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Galaxy Clusters Scaling Relations
To reliably detect galaxy cluster in publicly available Planck data one needs to reduce the foreground contaminations such as primary CMB anisotropies, instrumental noise, CO emission, thermal dust emission and, pointed/extended infrared sources. As an example, in the figure below, there are shown the Planck Nominal and foreground cleaned patches centred at the position of A1656 (Coma cluster) at 100–545 GHz .
The relation between the X-ray luminosity derived from ROSAT data, and the SZ Comptonization parameter, measured on Planck 2013 foreground cleaned Nominal maps, has been constrained. The clusters of our sample include ~600 clusters with masses one order of magnitude smaller than those used by the Planck Collaboration in a similar analysis. It also contains eight times more clusters in the redshift interval z ≤ 0.3. We confirm previous findings that the scaling relations do not evolve with redshift within the range probed by our catalogue [1].
Bibliography:
I. de Martino, F. Atrio-Barandela, ’SZ/X-ray scaling relations using X-ray data and Planck Nominal maps’, 2016, Mon. Not. R. Astron. Soc., 461, 3222−3232
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