CLASH-VLT: Constraints on the Dark Matter Equation of State from Accurate Measurements of Galaxy Cluster Mass Profiles

Autor(en)

Barbara Sartoris, Andrea Biviano, Piero Rosati, Stefano Borgani, Keiichi Umetsu, Matthias Bartelmann, Marisa Girardi, Claudio Grillo, Doron Lemze, Adi Zitrin, Italo Balestra, Amata Mercurio, Mario Nonino, Marc Postman, Nicole Czakon, Larry Bradley, Tom Broadhurst, Dan Coe, Elinor Medezinski, Peter Melchior, Massimo Meneghetti, Julian Merten, Marianna Annunziatella, Narciso Benitez, Oliver Czoske, Megan Donahue, Stefano Ettori, Holland Ford, Alexander Fritz, Dan Kelson, Anton Koekemoer, Ulrike Kuchner, Marco Lombardi, Christian Maier, Leonidas A. Moustakas, Emiliano Munari, Valentina Presotto, Marco Scodeggio, Stella Seitz, Paolo Tozzi, Wei Zheng, Bodo Ziegler

Abstrakt

A pressureless scenario for the dark matter (DM) fluid is a widely adopted hypothesis, despite the absence of direct observational evidence. According to general relativity, the total mass-energy content of a system shapes the gravitational potential well, but different test particles perceive this potential in different ways depending on their properties. Cluster galaxy velocities, being ≪c, depend solely on the gravitational potential, whereas photon trajectories reflect the contributions from the gravitational potential plus a relativistic-pressure term that depends on the cluster mass. We exploit this phenomenon to constrain the equation of state (EoS) parameter of the fluid, primarily DM, contained in galaxy clusters. We use complementary information provided by the kinematic and lensing mass profiles of the galaxy cluster MACS 1206.2-0847 at z = 0.44, as obtained in an extensive imaging and spectroscopic campaign within the Cluster Lensing And Supernova survey with Hubble. The unprecedented high quality of our data set and the properties of this cluster are well suited to determine the EoS parameter of the cluster fluid. Since baryons contribute at most 15% to the total mass in clusters and their pressure is negligible, the EoS parameter we derive describes the behavior of the DM fluid. We obtain the most stringent constraint on the DM EoS parameter to date, w = (p

_r+2 p

_t )/(3 c

²ρ) = 0.00 ± 0.15 (stat) ± 0.08 (syst), averaged over the radial range 0.5 Mpc ≤ r ≤ r

₂₀₀, where p

_r and p

_t are the radial and tangential pressure, and ρ is the density. We plan to further improve our constraint by applying the same procedure to all clusters from the ongoing Cluster Lensing And Supernova Survey with Hubble-Very Large Telescope program.

Organisation(en)

Institut für Astrophysik

Externe Organisation(en)

Università degli Studi di Trieste, Instituto Nazionale die Astrofisica (INAF), Instituto Nazionale di Fisica Nucleare, Universitá degli studi di Ferrara, National Taiwan University, Ludwig-Maximilians-Universität München, Universitätsklinikum Heidelberg, League of European Research Universities - LERU, Bispebjerg Hospital, University of Copenhagen, Johns Hopkins University, California Institute of Technology (Caltech), European Space Agency (ESA), Baltimore, University of the Basque Country, Ohio State University at Mansfield, National Aeronautics & Space Administration (NASA), Instituto Pirenaico de Ecología (CSIC), Instituto de Astrofísica de Andalucía, Michigan State University, Carnegie Institution for Science, Politecnico di Milano, Max-Planck-Gesellschaft

Journal

The Astrophysical journal Letters

Band

783

Anzahl der Seiten

5

ISSN

2041-8205

DOI

https://doi.org/10.1088/2041-8205/783/1/L11

Publikationsdatum

03-2014

Peer-reviewed

Ja

ÖFOS 2012

103003 Astronomie, 103004 Astrophysik

Schlagwörter

ASJC Scopus Sachgebiete

Astronomy and Astrophysics, Space and Planetary Science

Link zum Portal

https://ucrisportal.univie.ac.at/de/publications/bf42b88f-1aed-40eb-bab3-00fbfc1b09c3