Investigating the Origin of the Absorption-line Variability in the Narrow-line Seyfert 1 Galaxy WPVS 007

Green, Kaylie S.; Gallagher, Sarah C.; Leighly, Karen M.; Choi 최, Hyunseop 현섭; Grupe, Dirk; Terndrup, Donald M.; Richards, Gordon T.; Komossa, S.

doi:10.3847/1538-4357/ace2c4

Cited by 5 publications

(2 citation statements)

References 78 publications

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“…We found that the data did not require a less restrictive model with multiple velocity-resolved ionization parameters. In order to calculate the total column density, we first calculated column density values corrected for the covering fraction from each bin and summed the values ( Arav et al 2005;Leighly et al 2018;Choi et al 2020;Green et al 2023). Similarly, the wind energetics, such as mass outflow rate, momentum flux, and kinetic luminosity, for the BAL were computed from the sum of the values calculated for each top-hat bin.…”

Section: A1 Best-fit Simbal Modelmentioning

confidence: 99%

Multiphase Black Hole Feedback and a Bright [C ii] Halo in a LoBAL Quasar at z ∼ 6.6

Bischetti,

Choi 최현,

Fiore

et al. 2024

ApJ

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Although the mass growth of supermassive black holes during the epoch of reionization is expected to play a role in shaping the concurrent growth of their host galaxies, observational evidence of feedback at z ≳ 6 is still sparse. We perform the first multiscale and multiphase characterization of black-hole-driven outflows in the z ∼ 6.6 quasar J0923+0402 and assess how these winds impact the cold gas reservoir. We employ the SimBAL spectral synthesis to fit broad absorption line features and find a powerful ionized outflow on a ≲210 pc scale, with a kinetic power ∼2%–100% of the quasar luminosity. Atacama Large Millimeter/submillimeter Array (ALMA) observations of [C ii] emission allow us to study the morphology and kinematics of the cold gas. We detect high-velocity [C ii] emission, likely associated with a cold neutral outflow at ∼0.5−2 kpc scale in the host galaxy, and a bright extended [C ii] halo with a size of ∼15 kpc. For the first time at such an early epoch, we accurately constrain the outflow energetics in both the ionized and the atomic neutral gas phases. We find such energetics to be consistent with expectations for an efficient feedback mechanism, and both ejective and preventative feedback modes are likely at play. The scales and energetics of the ionized and atomic outflows suggest that they might be associated with different quasar accretion episodes. The results of this work indicate that strong black hole feedback is occurring in quasars at z ≳ 6 and is likely responsible for shaping the properties of the cold gas reservoir up to circumgalactic scales.

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Section: A1 Best-fit Simbal Modelmentioning

confidence: 99%

Multiphase Black Hole Feedback and a Bright [C ii] Halo in a LoBAL Quasar at z ∼ 6.6

Bischetti,

Choi 최현,

Fiore

et al. 2024

ApJ

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“…Crucial information about the physical state of these outflows and their origin can be drawn from the study of their variations with time (Lundgren et al 2007;Gibson et al 2008Gibson et al , 2010Filiz Ak et al 2012;Capellupo et al 2011Capellupo et al , 2012Vivek et al 2014; Filiz ⋆ Based on observations collected at Southern African Large Telescope (SALT; Programme IDs 2015-1-SCI-005, 2018-1-SCI-009, 2019-1-SCI-019 and 2020-1-SCI-011) and the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 093.A-0255. † E-mail: aromal@iucaa.in (PA) Ak et al 2013;McGraw et al 2017;Rogerson et al 2018;De Cicco et al 2018;Aromal et al 2022;Green et al 2023).…”

Section: Introductionmentioning

confidence: 99%

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

Aromal

Srianand

Petitjean

2022

Monthly Notices of the Royal Astronomical Society

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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 (zem= 2.04806) at ten different epochs spanning over 19 years. 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 photo-ionization 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 disk and both respond to changes in the ionizing continuum.

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Time variability of ultra fast BAL outflows using SALT: C iv equivalent width analysis

Aromal

Srianand

Petitjean

2023

Monthly Notices of the Royal Astronomical Society

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We study the time variability (over ≤7.3 yrs) of ultra fast outflows (UFOs) detected in a sample of 64 C iv broad absorption line (BAL) quasars (with 80 distinct BAL components) monitored using the Southern African Large Telescope. By comparing the properties of the quasar in our sample with those of a control sample of non-BAL quasars we show that the distributions of black hole mass are different and the bolometric luminosities and optical photometric variations of UFO BAL quasars are slightly smaller compared to that of non-BAL quasars. The detection fraction of C iv equivalent width (W) variability (∼95%), the fractional variability amplitude ($\frac{\Delta W}{W}$) and the fraction of “highly variable” BAL (i.e., $\big {|}\frac{\Delta W}{W}\big {|}$>0.67) components (∼ 33%) are higher in our sample compared to the general BAL population. The scatter in $\frac{\Delta W}{W}$ and the fraction of “highly variable” BALs increase with the time-scale probed. The $\frac{\Delta W}{W}$ distribution is asymmetric at large time scales. We attribute this to the BAL strengthening time scales being shorter than the weakening time scales. The BAL variability amplitude correlates strongly with the BAL properties compared to the quasar properties. BALs with low W, high-velocity, shallow profiles, and low-velocity width tend to show more variability. When multiple BAL components are present a correlated variability is seen between low- and high-velocity components with the latter showing a larger amplitude variations. We find an anti-correlation between the fractional variations in the continuum flux and W. While this suggests photoionization-induced variability, the scatter in continuum flux is much smaller than that of W.

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Investigating the Origin of the Absorption-line Variability in the Narrow-line Seyfert 1 Galaxy WPVS 007

Cited by 5 publications

References 78 publications

Multiphase Black Hole Feedback and a Bright [C ii] Halo in a LoBAL Quasar at z ∼ 6.6

Multiphase Black Hole Feedback and a Bright [C ii] Halo in a LoBAL Quasar at z ∼ 6.6

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

Time variability of ultra fast BAL outflows using SALT: C iv equivalent width analysis

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