The Surprisingly Constant Strength of O VI Absorbers over Cosmic Time

TL;DR

This study compiles and analyzes 775 high-resolution O VI absorbers across cosmic time, revealing a surprising constancy in their strength and supporting a cooling-flow origin over other models.

Contribution

It provides a comprehensive dataset of O VI absorbers from z=0 to 3 and demonstrates their invariant properties, challenging the photoionization model for intergalactic O VI.

Findings

O VI column density is insensitive to metallicity in galactic environments.

Intergalactic O VI components show weak evolution in column density from z=0.2 to 2.3.

IGM O VI line widths are broader at lower redshift, supporting a cooling-flow origin.

Abstract

O VI absorption is observed in a wide range of astrophysical environments, including the Local ISM, the disk and halo of the Milky Way, high-velocity clouds, the Magellanic clouds, starburst galaxies, the intergalactic medium, damped Lyman-alpha systems, and gamma-ray-burst host galaxies. Here a new compilation of 775 O VI absorbers drawn from the literature is presented, all observed at high resolution (instrumental FWHM<20 km/s) and covering the redshift range z=0-3. In galactic environments [log N(H I)>20], the mean O VI column density is shown to be insensitive to metallicity, taking a value log N(O VI)~14.5 for galaxies covering the range -1.6<[O/H]<0. In intergalactic environments [log N(H I)<17], the mean O VI component column density measured in datasets of similar sensitivity shows only weak evolution between z=0.2 and z=2.3, but IGM O VI components are on average almost twice as broad at z=0.2 than at z=2.3. The existence of a characteristic value of log N(O VI) for galactic O VI absorbers, and the lack of evolution in log N(O VI) for intergalactic absorbers, lend support to the ``cooling-flow' model of Heckman et al. (2002), in which all O VI absorbers are created in regions of initially-hot shock-heated plasma that are radiatively cooling through coronal temperatures. These regions could take several forms, including conductive, turbulent, or shocked boundary layers between warm (~10^4 K) clouds and hot (~10^6 K) plasma, although many such regions would have to be intersected by a typical galaxy-halo sightline to build up the characteristic galactic N(O VI). The alternative, widely-used model of single-phase photoionization for intergalactic O VI is ruled out by kinematic evidence in the majority of IGM O VI components at low and high redshift.