An excess of low-mass X-ray binaries in the outer halo of NGC 4472

TL;DR

This study uses Chandra X-ray observations to analyze the distribution of low-mass X-ray binaries in NGC 4472's outer halo, revealing an excess at large radii and an anti-correlation with metallicity, suggesting complex binary evolution effects.

Contribution

First detailed analysis of LMXB distribution in NGC 4472's halo, highlighting an excess at large radii and a novel anti-correlation with metallicity.

Findings

Number of field LMXBs increases with galactocentric radius.

Many LMXBs could host black holes due to flux limits.

Anti-correlation between LMXB density and metallicity in the halo.

Abstract

We present new Chandra observations of the outer halo of the giant elliptical galaxy NGC 4472 (M49) in the Virgo Cluster. The data extend to 130 kpc (28'), and have a combined exposure time of 150 ks. After identifying optical counterparts using the Next Generation Virgo Cluster Survey to remove background active galactic nuclei and globular cluster (GC) sources, and correcting for completeness, we find that the number of field low-mass X-ray binaries (LMXBs) per unit stellar V-band light increases significantly with galactocentric radius. Because the flux limit of the complete sample corresponds to the Eddington limit for neutron stars in NGC 4472, many of the ~90 field LMXBs in this sample could host black holes. The excess of field LMXBs at large galactocentric radii may be partially caused by natal kicks on black holes and neutron stars in binary systems in the inner part of the galaxy. Furthermore, since the metallicity in the halo of NGC 4472 strongly decreases towards larger galactocentric radii, the number of field LMXBs per unit stellar mass is anti-correlated with metallicity, opposite to what is observed in GCs. Another way to explain the spatial distribution of field LMXBs is therefore a reversed metallicity effect, although we have not identified a mechanism to explain this in terms of stellar and binary evolution.