XMM-Newton follow-up of a sample of apparent low surface brightness galaxy groups detected in the ROSAT All-Sky Survey

TL;DR

This study uses XMM-Newton observations to investigate a potentially new class of galaxy groups with unusually flat X-ray surface brightness profiles, which may have been missed in previous surveys and could impact cosmological analyses.

Contribution

It provides the first detailed X-ray analysis of a subset of these flat-profile galaxy groups, revealing their complex, multi-group structures and challenging existing detection assumptions.

Findings

All three observed systems are composed of multiple groups.

Measured surface brightness profile slopes are flatter than the canonical value.

None of the groups exceeds the flux limit of previous catalogs.

Abstract

Galaxy cluster cosmology relies on complete and pure samples spanning a large range of masses and redshifts. In Xu et al. (2018) and Xu et al. (2022), we discovered an apparently new population of galaxy groups and clusters with, on average, flatter X-ray surface brightness profiles than known clusters; this cluster population was missed in previous cluster surveys. The discovery of such a new class of objects could have a significant impact on cosmological applications of galaxy clusters. In this work we use a subsample of these systems to assess whether they belong to a new population. We follow up three of these galaxy groups and clusters with high-quality XMM-Newton observations. We produce clean images and spectra and use them for model fitting. We also identify known galaxies, groups, or clusters in the field. The observations reveal that all three systems are composed of multiple groups each, either at the same or at different redshifts. In total, we characterize nine groups. We measure flat surface brightness profiles with slope parameter $\beta < 0.6$; i.e, less than the canonical $\beta = 2/3$. For the two main central groups, we even measure $\beta < 0.4$. When the fluxes for the three observations are split up across the nine identified groups, none of them exceeds the typical flux limit adopted in previous RASS cluster catalogs, $\approx 3 \times 10^{-12}\,\mathrm{erg s^{-1}cm^{-2}}$ in the 0.1$-$2.4 keV energy band. The observations reveal that groups with flat surface brightness profiles exist. Whether they form a new, separate population requires additional follow-up observations of further systems from the Xu et al. sample, given the complexity we have discovered. Such extended low surface brightness systems, as well as multiple systems and projection effects, need to be taken into account when determining selection functions of group and cluster samples.