A precise understanding of the relations between observable X-ray properties of galaxy clusters and cluster mass is a vital part of the application of X-ray galaxy cluster surveys to test cosmological models. An understanding of how these relations evolve with redshift is just emerging from a number of observational data sets. 
The current literature provides a diverse and inhomogeneous picture of scaling relation evolution. We attempt to transform these results and the data on recently discovered distant clusters into an updated and consistent framework, and provide an overall view of scaling relation evolution. 
We study in particular the M-T, L_X-T, and M-L_X relation combining 14 published data sets supplemented with recently published data of distant clusters and new results from follow-up observations of the XMM-Newton Distant Cluster Project (XDCP). 
We find that the evolution of the M-T relation is consistent with the self-similar prediction, while the evolution of X-ray luminosity for a given temperature and mass for a given X-ray luminosity is slower than predicted. Our best fit results for the evolution factor E(z)^alpha are alpha = -1.04+-0.07 for the M-T relation, alpha = -0.23+0.12-0.62 for the L-T relation, and alpha = -0.93+0.62-0.12 for the M-L_X relation. We find that selection biases are the most likely reason for apparent inconsistencies between different published data sets. 
The new results provide the currently most robust calibration of high-redshift cluster mass estimates based on X-ray luminosity and temperature and help us to improve the prediction of the number of clusters to be found in future galaxy cluster X-ray surveys, such as eROSITA. The comparison of evolution results with hydrodynamical cosmological simulations suggests that early preheating of the intracluster medium provides the most suitable scenario to explain the observed evolution.

/pdf/observational-constraints-on-the-redshift-evolution-of-x-ray-ii0x2rfv7n.pdf

Observational constraints on the redshift evolution of X-ray scaling relations of galaxy clusters out to z ~ 1.5

We forecast the constraints on the values of s8, Om and cluster scaling-relation parameters which we expect to obtain from the XMM Cluster Survey (XCS). We assume a flat cold dark matter Universe and perform a Monte Carlo Markov Chain analysis of the evolution of the number density of galaxy clusters that takes into account a detailed simulated selection function. Comparing our current observed number of clusters shows good agreement with predictions. We determine the expected degradation of the constraints as a result of self-calibrating the luminositytemperature relation (with scatter), including temperature measurement errors, and relying on photometric methods for the estimation of galaxy cluster redshifts. We examine the effects of systematic errors in scaling relation and measurement error assumptions. Using only (T, z) self-calibration, we expect to measure Om to 0.03 (and O to the same accuracy assuming flatness), and s8 to 0.05, also constraining the normalization and slope of the luminositytemperature relation to 6 and 13 per cent (at 1s), respectively, in the process. Self-calibration fails to jointly constrain the scatter and redshift evolution of the luminositytemperature relation significantly. Additional archival and/or follow-up data will improve on this. We do not expect measurement errors or imperfect knowledge of their distribution to degrade constraints significantly. Scaling-relation systematics can easily lead to cosmological constraints 2s or more away from the fiducial model. Our treatment is the first exact treatment to this level of detail, and introduces a new `smoothed ML (Maximum Likelihood) estimate of expected constraints.

/pdf/the-xmm-cluster-survey-forecasting-cosmological-and-cluster-3683s0ruca.pdf

The XMM Cluster Survey: forecasting cosmological and cluster scaling-relation parameter constraints

Aip conf proc

The Soft X-ray Spectrometer (SXS) onboard the NeXT (New exploration X-ray Telescope) is an X-ray spectrometer
utilizing an X-ray microcalorimeter array. Combined with the soft X-ray telescope of 6 m focal length,
the instrument will have a ~ 290cm 2 effective at 6.7 keV. With the large effective area and the energy resolution
as good as 6 eV (FWHM), the instrument is very suited for the high-resolution spectroscopy of iron K emission
line. One of the major scientific objectives of SXS is to determine turbulent and/or macroscopic motions of the
hot gas in clusters of galaxies of up to z ~ 1. The instruments will use 6 × 6 or 8 × 8 format microcalorimeter
array which is similar to that of Suzaku XRS. The detector will be cooled to a cryogenic temperature of 50 mK
by multi-stage cooling system consisting of adiabatic demagnetization refrigerator, super fluid He, a 3He Joule
Thomson cooler, and double-stage stirling cycle cooler.

The x-ray microcalorimeter on the NeXT mission

Particles have tremendous potential as astronomical messengers, and conversely, studying the universe as a whole also teaches us about particle physics. This thesis encompasses both of these research directions. 
Many models predict a diffuse flux of high energy neutrinos from active galactic nuclei and other astrophysical sources. The "Astrophysics Underground" portion of this thesis describes a search for this neutrino flux performed by looking for very high energy upward-going muons using the Super-K detector. 
In addition to using particles to do astronomy, we can also use the universe itself as a particle physics lab. The "Particle Physics in the Sky" portion of this thesis focuses on extracting cosmological information from galaxy surveys. 
To overcome technical challenges faced by the latest galaxy surveys, we produced a comprehensive upgrade to mangle, a software package that processes the angular masks defining the survey area on the sky. We added dramatically faster algorithms and new useful features that are necessary for managing complex masks of current and next-generation galaxy surveys. 
With this software in hand, we utilized SDSS data to investigate the relation between galaxies and dark matter by studying relative bias, i.e., the relation between different types of galaxies. Separating galaxies by their luminosities and colors reveals a complicated picture: red galaxies are clustered more strongly than blue galaxies, with both the brightest and the faintest red galaxies showing the strongest clustering. Furthermore, red and blue galaxies tend to occupy different regions of space. In order to make precise measurements from the next generation of galaxy surveys, it will be essential to account for this complexity.

pdf/particle-physics-in-the-sky-and-astrophysics-underground-ld6hojca91.pdf

Particle Physics in the Sky and Astrophysics Underground: Connecting the Universe's Largest and Smallest Scales

The amount and nature of dark energy (DE) can be tightly constrained by measuring the spatial correlation features and evolution of a sample of ~ 100,000 galaxy clusters over the redshift range 0<z < 1.5. Such an X-ray survey will discover all collapsed structures with mass above 3.5e14 solar masss at redshifts z<2 (i.e. the full range where such objects are expected) in the high Galactic latitude sky. Above this mass threshold the tight correlations between X-ray observables and mass allow direct interpretation of the data. We describe the constraints on Dark Energy that can be inferred from such a survey, using powerful self-calibration techniques to relate the X-ray observables (luminosity and temperature) to the underlying mass.

An X-ray Galaxy Cluster Survey for Investigations of Dark Energy

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An X-ray Galaxy Cluster Survey for Investigations of Dark Energy