Compact massive objects in Virgo galaxies: the black hole population

TL;DR

This paper studies the distribution of massive black holes in Virgo galaxies, exploring how formation, ejection, and environmental factors influence their presence and scaling relations with host galaxies.

Contribution

It proposes a combined natural and nurture scenario explaining the observed MBH distribution and their scaling relations in Virgo galaxies.

Findings

MBHs are more common in massive galaxies (M>10^10 solar masses).

Lower mass galaxies tend to host star clusters rather than MBHs.

Environmental effects like tidal stripping influence MBH-host scaling relations.

Abstract

We investigate the distribution of massive black holes (MBHs) in the Virgo cluster. Observations suggest that AGN activity is widespread in massive galaxies (M>1e10 solar masses), while at lower galaxy masses star clusters are more abundant, which might imply a limited presence of central black holes in these galaxy-mass regimes. We explore if this possible threshold in MBH hosting, is linked to nature, nurture, or a mixture of both. The nature scenario arises naturally in hierarchical cosmologies, as MBH formation mechanisms typically are efficient in biased systems, which would later evolve into massive galaxies. Nurture, in the guise of MBH ejections following MBH mergers, provides an additional mechanism that is more effective for low mass, satellite galaxies. The combination of inefficient formation, and lower retention of MBHs, leads to the natural explanation of the distribution of compact massive ob jects in Virgo galaxies. If MBHs arrive to the correlation with the host mass and velocity dispersion during merger-triggered accretion episodes, sustained tidal stripping of the host galaxies creates a population of MBHs which lie above the expected scaling between the holes and their host mass, suggesting a possible environmental dependence.