Recalibration of the M<sub>BH</sub>–σ<sub>⋆</sub> Relation for AGN

Batiste, Merida; Bentz, Misty C.; Raimundo, S. I.; Vestergaard, M.; Onken, Christopher A.

doi:10.3847/2041-8213/aa6571

Cited by 71 publications

(65 citation statements)

References 41 publications

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“…The evolution behavior of star formation rate density within galaxies is similar to that of the black hole accretion rate density (e.g., Aird et al 2010;Madau & Dickinson 2014). The black hole mass is tightly related with the stellar mass (e.g., Kormendy & Ho 2013;Bell et al 2017) or stellar velocity dispersion (e.g., Gu et al 2009;Kormendy & Ho 2013;Bennert et al 2015;Batiste et al 2017) of the host galaxy bulge. These signatures reveal a connection between the AGN activity and global properties of host galaxies, which is widely researched and debated in the last decades (e.g., Ferrarese & Merritt 2000;Di Matteo et al 2005;Bundy et al 2008;Bongiorno et al 2012;Kormendy & Ho 2013;McAlpine et al 2017;Wang et al 2017;Biernacki et al 2017).…”

Section: Introductionmentioning

confidence: 67%

Collective Properties of Quasar Narrow Associated Absorption Lines

Chen

Pan²

2017

ApJ

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This paper statistically investigates the properties of C IV and Mg II narrow absorption lines (NALs) to look for velocity cuts that can well constrain quasar-associated NALs. The coverage fraction ( f c ) is defined as the ratio between the number of quasars exhibiting at least one detected absorber and the total number of quasars that can be used to detect absorptions with given criteria. We find that, for both C IV and Mg II absorbers, both the number density of absorbers in given velocity intervals (dn/dβ) and the f c show very significant excess at the low-velocity offset from the quasars, relative to the random occurrence that is expected for cosmologically intervening absorbers. These relative excess extensions for Mg II absorptions are not only evidently related to absorption strength but also to quasar luminosity, while they are mainly constrained within 2000 km s . Turning to C IV absorptions, the relative excess extensions of both dn/dβ and f c are mainly limited within v abs < 4000 km s, and depend neither on absorption strength nor on quasar luminosity. And also, the absorbers with v abs < 4000 km sshow obviously different redshift number density evolution from those with v abs > 4000 km s −1. We suggest velocity cuts of 4000 km s to define quasar C IV and Mg II associated NALs, respectively.

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Section: Introductionmentioning

confidence: 67%

Collective Properties of Quasar Narrow Associated Absorption Lines

Chen

Pan²

2017

ApJ

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“…Indeed the number of bars in the SDSS galaxies is significant (e.g., Consolandi 2016). Bars, as also pointed out by Shankar et al (2016), may increase velocity dispersions at fixed stellar mass (see also Graham et al 2011 andBatiste et al 2017). Nevertheless, even if such an effect is present, this would imply an intrinsic/unbiased SDSS σ-Mstar relation lower in normalization than what plotted in Figure 1, which would exacerbate the tension with the local sample of black holes in quiescent galaxies.…”

Section: The σ-Mstar Relation Of Active Galaxiesmentioning

confidence: 86%

Black hole scaling relations of active and quiescent galaxies: Addressing selection effects and constraining virial factors

Shankar

Bernardi

Richardson

et al. 2019

Monthly Notices of the Royal Astronomical Society

114

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Local samples of quiescent galaxies with dynamically measured black hole masses (M bh ) may suffer from an angular resolution-related selection effect, which could bias the observed scaling relations between M bh and host galaxy properties away from the intrinsic relations. In particular, previous work has shown that the observed M bh -M star relation is more strongly biased than the M bh -σ relation. Local samples of active galactic nuclei (AGN) do not suffer from this selection effect, as in these samples M bh is estimated from megamasers and/or reverberation mapping-based techniques. With the exception of megamasers, M bh -estimates in these AGN samples are proportional to a virial coefficient f vir . Direct modelling of the broad line region suggests that f vir ∼ 3.5. However, this results in a M bh -M star relation for AGN which lies below and is steeper than the one observed for quiescent black hole samples. A similar though milder trend is seen for the M bh -σ relation. Matching the high-mass end of the M bh -M star and M bh -σ relations observed in quiescent samples requires f vir 15 and f vir 7, respectively. On the other hand, f vir ∼ 3.5 yields M bh -σ and M bh -M star relations for AGN which are remarkably consistent with the expected "intrinsic" correlations for quiescent samples (i.e., once account has been made of the angular resolution-related selection effect), providing additional evidence that the sample of local quiescent black holes is biased. We also show that, as is the case for quiescent black holes, the M bh -M star scaling relation of AGN is driven by σ, thus providing additional key constraints to black hole-galaxy co-evolution models.

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“…This gives rise to outflows [141] of molecular and ionized gas that are likely radiatively driven. Understanding these outflows is critical as they may deliver feedback to the galaxy by clearing the inner regions of star forming gas, and assist in establishing the observed scaling relationships between galaxies and their supermassive black holes (SMBHs) [142][143][144][145].…”

Section: The Effects Of Agn and Mass Outflows On Line Emissionmentioning

confidence: 99%

Challenges and Techniques for Simulating Line Emission

et al. 2018

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Modeling emission lines from the millimeter to the UV and producing synthetic spectra is crucial for a good understanding of observations, yet it is an art filled with hazards. This is the proceedings of "Walking the Line", a 3-day conference held in 2018 that brought together scientists working on different aspects of emission line simulations, in order to share knowledge and discuss the methodology. Emission lines across the spectrum from the millimeter to the UV were discussed, with most of the focus on the interstellar medium, but also some topics on the circumgalactic medium. The most important quality of a useful model is a good synergy with observations and experiments. Challenges in simulating line emission are identified, some of which are already being worked upon, and others that must be addressed in the future for models to agree with observations. Recent advances in several areas aiming at achieving that synergy are summarized here, from micro-physical to galactic and circum-galactic scale.2 of 29 us to characterize the mass, composition, and chemical state of the ISM, as well as to trace galaxy properties such as star formation rate (SFR), metallicity and dynamics. For example, the emission from major cooling lines, such as Hα or [C II], is sensitive to the physical conditions (densities, radiation field) and dynamics of the ISM. In addition, emission lines work on all physical scales, from galaxy dynamics and inflows to turbulent and collapse motions in star-forming clouds and cores. By systematically comparing spectral-line signatures of different physical models, one can correctly identify the physical processes occurring in these regions. Furthermore, the emission from ionized interstellar gas contains particularly valuable information about the nature of the ionizing radiation sources in a galaxy. In fact, prominent optical emission lines are routinely used to estimate whether ionization is dominated by young massive stars (tracing SFR), an AGN or evolved, post-asymptotic giant branch (post-AGB) stars. Three of the most widely used line-ratio diagnostic "BPT" diagrams 1 , relate the [OIII]/Hβ ratio to the [NII]/Hα, [SII]/Hα and [OI]/Hα ratios. These diagrams have proven useful in identifying the nature of the ionizing radiation in large samples of galaxies in the local Universe [2,3]. Complementary to line emission are the observations of absorption lines of the circumgalactic medium (CGM), which can give key information on the history of the feedback, in terms of chemical, ionization, and thermodynamical state of the outflowing/inflowing gas, that regulates the star formation process. Gas kinematics, from both emission and absorption, give information about large scale gas flows. Thus galactic outflows, from active galactic nuclei (AGN) and starbursts, can be combined with CGM absorption line observations, to study the star formation history, AGN activity history, and feedback processes that regulate both the evolution of the galaxy and its environment.Looking back on the past three decades, t...

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Recalibration of the M_BH–σ_⋆ Relation for AGN

Cited by 71 publications

References 41 publications

Collective Properties of Quasar Narrow Associated Absorption Lines

Collective Properties of Quasar Narrow Associated Absorption Lines

Black hole scaling relations of active and quiescent galaxies: Addressing selection effects and constraining virial factors

Challenges and Techniques for Simulating Line Emission

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Recalibration of the MBH–σ⋆ Relation for AGN

Cited by 71 publications

References 41 publications

Collective Properties of Quasar Narrow Associated Absorption Lines

Collective Properties of Quasar Narrow Associated Absorption Lines

Black hole scaling relations of active and quiescent galaxies: Addressing selection effects and constraining virial factors

Challenges and Techniques for Simulating Line Emission

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Product

Resources

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Recalibration of the M_BH–σ_⋆ Relation for AGN