Black Hole Mass Scaling Relations for Early-type Galaxies. I. M BH–M *, sph and M BH–M *,gal

  title={Black Hole Mass Scaling Relations for Early-type Galaxies. I. M BH–M *, sph and M BH–M *,gal},
  author={Nandini Sahu and Alister W. Graham and Benjamin Lee Davis},
  journal={The Astrophysical Journal},
Analyzing a sample of 84 early-type galaxies with directly-measured super-massive black hole masses---nearly doubling the sample size of such galaxies with multi-component decompositions---a symmetric linear regression on the reduced (merger-free) sample of 76 galaxies reveals $M_{BH}\propto M_{*,sph}^{1.27\pm 0.07}$ with a total scatter of $\Delta_{rms}=$ 0.52 dex in the $\log(M_{BH})$ direction. However, and importantly, we discover that the ES/S0-type galaxies with disks are offset from the… 
The Black Hole Mass–Color Relations for Early- and Late-type Galaxies: Red and Blue Sequences
[Abridged] Tight correlations between supermassive black hole (SMBH) mass ($M_{\rm BH}$) and the properties of the host galaxy have useful implications for our understanding of the growth of SMBHs
The Black Hole–Bulge Mass Relation Including Dwarf Galaxies Hosting Active Galactic Nuclei
We present a new relationship between central black hole (BH) mass and host galaxy stellar bulge mass extending to the lowest BH masses known in dwarf galaxies ($M_{\rm BH} \lesssim 10^{5}
Revealing Hidden Substructures in the M BH–σ Diagram, and Refining the Bend in the L–σ Relation
Using 145 early- and late-type galaxies (ETGs and LTGs) with directly-measured super-massive black hole masses, $M_{BH}$, we build upon our previous discoveries that: (i) LTGs, most of which have
Defining the (Black Hole)–Spheroid Connection with the Discovery of Morphology-dependent Substructure in the M BH–n sph and M BH–R e,sph Diagrams: New Tests for Advanced Theories and Realistic Simulations
For 123 local galaxies with directly-measured black hole masses (MBH), we provide the host spheroid’s Sérsic index (nsph), effective half-light radius (Re,sph), and effective surface brightness (μe),
Probing black hole accretion tracks, scaling relations, and radiative efficiencies from stacked X-ray active galactic nuclei
The masses of supermassive black holes at the centres of local galaxies appear to be tightly correlated with the mass and velocity dispersions of their galactic hosts. However, the local M_bh–M_star
Central X-Ray Point Sources Found to Be Abundant in Low-mass, Late-type Galaxies Predicted to Contain an Intermediate-mass Black Hole
Building upon three late-type galaxies in the Virgo cluster with both a predicted black hole mass of less than ∼105 M ⊙ and a centrally located X-ray point source, we reveal 11 more such galaxies,
Constraining black hole-galaxy scaling relations from the large-scale clustering of Active Galactic Nuclei and implied mean radiative efficiency
A supermassive black hole has been found at the centre of nearly every galaxy observed with sufficient sensitivity. The masses of these black holes are observed to increase with either the total mass
Constraining black hole–galaxy scaling relations and radiative efficiency from galaxy clustering
The masses of supermassive black holes are observed to increase with either the total mass or the mean (random) velocity of the stars in their host galaxies. The origin of these correlations remains
Coevolution of black hole accretion and star formation in galaxies up to z = 3.5
Aims. We study the coevolution between the black hole accretion rate (BHAR) and the star formation rate (SFR) in different phases of galaxy life: main-sequence star-forming galaxies, quiescent
No Significant Evolution of Relations between Black Hole Mass and Galaxy Total Stellar Mass Up to z ∼ 2.5
We investigate the cosmic evolution of the ratio between black hole mass (MBH) and host galaxy total stellar mass (Mstellar) out to z~2.5 for a sample of 100 X-ray-selected moderate-luminosity,


The Most Precise Extra-Galactic Black-Hole Mass Measurement
I use archival data to measure the mass of the central black hole in NGC 4526, M = (4.70 +- 0.14) X 10^8 Msun. This 3% error bar is the most precise for an extra-galactic black hole and is close to
Gravitational wave research using pulsar timing arrays
A pulsar timing array (PTA) refers to a program of regular, high-precision timing observations of a widely distributed array of millisecond pulsars. Here we review the status of the three primary PTA
2007a, in American Astronomical Society
  • Meeting Abstracts,
  • 2007
Elliptical Galaxies With Nuclear Disks of Stars: Black Hole Search and Stellar Populations, HST Proposal
  • 2000
1987b, in Structure and Dynamics of Elliptical Galaxies, ed
  • 1987
Planck 2018 results
  • 2020
Spectroscopy of the Rapidly Rotating Nuclear Disk in the Virgo s0 NGC4526, HST Proposal
  • 1995
PASA, 33, e062, doi: 10.1017/pasa.2016.60 Ciotti, L
  • A&A,
  • 2016