Coordinated time variability of multi-phase ultra-fast outflows in J132216.25 + 052446.3. Issue 2 (30th May 2022)

• Record Type: Journal Article
• Authors: Aromal, P; Srianand, R; Petitjean, P
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 514:Issue 2(2022)
• Page Start: 1975
• Page End: 1989
• Publication Date: 2022-05-30
• Subjects: galaxies: active -- quasars: absorption lines -- quasars: general -- quasars: individual (J132216.25 + 052446.3); Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stac1460
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We present a time variability analysis of broad absorption lines (BAL; spread over the velocity range of 5800–29 000 km s −1 ) seen in the spectrum of J132216.25 + 052446.3 ( z em = 2.04806) at ten different epochs spanning over 19 yr. The strongest absorption component (BAL-A; spread over 5800–9900 km s −1 ) is made up of several narrow components having velocity separations close to C iv doublet splitting. The C iv, N v, and Si iv absorption from BAL-A show correlated optical depth variability without major changes in the velocity structure. A very broad and shallow absorption (BAL-C; spread over the velocity range 15 000–29 000 km s −1 ) emerged during our monitoring period coinciding with a dimming episode of J1322 + 0524. All the identified absorption lines show correlated variability with the equivalent widths increasing with decreasing flux. This together with the C iv emission line variability is consistent with ionization being the main driver of the correlated variability. The observed UV-continuum variations are weaker than what is required by the photoionization models. This together with a scatter in the C iv equivalent width at a given continuum flux can be understood if variations of the C iv ionizing photons are much larger than that of the UV continuum, the variations in the ionizing photon and UV fluxes are not correlated and/or the covering factor of the flow varies continuously. We suggest BAL-A is produced by a stable clumpy outflow located beyond the broad emission line region and BAL-C is a newly formed wind component located near the accretion disc and both respond to changes in the ionizing continuum.