On the discrepancy between the X-ray and UV absorption measurements of O vi in the local ISM

The total amount of OVI present in the interstellar medium (ISM) obtained via absorption measurements in UV and X-ray spectra is currently in disagreement, with the latter being significantly larger (by a factor of 10 or more) than the former. Previous works have proposed that the blend of the OVI Ka line (22.032 A) with the OII Kb-L12 line (22.04 A) could account for the stronger absorption observed in the X-ray spectra. Here we present a detailed study of the oxygen absorption in the local ISM, implementing our new model IGMabs, which includes photoabsorption cross-sections of highly ionized species of abundant elements as well as turbulence broadening. By analyzing high-resolution Chandra spectra of 13 low mass X-ray binaries (LMXBs) and 29 extragalactic sources, we have estimated the column densities of OI-OIII and from OVI-OVIII along multiple line-of-sights. We find that in most cases the OII Kb-L12 line accounts for < 30% of the total OVI Ka + OII Kb. We conclude that the amount of OII predicted by our model is still insufficient to explain the discrepancy between X-ray and UV measurements of OVI column densities.