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 present a time variability analysis of broad absorption lines (BAL; spreadover the velocity range of 5800-29000 km/s) seen in the spectrum ofJ132216.25+052446.3 (z(em)= 2.04806) at ten different epochs spanning over 19years. The strongest absorption component (BAL-A; spread over 5800-9900 km/s)is made up of several narrow components having velocity separations close to CIV doublet splitting. The C IV, N V, and Si IV absorption from BAL-A showcorrelated optical depth variability without significant changes in thevelocity structure. A very broad and shallow absorption (BAL-C; spread over thevelocity range 15000-29000 km/s) emerged during our monitoring periodcoinciding with a dimming episode of J1322+0524. All the identified absorptionlines show correlated variability with the equivalent widths increasing withdecreasing flux. This together with the C IV emission-line variability isconsistent with ionization being the main driver of the correlated variability.The observed UV-continuum variations are weaker than what is required by thephoto-ionization models. This together with a scatter in the C iv equivalentwidth at a given continuum flux can be understood if variations of the C IVionizing photons are much larger than that of the UV continuum, the variationsin the ionizing photon and UV fluxes are not correlated and/or the coveringfactor of the flow varies continuously. We suggest BAL-A is produced by astable clumpy outflow located beyond the broad emission line region and BAL-Cis a newly formed wind component located near the accretion disk and bothrespond to changes in the ionizing continuum.

Coordinated time variability of multi-phase ultra-fast outflows in J132216.25+052446.3