Transonic galactic outflows in a dark matter halo with a central black hole and its application to the Sombrero galaxy

TL;DR

This paper classifies transonic galactic outflows influenced by dark matter halos and black holes, revealing new solution types and applying them to the Sombrero galaxy to explain observed gas density profiles.

Contribution

It introduces a new class of transonic solutions near black holes and demonstrates their relevance to galaxy outflows, especially in quiescent galaxies like the Sombrero galaxy.

Findings

Black hole gravity creates a new transonic solution branch.

A slowly accelerating outflow can mimic hydrostatic gas density profiles.

The model explains observed gas distributions without active star formation.

Abstract

We have classified possible transonic solutions of galactic outflows in the gravitational potential of the dark matter halo (DMH) and super massive black hole (SMBH) under the assumptions of isothermal, spherically symmetric and steady state. It is clarified that the gravity of SMBH adds a new branch of transonic solutions with the transonic point in very close proximity to the centre in addition to the outer transonic point generated by the gravity of DMH. Because these two transonic solutions have substantially different mass fluxes and starting points, these solutions may have different influences on the evolution of galaxies and the release of metals into intergalactic space. We have applied our model to the Sombrero galaxy and obtained a new type of galactic outflow: a slowly accelerated transonic outflow through the transonic point at very distant region ($\simeq 126$\ kpc). In this galaxy, previous works reported that although the trace of the galactic outflow is observed by X-ray, the gas density distribution is consistent with the hydrostatic state. We have clarified that the slowly accelerating outflow has a gas density profile quite similar to that of the hydrostatic solution in the widely spread subsonic region. Thus, the slowly accelerating transonic solution cannot be distinguished from the hydrostatic solution in the observed region ($\leq 25$\ kpc) even if slow transonic flow exists. Our model provides a new perspective of galactic outflows and is applicable even to quiescent galaxies with inactive star formation.