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

Abstract

We present a determination of the supermassive black hole (SMBH) mass function for early-and latetype galaxies in the nearby universe (z < 0.0057), established from a volume-limited sample consisting of a statistically complete collection of the brightest spiral galaxies in the southern hemisphere. The sample is defined by limiting luminosity (redshift-independent) distance, D L = 25.4 Mpc, and a limiting absolute B-band magnitude, M B = −19.12. These limits define a sample of 140 spiral, 30 elliptical (E), and 38 lenticular (S0) galaxies. We established the Sérsic index distribution for earlytype (E/S0) galaxies in our sample. Davis et al. (2014) established the pitch angle distribution for their sample, which is identical to our late-type (spiral) galaxy sample. We then used the pitch angle and the Sérsic index distributions in order to estimate the SMBH mass function for our volume-limited sample. The observational simplicity of our approach relies on the empirical relation between the mass of the central SMBH and the Sérsic index ) for an early-type galaxy or the logarithmic spiral arm pitch angle (Berrier et al. 2013) for a spiral galaxy. Our SMBH mass function agrees well at the high-mass end with previous values in the literature. At the low-mass end, while inconsistencies exist in previous works that still need to be resolved, our work is more in line with expectations based on modeling of black hole evolution.

Is the cosmological constant of topological origin?

“…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].…”

“…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).…”

ALMA observations of molecular tori around massive black holes

“…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:…”

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

“…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).…”