Planck Intermediate Results. I. Further validation of new Planck clusters with XMM-Newton

TL;DR

This paper validates new Planck-detected galaxy clusters using XMM-Newton X-ray observations, confirming their nature, redshifts, and properties, and discusses implications for cluster detection and scaling relations.

Contribution

It provides a detailed validation of Planck cluster candidates with X-ray follow-up, confirming their cluster status, redshifts, and analyzing their X-ray and SZ properties, including bias indications.

Findings

Ten of eleven candidates are confirmed as clusters.

Clusters are found at redshifts 0.19 to 0.94.

Most clusters are X-ray underluminous for their mass.

Abstract

We present further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5<S/N<5.3 in the same 10-month survey maps used in the construction of the Early SZ sample. The sample was selected in order to test internal SZ quality flags, and the pertinence of these flags is discussed in light of the validation results. Ten of the candidates are found to be bona fide clusters lying below the RASS flux limit. Redshift estimates are available for all confirmed systems via X-ray Fe-line spectroscopy. They lie in the redshift range 0.19<z<0.94, demonstrating Planck's capability to detect clusters up to high z. The X-ray properties of the new clusters appear to be similar to previous new detections by Planck at lower z and higher SZ flux: the majority are X-ray underluminous for their mass, estimated using Y_X as mass proxy, and many have a disturbed morphology. We find tentative indication for Malmquist bias in the Y_SZ-Y_X relation, with a turnover at Y_SZ \sim 4 e-4 arcmin^2. We present additional new optical redshift determinations with ENO and ESO telescopes of candidates previously confirmed with XMM-Newton. The X-ray and optical redshifts for a total of 20 clusters are found to be in excellent agreement. We also show that useful lower limits can be put on cluster redshifts using X-ray data only via the use of the Y_X vs. Y_SZ and X-ray flux F_X vs. Y_SZ relations.