400d cluster survey

Main papers

Paper I:  --- catalog of distant objects, ROSAT detection, and survey area calibration
Paper II:  --- Chandra observations of complete samples at low and high z, discussion of cluster mass function derivation and systematics. A measurement of the evolving M-L relation
Paper III:  --- Cosmological constraints --- dark energy equation of state, neutrino mass, and sigma8

400d catalog papers

Burenin et al. 2007:  "400 square degrees ROSAT  PSPC galaxy cluster survey: Catalog and statistical calibration". (astro-ph/0610739)
Description of the 400d cluster list and statistical calibration of the catalog. Cluster log N – log S and evolving X-ray luminosity function. For description of the X-ray detection algorithm, see Vikhlinin et al. (1998).

Cluster mass estimates

Vikhlinin et al. 2006:  "Chandra Sample of Nearby Relaxed Galaxy Clusters: Mass, Gas Fraction, and Mass-Temperature Relation".
Hydrostatic total mass estimates in a sample of well-observed, low-z relaxed clusters. This work is a foundation of our calibration of scaling relations between total mass and X-ray observables.
Kotov & Vikhlinin 2006:  "Chandra Sample of Galaxy Clusters at z = 0.4-0.55: Evolution in the Mass-Temperature Relation".
Similar work, using a sample of high-z clusters.
Kravtsov, Vikhlinin & Nagai 2006:  "A New Robust Low-Scatter X-Ray Mass Indicator for Clusters of Galaxies".
Analysis of X-ray observables which can be used as high-quality total mass estimators. The YX parameter.
Nagai, Vikhlinin & Kravtsov 2007:  "Testing X-Ray Measurements of Galaxy Clusters with Cosmological Simulations".
This work uses mock Chandra data made from the output of cosmological simulations to test how accurately the cluster parameters are recovered in the X-ray analysis
Nagai, Kravtsov & Vikhlinin 2007:  "Effects of Galaxy Formation on Thermodynamics of the Intracluster Medium".
Comparison of gas temperature, density, pressure, and entropy profiles and scalings in the simulated clusters and in the Chandra sample of V06. The main conclusion is that the X-ray properties of ART-simulated clusters match very well the observations except for the innermost regions.

X-ray properties of high-redshift clusters

Vikhlinin et al. 2006:  "Lack of 'cooling flow' clusters at z>0.5". (astro-ph/0611438)
Analysis of Chandra images of the high-redshift 400d clusters shows a smaller fraction of objects with the peaked X-ray surface brightness profiles compared to the low-redshift population.

See also the 160d survey papers