English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We have identified a broad absorption line (BAL) outflow in the HST/STISspectrum of the quasar QSO B0254-3327B at velocity $v=-3200\text{ kms$^{-1}$}$. The outflow has absorption troughs from ions such as Ne VIII, NaIX, Si XII, and Ne V. We also report the first detection of S XIV absorptiontroughs, implying very high ionization. Via measurement of the ionic columndensities, photoionization analysis, and determination of the electron numberdensity of the outflow, we found the kinetic luminosity of the outflow systemto be up to $\sim1\%$ of the quasar's Eddington luminosity, or $\sim2\%$ of thebolometric luminosity, making it a potential contributor to AGN feedback. Asolution with two ionization phases was needed, as a single phase was notsufficient to satisfy the constraints from the measured ionic column densities.We find that the ionization parameter of the very high-ionization phase of theoutflow is within the expected range of an X-ray warm absorber as described byarXiv:astro-ph/0309096. We also examined the physical properties of the outflowof Q0254-334 along with previously studied extreme UV outflows, with a totalsample of 24 outflow systems, finding a weak negative correlation betweenoutflow velocity and distance from the central source. The very high-ionizationphase of the Q0254-334 outflow has one of the highest ionization parameters ofUV absorption outflows to date, which we attribute to the presence of S XIV.

BAL Outflow in Quasar B0254-3327B: Analysis and Comparison with Other Extreme UV Outflows