A Catalog of Galaxy Clusters Observed by XMM-Newton

By S. Snowden, R. Mushotzky, K. Kuntz, D. Davis. 2007

293 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/489d158db2d6d2e41dcdd608619aa39ff744604b

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Citations in the corpus

The EPIC-MOS particle-induced background spectra (2008, methodology): “…it poses a particular problem in the outer parts of the FOV where, for example, cluster emission is particularly interesting, and particularly weak (Snowden et al. 2008) In our effort to characterize the quiescent background, we made the discovery that the soft proton contamination is strongest…”
INNOVATIONS IN THE ANALYSIS OF CHANDRA-ACIS OBSERVATIONS (2010, background): “Alternatively, if no suitable “sky” region is available, then the astrophysical background must be directly modeled (Snowden et al. 2008).”
NuSTAR OBSERVATIONS OF THE BULLET CLUSTER: CONSTRAINTS ON INVERSE COMPTON EMISSION (2014, methodology): “…their location in the detector plane, and create an XSPEC-readable script that sets up and fits for all observation-specific component normalizations, much in the spirit of the background treatment in the XMM-Newton Extended Source Analysis Software package (as introduced in Snowden et al. 2008).”
DETECTION OF AN UNIDENTIFIED EMISSION LINE IN THE STACKED X-RAY SPECTRUM OF GALAXY CLUSTERS (2014, methodology): “However after the filtering some soft-proton residuals may remain in the data and were modeled by including an extra power law model component and diagonal response matrices provided in the SAS distribution in the final spectral analysis (Snowden et al. 2008).”
Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters (2009, background): “High quality data from the current generation of X–ray satellites (XMM-Newton, Chandra and Suzaku) have now established a number of observational facts concerning the thermo-dynamical and chemo-dynamical properties of the intra-cluster medium (ICM) for statistically representative sets of galaxy clu”
Total mass biases in X-ray galaxy clusters (2008, background): “…the largest accessible radius and r500 typically being the largest distance where the ICM temperature can be reliably estimated through X-ray observations (e.g. De Grandi & Molendi 2002; Piffaretti et al. 2005; Vikhlinin et al. 2005; Pratt et al. 2007; Snowden et al. 2008; Leccardi & Molendi 2008).”
CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS (2008, methodology): “The Chandra exposure is short but the best-fit values of our temperature profile agree well with the XMM-Newton results by Snowden et al. (2008).”
X-ray spectroscopy of the Virgo Cluster out to the virial radius (2011, methodology): “The filtering and extraction of the MOS data products and the subtraction of their instrumental background was performed using the XMM-Newton Extended Source Analysis Software (XMM-ESAS) and methods described in Kuntz & Snowden (2008); Snowden et al. (2008); Snowden & Kuntz (2010).”
Radial temperature profiles for a large sample of galaxy clusters observed with XMM-Newton (2008, result): “Recent observations with current experiments (i.e.XMM-Newton and Chandra) have clearly shown that cluster temperature profiles decline beyond the 15-20% of R180 (Piffaretti et al. 2005; Vikhlinin et al. 2005; Pratt et al. 2007; Snowden et al. 2008).”
JOINT ANALYSIS OF CLUSTER OBSERVATIONS. II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES (2012, background): “Typically, comparisons show that Chandra temperatures are 5%–15% higher (Snowden et al. 2008; Reese et al. 2010).”
GALAXY CLUSTER BARYON FRACTIONS REVISITED (2013, methodology): “The fit model and method used for the spectral fitting is outlined in Snowden et al. (2008) and is identical to the one described in our previous work (Sivanandam et al. 2009).”
Scaling Properties of a Complete X-ray Selected Galaxy Group Sample (2014, methodology): “All these different components exhibit different spectral and temporal characteristics (e.g., Lumb et al. 2002; Read & Ponman 2003; Kuntz & Snowden 2008; Snowden et al. 2008).”