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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We report a bimodality in the azimuthal angle ($\Phi$) distribution of gasaround galaxies traced by OVI absorption. We present the mean $\Phi$probability distribution function of 29 HST-imaged OVI absorbing (EW>0.1A) and24~non-absorbing (EW<0.1A) isolated galaxies (0.08<z<0.67) within 200kpc ofbackground quasars. We show that EW is anti-correlated with impact parameterand OVI covering fraction decreases from 80% within 50kpc to 33% at 200kpc. Thepresence of OVI absorption is azimuthally dependent and occurs between$\pm10-20^{\circ}$ of the galaxy projected major axis and within$\pm30^{\circ}$ of the projected minor axis. We find higher EWs along theprojected minor axis with weaker EWs along the project major axis. Highlyinclined galaxies have the lowest covering fractions due to minimizedoutflow/inflow cross-section geometry. Absorbing galaxies also have bluercolors while non-absorbers have redder colors, suggesting that star-formationis a key driver in the OVI detection rate. OVI surrounding blue galaxies existsprimarily along the projected minor axis with wide opening angles while OVIsurrounding red galaxies exists primarily along the projected major axis withsmaller opening angles, which may explain why absorption around red galaxies isless frequently detected. Our results are consistent with CGM originating frommajor axis-fed inflows/recycled gas and from minor axis-driven outflows.Non-detected OVI occurs between $\Phi=20-60^{\circ}$, suggesting that OVI isnot mixed throughout the CGM and remains confined within the outflows and thedisk-plane. We find low OVI covering fractions within $\pm10^{\circ}$ of theprojected major axis, suggesting that cool dense gas resides in a narrow planergeometry surrounded by diffuse OVI gas.

The Azimuthal Dependence of Outflows and Accretion Detected Using OVI Absorption