Maqola

<i>CHANDRA</i>CLUSTER COSMOLOGY PROJECT. II. SAMPLES AND X-RAY DATA REDUCTION

A. VikhlininHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAR. BureninSpace Research Institute (IKI), Profsoyuznaya 84/32, Moscow, RussiaH. EbelingInstitute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USAW. FormanHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAA. HornstrupC. JonesHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAAndrey V. KravtsovDepartment of Astronomy and Astrophysics, Kavli Institute for Cosmological Physics, Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USAS. S. MurrayHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USADaisuke NagaiDepartment of Physics and Yale Center for Astronomy & Astrophysics, Yale University, New Haven, CT 06520, USAH. QuintanaDepartamento de Astronomia y Astrofisica, Pontificia Universidad Catolica de Chile, Casilla 306, Santiago, 22, ChileAlexey VoevodkinLos Alamos National Laboratory, Los Alamos, NM 87545, USA

2009en

ABI

Annotatsiya

We discuss the measurements of the galaxy cluster mass functions at z=~0.05 and z=~0.5 using high-quality Chandra observations of samples derived from the ROSAT PSPC All-Sky and 400deg^2 surveys. We provide a full reference for the data analysis procedures, present updated calibration of relations between the total cluster mass and its X-ray indicators (T_X, Mgas, and Y_X) based on a subsample of low-z relaxed clusters, and present a first measurement of the evolving L_X-Mtot relation (with Mtot estimated from Y_X) obtained from a well-defined statistically complete cluster sample and with appropriate corrections for the Malmquist bias applied. Finally, we present the derived cluster mass functions, estimate the systematic uncertainties in this measurement, and discuss the calculation of the likelihood function. We confidently measure the evolution in the cluster comoving number density at a fixed mass threshold, e.g., by a factor of 5.0 +- 1.2 at M_500=2.5e14 h^-1 Msun between z=0 and 0.5. This evolution reflects the growth of density perturbations and can be used for the cosmological constraints complementing those from the distance-redshift relation.

Hali tarjima qilinmagan

Identifikatorlar

DOI: 10.1088/0004-637x/692/2/1033

Iqtiboslar va manbalar

2 ta iqtibos0 ta foydalanilgan manba

Koʻrsatkichlar — AkademScholar