@article{753fb222aa22475eb5aa5f42216c7dd2,
title = "The GOGREEN survey: Internal dynamics of clusters of galaxies at redshift 0.9-1.4",
abstract = "Context. The study of galaxy cluster mass profiles (M(r)) provides constraints on the nature of dark matter and on physical processes affecting the mass distribution. The study of galaxy cluster velocity anisotropy profiles (β(r)) informs the orbits of galaxies in clusters, which are related to their evolution. The combination of mass profiles and velocity anisotropy profiles allows us to determine the pseudo phase-space density profiles (Q(r)); numerical simulations predict that these profiles follow a simple power law in cluster-centric distance. Aims. We determine the mass, velocity anisotropy, and pseudo phase-space density profiles of clusters of galaxies at the highest redshifts investigated in detail to date. Methods. We exploited the combination of the GOGREEN and GCLASS spectroscopic data-sets for 14 clusters with mass M200 ≥ 1014 M⊙ at redshifts 0.9 ≤ z ≤ 1.4. We constructed an ensemble cluster by stacking 581 spectroscopically identified cluster members with stellar mass M∗ ≥ 109.5 M⊙. We used the MAMPOSSt method to constrain several M(r) and β(r) models, and we then inverted the Jeans equation to determine the ensemble cluster β(r) in a non-parametric way. Finally, we combined the results of the M(r) and β(r) analysis to determine Q(r) for the ensemble cluster. Results. The concentration c200 of the ensemble cluster mass profile is in excellent agreement with predictions from Λ cold dark matter (ΛCDM) cosmological numerical simulations, and with previous determinations for clusters of similar mass and at similar redshifts, obtained from gravitational lensing and X-ray data. We see no significant difference between the total mass density and either the galaxy number density distributions or the stellar mass distribution. Star-forming galaxies are spatially significantly less concentrated than quiescent galaxies. The orbits of cluster galaxies are isotropic near the center and more radial outside. Star-forming galaxies and galaxies of low stellar mass tend to move on more radially elongated orbits than quiescent galaxies and galaxies of high stellar mass. The profile Q(r), determined using either the total mass or the number density profile, is very close to the power-law behavior predicted by numerical simulations. Conclusions. The internal dynamics of clusters at the highest redshift probed in detail to date are very similar to those of lower-redshift clusters, and in excellent agreement with predictions of numerical simulations. The clusters in our sample have already reached a high degree of dynamical relaxation.",
keywords = "Cosmology: observations, Galaxies: clusters: general, Galaxies: evolution",
author = "A. Biviano and {Van Der Burg}, {R. F.J.} and Balogh, {M. L.} and E. Munari and Cooper, {M. C.} and {De Lucia}, G. and R. Demarco and P. Jablonka and A. Muzzin and J. Nantais and Old, {L. J.} and G. Rudnick and B. Vulcani and G. Wilson and Yee, {H. K.C.} and D. Zaritsky and P. Cerulo and J. Chan and A. Finoguenov and D. Gilbank and C. Lidman and I. Pintos-Castro and H. Shipley",
note = "Funding Information: Acknowledgements. This work was enabled by observations made from the Gemini North, Subaru and CFHT telescopes, located within the Maunakea Science Reserve and adjacent to the summit of Maunakea. We are grateful for the privilege of observing the Universe from a place that is unique in both its astronomical quality and its cultural significance. We thank the referee for her/his useful comments that helped improving the scientific content of this paper. RD gratefully acknowledges support from the Chilean Centro de Exce-lencia en Astrof{\'i}sica y Tecnolog{\'i}as Afines (CATA) BASAL grant AFB-170002. JN received support from Universidad Andr{\'e}s Bello research grant DI-12-19/R. LJO acknowledges the support of a European Space Agency (ESA) Research Fellowship. GR acknowledges support from the National Science Foundation grants AST-1517815, AST-1716690, and AST-1814159 and NASA HST grant AR-14310. GR also acknowledges the support of an ESO visiting science fellowship. BV acknowledges financial contribution from the grant PRIN MIUR 2017 n.20173ML3WW_001 (PI Cimatti) and from the INAF main-stream funding programme (PI Vulcani). MLB acknowledges support from the National Science and Engineering Research Council (NSERC) Discovery Grant program. GW gratefully acknowledges support from the National Science Foundation through grant AST-1517863, from HST program number GO-15294, and from grant number 80NSSC17K0019 issued through the NASA Astrophysics Data Analysis Program (ADAP). Support for program number GO-15294 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. We thank the International Space Science Institute (ISSI) for providing financial support and a meeting facility that inspired insightful discussions for team “COSWEB: The Cosmic Web and Galaxy Evolution”. The Millennium Simulations databases used in this paper and the web application providing online access to them were constructed as part of the activities of the German Astrophysical Virtual Observatory. For this work we made use of the softwares Numpy (Harris et al. 2020) and Scipy (Virtanen et al. 2020). Funding Information: This work was enabled by observations made from the Gemini North, Subaru and CFHT telescopes, located within the Maunakea Science Reserve and adjacent to the summit of Maunakea. We are grateful for the privilege of observing the Universe from a place that is unique in both its astronomical quality and its cultural significance. We thank the referee for her/his useful comments that helped improving the scientific content of this paper. RD gratefully acknowledges support from the Chilean Centro de Excelencia en Astrof?sica y Tecnolog?as Afines (CATA) BASAL grant AFB-170002. JN received support from Universidad Andr?s Bello research grant DI-12-19/R. LJO acknowledges the support of a European Space Agency (ESA) Research Fellowship. GR acknowledges support from the National Science Foundation grants AST-1517815, AST-1716690, and AST-1814159 and NASA HST grant AR-14310. GR also acknowledges the support of an ESO visiting science fellowship. BV acknowledges financial contribution from the grant PRIN MIUR 2017 n.20173ML3WW-001 (PI Cimatti) and from the INAF main-stream funding programme (PI Vulcani). MLB acknowledges support from the National Science and Engineering Research Council (NSERC) Discovery Grant program. GW gratefully acknowledges support from the National Science Foundation through grant AST-1517863, from HST program number GO-15294, and from grant number 80NSSC17K0019 issued through the NASA Astrophysics Data Analysis Program (ADAP). Support for program number GO-15294 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. We thank the International Space Science Institute (ISSI) for providing financial support and a meeting facility that inspired insightful discussions for team {"}COSWEB: The Cosmic Web and Galaxy Evolution{"}. The Millennium Simulations databases used in this paper and the web application providing online access to them were constructed as part of the activities of the German Astrophysical Virtual Observatory. For this work we made use of the softwares Numpy (Harris et al. 2020) and Scipy (Virtanen et al. 2020). Publisher Copyright: {\textcopyright} 2021 ESO.",
year = "2021",
month = jun,
day = "1",
doi = "10.1051/0004-6361/202140564",
language = "English (US)",
volume = "650",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
}