Observational constraints on the feeding of supermassive black holes

Storchi‐Bergmann, Thaisa; Schnorr-Müller, A.

doi:10.1038/s41550-018-0611-0

Cited by 145 publications

(82 citation statements)

References 233 publications

(262 reference statements)

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“…The above results are in agreement with those of previous studies by our AGNIFS group, in which we have additionally reported, for H 2 , the presence of inflows in a number of galaxies. We have also found that outflows are most easily seen in the ionized gas (Storchi-Bergmann & Schnorr-Müller 2019) and that this gas shows a more centrally concentrated flux distribution than that of H 2 Riffel et al (2018), also in agreement with what we found in the present paper.…”

Section: Gas Kinematicssupporting

confidence: 92%

Gemini NIFS survey of feeding and feedback in nearby active galaxies – III. Ionized versus warm molecular gas masses and distributions

Schönell

Storchi‐Bergmann

Riffel

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We have used the Gemini Near-Infrared Integral Field Spectrograph (NIFS) in the J and K bands to map the distribution, excitation and kinematics of the ionized H ii and warm molecular gas H 2 , in the inner few 100 pc of 6 nearby active galaxies: NGC 788, Mrk 607, NGC 3227, NGC 3516, NGC 5506, NGC 5899. For most galaxies, this is the first time that such maps have been obtained. The ionized and H 2 gas show distinct kinematics: while the H 2 gas is mostly rotating in the galaxy plane with low velocity dispersion (σ), the ionized gas usually shows signatures of outflows associated with higher σ values, most clearly seen in the [Fe ii] emission line. These two gas species also present distinct flux distributions: the H 2 is more uniformly spread over the whole galaxy plane, while the ionized gas is more concentrated around the nucleus and/or collimated along the ionization axis of its Active Galactic Nucleus (AGN), presenting a steeper gradient in the average surface mass density profile than the H 2 gas. The total H ii masses cover the range 2 × 10 5 − 2 × 10 7 M ⊙ , with surface mass densities in the range 3-150 M ⊙ pc −2 , while for the warm H 2 the values are 10 3−4 times lower. We estimate that the available gas reservoir is at least ≈ 100 times more massive than needed to power the AGN. If this gas form new stars the star-formation rates, obtained from the Kennicutt-schmidt scalling relation, are in the range 1-260× 10 −3 M ⊙ yr −1 . But the gas will also -at least in part -be ejected in the form of the observed otflows.

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Section: Gas Kinematicssupporting

confidence: 92%

Gemini NIFS survey of feeding and feedback in nearby active galaxies – III. Ionized versus warm molecular gas masses and distributions

Schönell

Storchi‐Bergmann

Riffel

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The feeding of SMBHs begins with materials accretion at extragalactic scales, which subsequently passes through galactic and nuclear scales to the broad-line region (BLR) and accretion disk before falling into the black hole Article number, page 1 of 30 arXiv:1912.07734v1 [astro-ph.GA] 16 Dec 2019 A&A proofs: manuscript no. aanda or being ejected by jets or winds (Storchi-Bergmann & Schnorr-Müller 2019). The materials in the host galaxy residing near the nucleus can be ionized by radiation (e.g., Davidson 1972;Netzer 1985).…”

Section: Introductionmentioning

confidence: 99%

LLAMA: TheM_BH–σ_⋆relation of the most luminous local AGNs

Çağlar

Burtscher

Brandl

et al. 2020

A&A

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Context. The M BH -σ relation is considered a result of co-evolution between the host galaxies and their super-massive black holes. For elliptical bulge hosting inactive galaxies, this relation is well established, but there is still discussion whether active galaxies follow the same relation. Aims. In this paper, we estimate black hole masses for a sample of 19 local luminous AGNs (LLAMA) in order to test their location on the M BH -σ relation. In addition, we test how robustly we can determine the stellar velocity dispersion in the presence of an AGN continuum, AGN emission lines and as a function of signal/noise ratio. Methods. Super-massive black hole masses (M BH ) were derived from the broad-line based relations for Hα, Hβ and Paβ emission line profiles for the Type 1 AGNs. We compare the bulge stellar velocity dispersion (σ ) as determined from the Ca II triplet (CaT) with the dispersion measured from the near-infrared CO (2-0) absorption features for each AGN and find them to be consistent with each other. We apply an extinction correction to the observed broad line fluxes and we correct the stellar velocity dispersion by an average rotation contribution as determined from spatially resolved stellar kinematic maps. Results. The Hα-based black hole masses of our sample of AGNs were estimated in the range 6.34 ≤ log M BH ≤ 7.75 M and the σ CaT estimates range between 73 ≤ σ CaT ≤ 227 km s −1 . From the so-constructed M BH -σ relation for our Type 1 AGNs, we estimate the black hole masses for the Type 2 AGNs and the inactive galaxies in our sample. Conclusions. In conclusion, we find that our sample of local luminous AGNs is consistent with the M BH -σ relation of lower luminosity AGNs and inactive galaxies, after correcting for dust extinction and the rotational contribution to the stellar velocity dispersion.

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“…Therefore understanding the mechanisms that are involved in transferring the gas from kiloparsec to sub-parsec scales is crucial (e.g. recent review of Storchi-Bergmann & Schnorr-Müller 2019).…”

Section: Introductionmentioning

confidence: 99%

Central kiloparsec of NGC 1326 observed with SINFONI

Fazeli

Busch

Eckart

et al. 2020

A&A

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Gas inflow processes in the vicinity of galactic nuclei play a crucial role in galaxy evolution and supermassive black hole growth. Exploring the central kiloparsec of galaxies is essential to shed more light on this subject. We present near-infrared H- and K-band results of the nuclear region of the nearby galaxy NGC 1326, observed with the integral-field spectrograph SINFONI mounted on the Very Large Telescope. The field of view covers 9″ × 9″ (650 × 650 pc2). Our work is concentrated on excitation conditions, morphology, and stellar content. The nucleus of NGC 1326 was classified as a LINER, however in our data we observed an absence of ionised gas emission in the central r ∼ 3″. We studied the morphology by analysing the distribution of ionised and molecular gas, and thereby detected an elliptically shaped, circum-nuclear star-forming ring at a mean radius of 300 pc. We estimate the starburst regions in the ring to be young with dominating ages of < 10 Myr. The molecular gas distribution also reveals an elongated east to west central structure about 3″ in radius, where gas is excited by slow or mild shock mechanisms. We calculate the ionised gas mass of 8 × 105 M⊙ completely concentrated in the nuclear ring and the warm molecular gas mass of 187 M⊙, from which half is concentrated in the ring and the other half in the elongated central structure. The stellar velocity fields show pure rotation in the plane of the galaxy. The gas velocity fields show similar rotation in the ring, but in the central elongated H2 structure they show much higher amplitudes and indications of further deviation from the stellar rotation in the central 1″ aperture. We suggest that the central 6″ elongated H2 structure might be a fast-rotating central disc. The CO(3–2) emission observations with the Atacama Large Millimeter/submillimeter Array reveal a central 1″ torus. In the central 1″ of the H2 velocity field and residual maps, we find indications for a further decoupled structure closer to a nuclear disc, which could be identified with the torus surrounding the supermassive black hole.

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Observational constraints on the feeding of supermassive black holes

Cited by 145 publications

References 233 publications

Gemini NIFS survey of feeding and feedback in nearby active galaxies – III. Ionized versus warm molecular gas masses and distributions

Gemini NIFS survey of feeding and feedback in nearby active galaxies – III. Ionized versus warm molecular gas masses and distributions

LLAMA: TheM_BH–σ_⋆relation of the most luminous local AGNs

Central kiloparsec of NGC 1326 observed with SINFONI

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Observational constraints on the feeding of supermassive black holes

Cited by 145 publications

References 233 publications

Gemini NIFS survey of feeding and feedback in nearby active galaxies – III. Ionized versus warm molecular gas masses and distributions

Gemini NIFS survey of feeding and feedback in nearby active galaxies – III. Ionized versus warm molecular gas masses and distributions

LLAMA: TheMBH–σ⋆relation of the most luminous local AGNs

Central kiloparsec of NGC 1326 observed with SINFONI

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LLAMA: TheM_BH–σ_⋆relation of the most luminous local AGNs