THE LOCAL BLACK HOLE MASS FUNCTION DERIVED FROM THE M<sub>BH</sub>–P AND THE M<sub>BH</sub>–n RELATIONS

Mutlu-Pakdil, Burçin; Seigar, Marc S.; Davis, Benjamin L.

doi:10.3847/0004-637x/830/2/117

Cited by 39 publications

(43 citation statements)

References 59 publications

(121 reference statements)

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“…It depends on the Betti numbers of the spacetime [24,49], the isoperimetric constant [38] and the volume of the manifold boundary. The interpretations of Λ T in terms of number and surface of BHs in the Universe allows to evaluate it from current estimates of the BH distribution of the Universe [41][42][43][44]. We found, with some reasonable assumptions on the isoperimetric constant, that it is compatible with current cosmological constant observations [4][5][6][7]47], escaping the cosmological constant fine tuning problem [9,10].…”

Section: Discussionsupporting

confidence: 62%

“…We chose to evaluate the BH mass distribution based on the observations and computations of Refs [41][42][43][44]. From them, we have extracted averages and standard deviations from the expected peaks in the BH distributions around stellar mass BHs, Primordial BHs (PBHs), Intermediate mass BHs (IMBHs) and Super Massive BHs (SMBHs).…”

Section: Average Bh Mass Evaluationmentioning

confidence: 99%

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Is the cosmological constant of topological origin?

Delliou

Espiro

2020

Physics of the Dark Universe

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The observed value of the cosmological constant poses large theoretical problems. We find that topology of the Universe provides a natural source for it. Restricting dynamically an Einstein-Cartan gravity to General Relativity in our observed Universe allows topological invariants to induce an effective cosmological constant from dynamical quintessence-like topological fields. Its evaluation through the boundary of black holes yields a range compatible with the observed value, with uncertainty of three orders of magnitude. In turns, it provides a measurement of the Universe's isoperimetric constant.

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Section: Discussionsupporting

confidence: 62%

Section: Average Bh Mass Evaluationmentioning

confidence: 99%

Is the cosmological constant of topological origin?

Delliou

Espiro

2020

Physics of the Dark Universe

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“…These values are indicated in Table 7, and are indeed about 1-30 times (on average 4 times) below the previous ones. (3) 6.60±.3 42.8 N1433 6.61±.37 7.24±.4 (4) -40.0 N1566 7.11±.32 6.48±.2 (5) 6.83±.3 41.4 N1672 7.08±.9 6.00±.6 (6) 7.70±.1 39.3 N1808 6.74±.35 7.20±.6 (7) -40.6 N1068 6.93±.37 7.15±.1 (8) 7.17±.2 44.7 Column 2 lists BH masses estimated from the spiral pitch angle (Davis et al 2014), except for NGC 1326, from the Sersic index (Mutlu-Pakdil et al 2016). Column 3 is from other estimations:…”

Section: Model Of the Gravitational Potentialmentioning

confidence: 99%

ALMA observations of molecular tori around massive black holes

Combes

García‐Burillo

Audibert

et al. 2019

A&A

208

243

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We report Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO(3-2) emission in a sample of seven Seyfert/LINER galaxies at the unprecedented spatial resolution of 0 . 1 = 4-9 pc. Our aim is to explore the close environment of active galactic nuclei (AGN), and the dynamical structures leading to their fueling, through the morphology and kinematics of the gas inside the sphere of influence of the black hole. The selected galaxies host low-luminosity AGN and have a wide range of activity types (Seyferts 1 to 2, LINERs), and barred or ringed morphologies. The observed maps reveal the existence of circumnuclear disk structures, defined by their morphology and decoupled kinematics, in most of the sample. We call these structures molecular tori, even though they often appear as disks without holes in the center. They have varying orientations along the line of sight, unaligned with the host galaxy orientation. The radius of the tori ranges from 6 to 27 pc, and their mass from 0.7 × 10 7 to 3.9 × 10 7 M . The most edge-on orientations of the torus correspond to obscured Seyferts. In only one case (NGC 1365), the AGN is centered on the central gas hole of the torus. On a larger scale, the gas is always piled up in a few resonant rings 100 pc in scale that play the role of a reservoir to fuel the nucleus. In some cases, a trailing spiral is observed inside the ring, providing evidence for feeding processes. More frequently, the torus and the AGN are slightly off-centered with respect to the bar-resonant ring position, implying that the black hole is wandering by a few 10 pc amplitude around the center of mass of the galaxy. Our spatial resolution allows us to measure gas velocities inside the sphere of influence of the central black holes. By fitting the observations with different simulated cubes, varying the torus inclination and the black hole mass, it is possible to estimate the mass of the central black hole, which is in general difficult for such late-type galaxies, with only a pseudo-bulge. In some cases, AGN feedback is revealed through a molecular outflow, which will be studied in detail in a subsequent article.

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“…d Black hole mass derived from dynamical gas measurements by Combes et al (2019), who report on Atacama Large Millimeter/submillimeter Array observations of molecular tori around active galactic nuclei. e New pitch angle measurement using 2dfft (Davis et al 2012(Davis et al , 2016, spirality (Shields et al 2015a,b), and/or sparcfire Forty-two galaxies out of our total sample of 48 galaxies have v max measurements in the literature. These are mostly (29 out of 42) from the HyperLeda database 7 (Paturel et al 2003), which provides homogenized maximum rotational velocities calculated from the 21 cm line maximum widths (W max ) or available rotation curves (generally Hα rotation curves).…”

Section: Datamentioning

confidence: 99%

A Consistent Set of Empirical Scaling Relations for Spiral Galaxies: The (v_max, M_oM)–(σ₀, M_BH, ϕ) Relations

Davis

Graham

Combes

2019

ApJ

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Using the latest sample of 48 spiral galaxies having a directly measured supermassive black hole mass, M BH , we determine how the maximum disk rotational velocity, v max (and the implied dark matter halo mass, M DM ), correlates with the (i) black hole mass, (ii) central velocity dispersion, σ 0 , and (iii) spiral-arm pitch angle, φ. We find that M BH ∝ v 10.62±1.37 max ∝ M 4.35±0.66 DM , significantly steeper than previously reported, and with a total root mean square scatter (0.58 dex) similar to that about the M BH -σ 0 relation for spiral galaxies-in stark disagreement with claims that M BH does not correlate with disks. Moreover, this M BH -v max relation is consistent with the unification of the Tully-Fisher relation (involving the total stellar mass, M * ,tot ) and the steep M BH ∝ M 3.05±0.53 * ,tot relation observed in spiral galaxies. We also find that DM, consistent with past studies connecting stellar bulges (with σ 0 100 km s −1 ), dark matter halos, and a nonconstant v max /σ 0 ratio. Finally, we report that tan |φ| ∝ (−1.18 ± 0.19) log v max ∝ (−0.48 ± 0.09) log M DM , providing a novel formulation between the geometry (i.e., the logarithmic spiral-arm pitch angle) and kinematics of spiral galaxy disks. While the v max -φ relation may facilitate distance estimations to face-on spiral galaxies through the Tully-Fisher relation and using φ as a proxy for v max , the M DM -φ relation provides a path for determining dark matter halo masses from imaging data alone. Furthermore, based on a spiral galaxy sample size that is double the size used previously, the self-consistent relations presented here provide dramatically revised constraints for theory and simulations.4 If we calculate the Tully-Fisher relation from our dataset, we find that M * ,tot ∝ v 3.94±1.01 rot , which is consistent with Equation (1) at the level of 0.05 σ. 5 The dynamics of newly assembled massive objects (DY-NAMO) project (Green et al. 2010(Green et al. , 2014Bassett et al. 2014) demonstrated that their more local (z ∼ 0.1) sample of galaxies, selected to have high star-formation rates, are analogs of turbulent z 2 disk galaxies, with similar vrot/σ 0 ratios. 46 The quantity vmax should not be confused with the circular rotation velocity of the disk of our Galaxy at the location of the Sun and equal to (238 ± 15) km s −1 (Bland-Hawthorn & Gerhard 2016) or (229.0 ± 0.2) km s −1 (Eilers et al. 2019).

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THE LOCAL BLACK HOLE MASS FUNCTION DERIVED FROM THE M_BH–P AND THE M_BH–n RELATIONS

Cited by 39 publications

References 59 publications

Is the cosmological constant of topological origin?

Is the cosmological constant of topological origin?

ALMA observations of molecular tori around massive black holes

A Consistent Set of Empirical Scaling Relations for Spiral Galaxies: The (v_max, M_oM)–(σ₀, M_BH, ϕ) Relations

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THE LOCAL BLACK HOLE MASS FUNCTION DERIVED FROM THE MBH–P AND THE MBH–n RELATIONS

Cited by 39 publications

References 59 publications

Is the cosmological constant of topological origin?

Is the cosmological constant of topological origin?

ALMA observations of molecular tori around massive black holes

A Consistent Set of Empirical Scaling Relations for Spiral Galaxies: The (vmax, MoM)–(σ0, MBH, ϕ) Relations

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Product

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THE LOCAL BLACK HOLE MASS FUNCTION DERIVED FROM THE M_BH–P AND THE M_BH–n RELATIONS

A Consistent Set of Empirical Scaling Relations for Spiral Galaxies: The (v_max, M_oM)–(σ₀, M_BH, ϕ) Relations