Supermassive Black Holes, Pseudobulges, and the Narrow-Line Seyfert 1 Galaxies

Mathur, S.; Fields, Dale L.; Peterson, B. M.; Grupe, D.

doi:10.1088/0004-637x/754/2/146

Cited by 114 publications

(138 citation statements)

References 74 publications

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“…Our results thus suggest that models in which late time disk instabilities, mainly characterized by the formation of bars, are not closely related to BH growth, tend to generate a larger scatter in the M bh -M bulge relation in better agreement with the broad distribution of BHs we observe today. This finding confirms prior expectations (see, e.g., Kormendy et al 2011;Mathur et al 2012, and references therein).…”

Section: Discussionsupporting

confidence: 92%

“…Different authors have used different techniques to estimate BH (and bulge) masses, and each technique has its own set of errors. The average error in BH masses for active and inactive galaxies is of the order of ∼0.3 dex (see, e.g., Mathur et al 2012). Of similar magnitude is the propagated error on stellar masses at fixed galaxy colour (see, e.g., Bell et al 2003).…”

Section: Datamentioning

confidence: 94%

“…Perhaps one of the most pressing reason to argue for supplementary routes of BH evolution is the prevalence of pseudobulges hosting BHs (e.g., Hu 2008;Gadotti & Kauffmann 2009;Kormendy et al 2011;Mathur et al 2012;Orban de Xivry et al 2011). "Pseudobulges" are structurally and dynamically different from "classical" bulges and ellipticals, which can also have very low specific angular momentum (e.g., Emsellem et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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Black holes in pseudobulges: demography and models

Shankar

Marulli

Mathur

et al. 2012

A&A

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Context. There is mounting evidence that a significant fraction of black holes (BHs) today live in late-type galaxies, including bulgeless galaxies and those hosting pseudobulges, and are significantly undermassive with respect to the scaling relations followed by their counterpart BHs in classical bulges of similar stellar (or even bulge) mass. Aims. Here we discuss the predictions of two state-of-the-art hierarchical galaxy formation models in which BHs grow via mergers and, in one, also via disc instability. Our aim is to understand if the wealth of new data on local BH demography is consistent with standard models. Methods. We follow the merger trees of representative subsamples of BHs and compute the fractional contributions of different processes to the final BH mass. Results. We show that the model in which BHs always closely follow the growth of their host bulges, also during late disk instabilities (i.e., bars), produces too narrow a distribution of BHs at fixed stellar mass to account for the numerous low-mass BHs now detected in later-type galaxies. Models with a looser connection between BH growth and bar instability instead predict the existence of a larger number of undermassive BHs, in better agreement with the observations. Conclusions. The scatter in the updated local BH-bulge mass relation (with no restriction on galaxy type) appears to be quite large when including later-type systems, but it can still be managed to be reproduced within current hierarchical models. However, the fuelling of BHs during the late bar-instability mode needs to be better quantified/improved to properly fit the data. We conclude discussing how the possibly large number of BHs in later type galaxies demands for an in-depth revision of the local BH mass function and its modelling.

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Section: Discussionsupporting

confidence: 92%

Section: Datamentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

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Black holes in pseudobulges: demography and models

Shankar

Marulli

Mathur

et al. 2012

A&A

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“…The right bottom subplot shows the z = 2, 5 and 7 Magorrian relations of the Tiamat result with thick lines compared with the z ∼ 0.6 Tiamat-125-HR Magorrian relation. Observations from the local Universe are indicated with different symbols (Thornton et al 2008;Jiang et al 2011;Mathur et al 2012;Jiang et al 2013;Reines et al 2013;Scott et al 2013;Busch et al 2014;Sanghvi et al 2014;Yuan et al 2014). We see that the model predicts a similar Magorrian relation at z ∼ 0.6 compared to the local observations and we find an increasing normalization towards lower redshifts in the mass range of 10 10 M < M * < 10 12 M .…”

Section: Black Hole Propertiessupporting

confidence: 51%

Dark-ages reionization and galaxy formation simulation – X. The small contribution of quasars to reionization

Qin

Mutch

Poole

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Motivated by recent measurements of the number density of faint AGN at high redshift, we investigate the contribution of quasars to reionization by tracking the growth of central supermassive black holes in an update of the Meraxes semi-analytic model. The model is calibrated against the observed stellar mass function at z ∼ 0.6 − 7, the black hole mass function at z 0.5, the global ionizing emissivity at z ∼ 2 − 5 and the Thomson scattering optical depth. The model reproduces a Magorrian relation in agreement with observations at z < 0.5 and predicts a decreasing black hole mass towards higher redshifts at fixed total stellar mass. With the implementation of an opening angle of 80 deg for quasar radiation, corresponding to an observable fraction of ∼23.4 per cent due to obscuration by dust, the model is able to reproduce the observed quasar luminosity function at z ∼ 0.6 − 6. The stellar light from galaxies hosting faint AGN contributes a significant or dominant fraction of the UV flux. At high redshift, the model is consistent with the bright end quasar luminosity function and suggests that the recent faint z ∼ 4 AGN sample compiled by Giallongo et al. (2015) includes a significant fraction of stellar light. Direct application of this luminosity function to the calculation of AGN ionizing emissivity consequently overestimates the number of ionizing photons produced by quasars by a factor of 3 at z ∼ 6. We conclude that quasars are unlikely to make a significant contribution to reionization.

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“…One possible explanation, advanced by Doi et al (2012), is that in the case of RLNLS1s, the jet has low kinetic power because of the low mass and because it has to propagate in a gas-rich environment, while in BL Lacs the jet power is slightly greater and develops in a more rarified medium. Another possibility is to invoke the young age of RLNLS1s (Mathur 2000, Mathur et al 2012) and, indeed, many authors made the hypothesis of a link with GPS/CSS sources, which in turn are believed to be very young radio galaxies (Oshlack et al 2001, Komossa et al 2006a, Gallo et al 2006, Yuan et al 2008, Caccianiga et al 2014). Yet another option has been proposed by Gu & Chen (2010): the jet activity could be intermittent, as observed in other Seyferts (e.g.…”

Section: Discussionmentioning

confidence: 99%

Properties of flat-spectrum radio-loud narrow-line Seyfert 1 galaxies

Foschini

Berton

Caccianiga

et al. 2015

A&A

188

344

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We have conducted a multiwavelength survey of 42 radio loud narrow-1ine Seyfert 1 galaxies (RLNLS1s), selected by searching among all the known sources of this type and omitting those with steep radio spectra. We analyse data from radio frequencies to X-rays, and supplement these with information available from online catalogues and the literature in order to cover the full electromagnetic spectrum. This is the largest known multiwavelength survey for this type of source. We detected 90% of the sources in X-rays and found 17% at γ rays. Extreme variability at high energies was also found, down to timescales as short as hours. In some sources, dramatic spectral and flux changes suggest interplay between a relativistic jet and the accretion disk. The estimated masses of the central black holes are in the range ∼ 10 6−8 M ⊙ , lower than those of blazars, while the accretion luminosities span a range from ∼ 0.01 to ∼ 0.49 times the Eddington limit, with an outlier at 0.003, similar to those of quasars. The distribution of the calculated jet power spans a range from ∼ 10 42.6 to ∼ 10 45.6 erg s −1 , generally lower than quasars and BL Lac objects, but partially overlapping with the latter. Once normalised by the mass of the central black holes, the jet power of the three types of active galactic nuclei are consistent with each other, indicating that the jets are similar and the observational differences are due to scaling factors. Despite the observational differences, the central engine of RLNLS1s is apparently quite similar to that of blazars. The historical difficulties in finding radio-loud narrow-line Seyfert 1 galaxies might be due to their low power and to intermittent jet activity.

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Supermassive Black Holes, Pseudobulges, and the Narrow-Line Seyfert 1 Galaxies

Cited by 114 publications

References 74 publications

Black holes in pseudobulges: demography and models

Black holes in pseudobulges: demography and models

Dark-ages reionization and galaxy formation simulation – X. The small contribution of quasars to reionization

Properties of flat-spectrum radio-loud narrow-line Seyfert 1 galaxies

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