Next Generation Virgo Cluster Survey (NGVS). XXXI. the Kinematics of Intracluster Globular Clusters in the Core of the Virgo Cluster
AU - Longobardi, Alessia
AU - Peng, Eric W.
AU - Côté, Patrick
AU - Mihos, J. Christopher
AU - Ferrarese, Laura
AU - Puzia, Thomas H.
AU - Lançon, Ariane
AU - Zhang, Hong Xin
AU - Muñoz, Roberto P.
AU - Blakeslee, John P.
AU - Guhathakurta, Puragra
AU - Durrell, Patrick R.
AU - Sánchez-Janssen, Rúben
AU - Toloba, Elisa
AU - Jordán, Andrés
AU - Eyheramendy, Susana
AU - Cuillandre, Jean Charles
AU - Gwyn, Stephen D.J.
AU - Boselli, Alessandro
AU - Duc, Pierre Alain
AU - Liu, Chengze
AU - Alamo-Martínez, Karla
AU - Powalka, Mathieu
AU - Lim, Sungsoon
N1 - Funding Information:
A.L. is thankful to E. Emsellem and L. Sales for constructive and useful discussion on the analysis and interpretation of the data. E.W.P. and S.L. acknowledge support from the National Natural Science Foundation of China through grant 11573002. E.W.P. also acknowledges travel support from the Chinese Academy of Sciences South America Center for Astronomy (CASSACA) that was essential for developing the photometric classification techniques used in this paper. S.E. and A.J. acknowledge support from project IC120009 “Millennium Institute of Astrophysics (MAS)” of the Millennium Science Initiative, Chilean Ministry of Economy. A.J. acknowledges additional support from project BASAL CATA PFB-06. T.H.P. acknowledges support through the FONDECYT Regular Project 1161817 and the BASAL Center for Astrophysics and Associated Technologies (PFB-06). T.H.P. and A.L. acknowledge ECOS-Sud/CONICYT project C15U02. H.-X.Z. acknowledges support from the CAS Pioneer Hundred Talents Program. C.L. acknowledges the NSFC grants 11673017, 11203017, and 11433002. C.L. is supported by the Key Laboratory for Particle Physics, Astrophysics and Cosmology, Ministry of Education. This paper is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. MMT telescope time was granted, in part, by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. Data presented in this paper were obtained at the Anglo-Australian Telescope, which is operated by the Australian Astronomical Observatory. Data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The observatory was made possible by the generous financial support of the W.M. Keck Foundation. This research made use of Astropy (http://www.astropy.org), a community-developed core Python package for astronomy.
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.
PY - 2018/9/1
Y1 - 2018/9/1
N2 - Intracluster (IC) populations are expected to be a natural result of the hierarchical assembly of clusters, yet their low space densities make them difficult to detect and study. We present the first definitive kinematic detection of an IC population of globular clusters (GCs) in the Virgo cluster, around the central galaxy M87. This study focuses on the Virgo core, for which the combination of Next Generation Virgo Cluster Survey photometry and follow-up spectroscopy allows us to reject foreground star contamination and explore GC kinematics over the full Virgo dynamical range. The GC kinematics changes gradually with galactocentric distance, decreasing in mean velocity and increasing in velocity dispersion, eventually becoming indistinguishable from the kinematics of Virgo dwarf galaxies at R > 320 kpc. By kinematically tagging M87 halo and intracluster GCs, we find that (1) the M87 halo has a smaller fraction (52 ± 3%) of blue clusters with respect to the IC counterpart (77 ± 10%), (2) the (g′-r′)0 versus (i′-z′)0 color-color diagrams reveal a galaxy population that is redder than the IC population, which may be due to a different composition in chemical abundance and progenitor mass, and (3) the ICGC distribution is shallower and more extended than the M87 GCs, yet still centrally concentrated. The ICGC specific frequency, S N,ICL = 10.2 ± 4.8, is consistent with what is observed for the population of quenched, low-mass galaxies within 1 Mpc from the cluster's center. The IC population at Virgo's center is thus consistent with being an accreted component from low-mass galaxies tidally stripped or disrupted through interactions, with a total mass of.
AB - Intracluster (IC) populations are expected to be a natural result of the hierarchical assembly of clusters, yet their low space densities make them difficult to detect and study. We present the first definitive kinematic detection of an IC population of globular clusters (GCs) in the Virgo cluster, around the central galaxy M87. This study focuses on the Virgo core, for which the combination of Next Generation Virgo Cluster Survey photometry and follow-up spectroscopy allows us to reject foreground star contamination and explore GC kinematics over the full Virgo dynamical range. The GC kinematics changes gradually with galactocentric distance, decreasing in mean velocity and increasing in velocity dispersion, eventually becoming indistinguishable from the kinematics of Virgo dwarf galaxies at R > 320 kpc. By kinematically tagging M87 halo and intracluster GCs, we find that (1) the M87 halo has a smaller fraction (52 ± 3%) of blue clusters with respect to the IC counterpart (77 ± 10%), (2) the (g′-r′)0 versus (i′-z′)0 color-color diagrams reveal a galaxy population that is redder than the IC population, which may be due to a different composition in chemical abundance and progenitor mass, and (3) the ICGC distribution is shallower and more extended than the M87 GCs, yet still centrally concentrated. The ICGC specific frequency, S N,ICL = 10.2 ± 4.8, is consistent with what is observed for the population of quenched, low-mass galaxies within 1 Mpc from the cluster's center. The IC population at Virgo's center is thus consistent with being an accreted component from low-mass galaxies tidally stripped or disrupted through interactions, with a total mass of.
KW - galaxies: clusters: individual (Virgo)
KW - galaxies: individual (M87)
KW - galaxies: kinematics and dynamics
KW - galaxies: star clusters: general
KW - globular clusters: general
UR - http://www.scopus.com/inward/record.url?scp=85053131459&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/aad3d2
DO - 10.3847/1538-4357/aad3d2
M3 - Article
AN - SCOPUS:85053131459
SN - 0004-637X
VL - 864
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 36
ER -