A local baseline of the black hole mass scaling relations for active galaxies. IV. Correlations between $M_{\rm BH}$ and host galaxy $σ$, stellar mass, and luminosity

Bennert, Vardha N.; Treu, Tommaso; Ding, Xuheng; Stomberg, Isak; Birrer, Simon; Snyder, Tomas; Malkan, Matthew A.; Stephens, Andrew W.; Auger, Matthew W.

doi:10.48550/arxiv.2101.10355

Cited by 3 publications

(5 citation statements)

References 78 publications

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“…The same IMF and stellar population model are assumed in both works when converting the decomposed galaxy fluxes to bulge or stellar masses. Their bulge masses range from 9.0 < log M bulge < 10.3, and closely follow the M BH −M bulge relation defined by quiescent galaxies (Bennert et al 2011b(Bennert et al , 2021. The inclusion of the local AGN sample thus helps to improve the constraint on the M BH −M bulge relation at the low-mass end.…”

Section: Methods and Sample Selectionsupporting

confidence: 55%

Synchronized Co-evolution between Supermassive Black Holes and Galaxies Over the Last Seven Billion Years as Revealed by the Hyper Suprime-Cam

Li,

Silverman,

Ding

et al. 2021

Preprint

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We measure the evolution of the M BH − M relation using 584 uniformly-selected SDSS quasars at 0.2 < z < 0.8. The black-hole masses (M BH ) are derived from the single-epoch virial mass estimator using the Hβ emission line, and span the range 7.0 < log M BH /M < 9.5. The host-galaxy stellar masses (M ), which cover the interval 10.0 < log M /M < 11.5, are determined by performing two-dimensional quasar-host decomposition of the Hyper Suprime-Cam images and spectral energy distribution fitting. To quantify sample-selection biases and measurement uncertainties on the mass terms, a mock quasar sample is constructed to jointly constrain the redshift evolution of the M BH − M relation and its intrinsic scatter (σ µ ) through forward modeling. We find that the level of evolution is degenerate with σ µ , such that both positive mild evolution (i.e, M BH /M increases with redshift) with a small σ µ , and negative mild evolution with a larger σ µ are consistent with our data. The posterior distribution of σ µ enables us to put a strong constraint on the intrinsic scatter of the M BH − M relation, which has a best inference of 0.25 +0.03 −0.04 dex, consistent with the local value. The redshift evolution of the M BH − M relation relative to the local relation is constrained to be (1 + z) 0.12 +0.28 −0.27 , in agreement with no significant evolution since z ∼ 0.8. The tight and non-evolving M BH − M relation is suggestive of a coupling through AGN feedback or/and a common gas supply at work, thus restricting the mass ratio of galaxies and their black holes to a limited range. Given the considerable stellar disk component, the M BH − M bulge relation may evolve as previously seen at higher redshifts.

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Section: Methods and Sample Selectionsupporting

confidence: 55%

Synchronized Co-evolution between Supermassive Black Holes and Galaxies Over the Last Seven Billion Years as Revealed by the Hyper Suprime-Cam

Li,

Silverman,

Ding

et al. 2021

Preprint

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“…galight adds a number of features to process large numbers of images from survey data. This tool has been used to model the galaxy images from Hubble Space Telescope (HST) [5,6] and Subaru Hyper Suprime-Cam (HSC) [7,8], including a sample of ∼1.5 million galaxies and ∼5 thousand quasars profiting from the automatic features.…”

Section: Introductionmentioning

confidence: 99%

“…We highlight features in the Appendix and a summary is given in Section 5. We refer the reader to a number of studies that have made use of galight [5,6,7,8].…”

Section: Introductionmentioning

confidence: 99%

Galaxy shapes of Light (GaLight): a 2D modeling of galaxy images

Ding¹,

Birrer²,

Treu³

et al. 2021

Preprint

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galight is a Python-based open-source package that can be used to perform two-dimensional model fitting of optical and nearinfrared images to characterize the light distribution of galaxies with components including a disk, bulge, bar, and quasar. The decomposition of stellar components has been demonstrated in published studies of inactive galaxies and quasar host galaxies observed by the Hubble Space Telescope and Subaru's Hyper Suprime-Cam. galight utilizes the image modeling capabilities of lenstronomy while redesigning the user interface for the analysis of large samples of extragalactic sources. The package is user-friendly with some automatic features such as determining the cutout size of the modeling frame, searching for PSF-stars in field-of-view, estimating the noise map of the data, identifying all the objects to set the initial model and associated parameters to fit them simultaneously. These features minimize the manpower and allow the automatic fitting tasks. The software is distributed under the MIT license. The source code, installation guidelines, and example notebooks code can be found at https://galight. readthedocs.io/en/latest/.

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“…where L sph,I is the I-band spheroid luminosity, and α = 9.11 ± 1.15 and β = 1.02 ± 0.11 for quiescent galaxies and α = 8.88 ± 0.05 and β = 1.02 (fixed) for type 1 AGN (Bennert et al 2021). We estimate L sph,I by the following procedure.…”

Section: Black Hole Mass and Eddington Luminositymentioning

confidence: 99%

“…For spiral galaxies, the flux is dominated by disk. Bennert et al (2021) shows that the average difference between the spheroid and the disk magnitudes is m sph − m disk = 0.795 (Table 4 in Bennert et al 2021). We use this correction for spiral galaxies and galaxies with unknown morphology.…”

Section: Black Hole Mass and Eddington Luminositymentioning

confidence: 99%

Variability Selected Active Galactic Nuclei from ASAS-SN Survey: Constraining the Low Luminosity AGN Population

Yuk,

Dai,

Jayasinghe

et al. 2022

Preprint

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Low luminosity active galactic nuclei (LLAGN) probe accretion physics in the low Eddington regime and can provide additional clues about galaxy evolution. AGN variability is ubiquitous and thus provides a reliable tool for finding AGN. We analyze the All-Sky Automated Survey for Supernovae light curves of 1218 galaxies with g < 14 mag and Sloan Digital Sky Survey spectra in search of AGN. We find 37 objects that are both variable and have AGN-like structure functions, which is about 3% of the sample. The majority of the variability selected AGN are LLAGN with Eddington ratios ranging from 10 −4 to 10 −2 . We thus estimate the fraction of LLAGN in the population of galaxies as 2% down to a median Eddington ratio of 2 × 10 −3 . Combining the BPT line ratio diagnostics and the broad line AGN, up to ∼60% of the AGN candidates are confirmed spectroscopically. The BPT diagnostics also classified 10-30% of the candidates as star forming galaxies rather than AGN. INTRODUCTIONActive galactic nuclei (AGN) are some of the most luminous objects found in the universe, driven by accretion onto a supermassive black hole. Studies show that AGN and their host galaxy properties are strongly correlated. For example, the AGN class is closely related to galaxy morphology (e.g.,

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A local baseline of the black hole mass scaling relations for active galaxies. IV. Correlations between $M_{\rm BH}$ and host galaxy $σ$, stellar mass, and luminosity

Abstract: A local baseline of the black hole mass scaling relations for active galaxies. IV. Correlations between M BH and host galaxy σ, stellar mass, and luminosity.

Cited by 3 publications

References 78 publications

Synchronized Co-evolution between Supermassive Black Holes and Galaxies Over the Last Seven Billion Years as Revealed by the Hyper Suprime-Cam

Synchronized Co-evolution between Supermassive Black Holes and Galaxies Over the Last Seven Billion Years as Revealed by the Hyper Suprime-Cam

Galaxy shapes of Light (GaLight): a 2D modeling of galaxy images

Variability Selected Active Galactic Nuclei from ASAS-SN Survey: Constraining the Low Luminosity AGN Population

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