We determine the relation between the Comptonization parameter predicted using X-ray data $Y_{ C,Xray}$ and the X-ray luminosity $L_X$, both magnitudes derived from ROSAT data, with the Comptonization parameter $Y_{ C,SZ}$ measured on { \it Planck} 2013 foreground cleaned Nominal maps. The 560 clusters of our sample includes clusters with masses $M\ge 10^{ 13}M_\odot$, 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 $z\le 0.3$. The prediction of the $\beta=2/3$ model convolved with the Planck antenna beam agrees with the anisotropies measured in foreground cleaned Planck Nominal maps within the X-ray emitting region, confirming the results of an earlier analysis (Atrio-Barandela et al. 2008). The universal pressure profile overestimates the signal by a 15-21\% depending on the angular aperture. We show that the discrepancy is not due to the presence of { \it cool-core} systems but it is an indication of a brake in the $L_X-M$ relation towards low mass systems. We show that relation of the Comptonization parameter averaged over the region that emits 99\% of the X-ray flux and and the X-ray luminosity is consistent with the predictions of the self-similar model. We confirm previous findings that the scaling relations studied here do not evolve with redshift within the range probed by our catalog.
Categories: astro-ph.CO