400d survey: publications

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

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).

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 Y_X 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.

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.