Aims: We present a uniform catalog of the images and radial profiles of the
temperature, abundance, and brightness for 70 clusters of galaxies observed by
XMM-Newton.
  Methods: We use a new "first principles" approach to the modeling and removal
of the background components; the quiescent particle background, the cosmic
diffuse emission, the soft proton contamination, and the solar wind charge
exchange emission. Each of the background components demonstrate significant
spectral variability, several have spatial distributions that are not described
by the photon vignetting function, and all except for the cosmic diffuse
emission are temporally variable. Because these backgrounds strongly affect the
analysis of low surface brightness objects, we provide a detailed description
our methods of identification, characterization, and removal.
  Results: We have applied these methods to a large collection of XMM-Newton
observations of clusters of galaxies and present the resulting catalog. We find
significant systematic differences between the Chandra and XMM-Newton
temperatures.Comment: Accepted for publication in A&A, 55 pages with 42 figure

Davis, D. S.

Kuntz, K. D.

Mushotzky, R. M.

Snowden, S. L.

English

arXiv

Aims.We present a uniform catalog of the images and radial profiles of the temperature,
abundance, and brightness for 70 clusters of galaxies observed by XMM-Newton.
        Methods.We use a new “first principles” approach to the modeling and removal
of the background components; the quiescent particle background,
the cosmic diffuse emission, the soft proton contamination, 
and the solar wind charge exchange emission.
Each of the background components demonstrate significant spectral variability,
several have spatial distributions that are not described 
by the photon vignetting function,
and all except for the cosmic diffuse emission are temporally variable.
Because these backgrounds strongly affect the analysis of low surface brightness objects,
we provide a detailed description our methods of identification, characterization,
and removal.
        Results.We have applied these methods to a large collection of XMM-Newton observations
of clusters of galaxies and present the resulting catalog.
We find significant systematic differences 
between the Chandra and XMM-Newton temperatures

S. L. Snowden

R. F. Mushotzky

K. D. Kuntz

D. S. Davis

EDP Sciences OAI-PMH repository (1.2.0)

A catalog of galaxy clusters observed by XMM-Newton

Images and the radial profiles of the temperature, abundance, and brightness for 70 clusters of galaxies observed by XMM-Newton are presented along with a detailed discussion of the data reduction and analysis methods, including background modeling, which were used in the processing. Proper consideration of the various background components is vital to extend the reliable determination of cluster parameters to the largest possible cluster radii. The various components of the background including the quiescent particle background, cosmic diffuse emission, soft proton contamination, and solar wind charge exchange emission are discussed along with suggested means of their identification, filtering, and/or their modeling and subtraction. Every component is spectrally variable, sometimes significantly so, and all components except the cosmic background are temporally variable as well. The distributions of the events over the FOV vary between the components, and some distributions vary with energy. The scientific results from observations of low surface brightness objects and the diffuse background itself can be strongly affected by these background components and therefore great care should be taken in their consideration

Davis, David S.

NASA Technical Reports Server

A Catalog of Galaxy Clusters Observed by XMM-Newton

A Catalog of Galaxy Clusters Observed by XMM-Newton

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EDP Sciences OAI-PMH repository (1.2.0)

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