The Structure of the Circumgalactic Medium of Galaxies: Cool Accretion Inflow Around NGC 1097

TL;DR

This study uses Hubble Space Telescope UV spectra of four sightlines passing through NGC 1097's halo to analyze the distribution, kinematics, and composition of circumgalactic gas, revealing infalling gas and a disk-like structure.

Contribution

It provides detailed observational evidence of the gas distribution and kinematics in a typical galaxy halo, highlighting infall and potential outflows in the circumgalactic medium.

Findings

Detection of Lyman-alpha absorption along all sightlines.

Identification of metal lines mainly in inner sightlines.

Gas distribution consistent with a rotating, infalling disk-like structure.

Abstract

We present Hubble Space Telescope far-UV spectra of 4 QSOs whose sightlines pass through the halo of NGC 1097 at impact parameters of 48 -165 kpc. NGC 1097 is a nearby spiral galaxy that has undergone at least two minor merger events, but no apparent major mergers, and is relatively isolated with respect to other nearby bright galaxies. This makes NGC 1097 a good case study for exploring baryons in a paradigmatic bright-galaxy halo. Lyman-alpha absorption is detected along all sightlines and Si III 1206 is found along the 3 smallest impact parameter sightlines; metal lines of C II, Si II and Si IV are only found with certainty towards the inner-most sightline. The kinematics of the absorption lines are best replicated by a model with a disk-like distribution of gas approximately planar to the observed 21 cm H I disk, that is rotating more slowly than the inner disk, and into which gas is infalling from the intergalactic medium. Some part of the absorption towards the inner-most sightline may arise either from a small-scale outflow, or from tidal debris associated with the minor merger that gives rise to the well known `dog-leg' stellar stream that projects from NGC 1097. When compared to other studies, NGC 1097 appears to be a `typical' absorber, although the large dispersion in absorption line column density and equivalent width in a single halo goes perhaps some way in explaining the wide range of these values seen in higher-redshift studies.