Intergalactic-Absorption Confounding Circumgalactic Observations

TL;DR

This paper proposes that a significant portion of warm-ion absorption observed around galaxies may originate from the intergalactic medium rather than the circumgalactic medium, impacting the interpretation of such observations.

Contribution

It introduces a simple spherical collapse model to quantify IGM contributions to warm-ion columns, challenging previous assumptions that mainly attributed these to the CGM.

Findings

IGM can produce over 75% of O VI columns in massive halos.

The model reproduces observed O VI trends with impact parameter and halo mass.

IGM envelopes may dominate warm-ion absorption, complicating CGM analysis.

Abstract

The origin of warm ions in the circum-galactic medium (CGM) surrounding massive galaxies remains a mystery. In this paper, we argue that a significant fraction of the observed warm-ion columns may arise in the intergalactic medium (IGM) surrounding galactic halos. We use a simple spherical collapse model of the dark matter (DM) halos and their baryonic content to compute the evolving ion fractions within and outside virial halos. We show that the photoionized IGM may produce a thick blanket of warm ions around the CGM, thereby contaminating CGM observations. We find that the IGM contributes $> 75\%$ of the total \ion{O}{6} column densities in halos with virial masses exceeding a few times $10^{11}~M_\odot$, and that it may dominate the \ion{O}{6} absorption even for lower mass-halos, depending on the impact parameter. We compare our results with observations and find that our simplified model reproduces the overall \ion{O}{6} columns as well as their trend with the impact parameter and halo mass. We show that observed warm ion columns may be completely dominated by the IGM envelopes, consistent with CGM$^2$ data. We, therefore, suggest that theoretical interpretations of CGM-survey observations must consider the possible contribution of the surrounding IGM. Although our simplified model suggests that it may be possible to kinematically distinguish between CGM and IGM origins through the absorption line profiles, this distinction is likely unfeasible in realistic astrophysical halos, due to the complex velocity structure in the multi-phased CGM.