The Coevolution of Galaxies and Supermassive Black Holes in the Near Universe

Storchi‐Bergmann, Thaisa

doi:10.1007/s13538-013-0168-4

Cited by 3 publications

(2 citation statements)

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“…(iii) Inflows are observed in H 2 (e.g., Müller-Sánchez et al 2006;Riffel et al 2013b;Mazzalay et al 2014) in Seyfert galaxies and in low-ionization gas in LINERs (Fathi et al 2006;Storchi-Bergmann et al 2007;Schnorr-Müller al. 2011 with mass inflow rates in the range 10 −1 -10 1 M yr −1 (Storchi-Bergmann 2013. (iv) The stellar kinematics of Seyfert galaxies reveals cold nuclear structures composed of young stars, usually associated with a significant gas reservoir (Riffel et al 2010b(Riffel et al , 2011cStorchiBergmann et al 2012;Hicks et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Feeding versus feedback in active galactic nuclei from near-infrared integral field spectroscopy – X. NGC 5929

Riffel

Storchi‐Bergmann

2015

Mon. Not. R. Astron. Soc.

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We present near-infrared emission-line flux distributions, excitation and kinematics, as well as stellar kinematics, of the inner 520 × 520 pc 2 of the Seyfert 2 galaxy NGC 5929. The observations were performed with Gemini's Near-Infrared Integral Field Spectrograph (NIFS) at a spatial resolution of ∼20 pc and spectral resolution of 40 km s −1 in the J and K l bands. The flux distributions of H 2 , [Fe II], [P II] and H recombination lines are extended over most of the field of view, with the highest intensity levels observed along PA = 60/240• , and well correlated with the radio emission. The H 2 and [Fe II] line emission originated in thermal processes, mainly due to heating of the gas by X-rays from the central active galactic nucleus (AGN). The contribution of shocks due to the radio jet is observed at locations co-spatial with the radio hotspots at 0.50 arcsec north-east and 0.60 arcsec south-west of the nucleus, as evidenced by the emission-line ratio and gas kinematics. The stellar kinematics shows rotation with an amplitude at 250 pc from the nucleus of ∼200 km s −1 after correcting for the inferred inclination of 18.3• . The stellar velocity dispersion obtained from the integrated K-band spectrum is σ * = 133 ± 8 km s −1 , which implies a mass for the supermassive black hole of M • = 5.2 1.6 −1.2 × 10 7 M , using the M • -σ * relation. The gas kinematics present three components: (1) gas in the plane of the galaxy in counter-rotation relative to the stars; (2) an outflow perpendicular to the radio jet that seems to be due to an equatorial AGN outflow; and (3) turbulence of the gas observed in association with the radio hotspots, supporting an interaction of the radio jet with the gas of the disc. We estimated the masses of ionized gas and warm molecular gas to be ∼1.3 × 10 6 M and ∼470 M , respectively.

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Section: Introductionmentioning

confidence: 99%

Feeding versus feedback in active galactic nuclei from near-infrared integral field spectroscopy – X. NGC 5929

Riffel

Storchi‐Bergmann

2015

Mon. Not. R. Astron. Soc.

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“…Radial velocity shifts of broad emission lines can also result from recoiling BHs (Herrmann et al 2007;Eracleous et al 2012), tidal disruption events (Gezari 2021), and gas outflows/ inflows (Brotherton et al 1994;Storchi-Bergmann 2010;Rakshit & Woo 2018;Kovačević-Dojčinović et al 2022). In addition, Barth et al (2015) found that Hβ velocity centroids can undergo dramatic changes, on timescales of a month, in response to continuum flux variations.…”

Section: Introductionmentioning

confidence: 99%

The SDSS-V Black Hole Mapper Reverberation Mapping Project: Unusual Broad-line Variability in a Luminous Quasar

Fries

Trump

Davis

et al. 2023

ApJ

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We present a high-cadence multiepoch analysis of dramatic variability of three broad emission lines (Mg ii, Hβ, and Hα) in the spectra of the luminous quasar (λ L λ (5100 Å) = 4.7 × 1044 erg s−1) SDSS J141041.25+531849.0 at z = 0.359 with 127 spectroscopic epochs over nine years of monitoring (2013–2022). We observe anticorrelations between the broad emission-line widths and flux in all three emission lines, indicating that all three broad emission lines “breathe” in response to stochastic continuum variations. We also observe dramatic radial velocity shifts in all three broad emission lines, ranging from Δv ∼ 400 km s−1 to ∼800 km s−1, that vary over the course of the monitoring period. Our preferred explanation for the broad-line variability is complex kinematics in the gas in the broad-line region. We suggest a model for the broad-line variability that includes a combination of gas inflow with a radial gradient, an azimuthal asymmetry (e.g., a hot spot), superimposed on the stochastic flux-driven changes to the optimal emission region (“line breathing”). Similar instances of line-profile variability due to complex gas kinematics around quasars are likely to represent an important source of false positives in radial velocity searches for binary black holes, which typically lack the kind of high-cadence data we analyze here. The long-duration, wide-field, and many-epoch spectroscopic monitoring of SDSS-V BHM-RM provides an excellent opportunity for identifying and characterizing broad emission-line variability, and the inferred nature of the inner gas environment, of luminous quasars.

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Insights on the Dusty Torus and Neutral Torus From Optical and X-Ray Obscuration in a Complete Volume Limited Hard X-Ray Agn Sample

Davies

Burtscher

Rosario

et al. 2015

ApJ

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We describe a complete volume limited sample of nearby active galaxies selected by their 14-195 keV luminosity, and outline its rationale for studying the mechanisms regulating gas inflow and outflow. We describe also a complementary sample of inactive galaxies, selected to match the AGN host galaxy properties. The active sample appears to have no bias in terms of AGN type, the only difference being the neutral absorbing column which is two orders of magnitude greater for the Seyfert 2s. In the luminosity range spanned by the sample, log L 14−195 keV [erg s −1 ] = 42.4-43.7, the optically obscured and X-ray absorbed fractions are 50-65%. The similarity of these fractions to more distant spectroscopic AGN samples, although over a limited luminosity range, suggests that the torus does not strongly evolve with redshift. Our sample confirms that X-ray unabsorbed Seyfert 2s are rare, comprising not more than a few percent of the Seyfert 2 population. At higher luminosities, the optically obscured fraction decreases (as expected for the increasing dust sublimation radius), but the X-ray absorbed fraction changes little. We argue that the cold X-ray absorption in these Seyfert 1s can be accounted for by neutral gas in clouds that also contribute to the broad line region (BLR) emission; and suggest that a geometrically thick neutral gas torus co-exists with the BLR and bridges the gap to the dusty torus.

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The Coevolution of Galaxies and Supermassive Black Holes in the Near Universe

Cited by 3 publications

References 30 publications

Feeding versus feedback in active galactic nuclei from near-infrared integral field spectroscopy – X. NGC 5929

Feeding versus feedback in active galactic nuclei from near-infrared integral field spectroscopy – X. NGC 5929

The SDSS-V Black Hole Mapper Reverberation Mapping Project: Unusual Broad-line Variability in a Luminous Quasar

Insights on the Dusty Torus and Neutral Torus From Optical and X-Ray Obscuration in a Complete Volume Limited Hard X-Ray Agn Sample

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