The central black hole mass of the high-σ but low-bulge-luminosity lenticular galaxy NGC 1332★ (original) (raw)
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An over-massive black hole in the compact lenticular galaxy NGC 1277
Nature, 2012
All massive galaxies likely have supermassive black holes at their centers, and the masses of the black holes are known to correlate with properties of the host galaxy bulge component 1 . Several explanations have been proposed for the existence of these locallyestablished empirical relationships; they include the non-causal, statistical process of galaxy-galaxy merging 2 , direct feedback between the black hole and its host galaxy 3 , or galaxy-galaxy merging and the subsequent violent relaxation and dissipation 4 . The empirical scaling relations are thus important for distinguishing between various theoretical models of galaxy evolution 5, 6 , and they further form the basis for all black hole mass measurements at large distances. In particular, observations have shown that the mass of the black hole is typically 0.1% of the stellar bulge mass of the galaxy 7, 8 . The small galaxy NGC 4486B currently has the largest published fraction of its mass in a black hole at 11 per cent 1, 9 . Here we report observations of the stellar kinematics of NGC 1277, which is a compact, disky galaxy with a mass of 1.2 × 10 11 M . From the data, we determine that the mass of the central black hole is 1.7 × 10 10 M , or 59% its bulge mass. Five other compact galaxies have properties similar to NGC 1277 and therefore may also contain over-sized black holes. It is not yet known if these galaxies represent a tail of a distribution, or if disk-dominated galaxies fail to follow the normal black hole mass scaling relations 4, 10 .
Dynamical Measurements of Black Hole Masses in Four Brightest Cluster Galaxies at 100 Mpc
2012
We present stellar kinematics and orbit superposition models for the central regions of four brightest cluster galaxies, based upon integral-field spectroscopy at Gemini, Keck, and McDonald Observatories. Our integral-field data span radii from <100 pc to tens of kiloparsecs, comparable to the effective radius of each galaxy. We report black hole masses, M • , of 2.1 +1.6 −1.6 × 10 10 M for NGC 4889, 9.7 +3.0 −2.5 × 10 9 M for NGC 3842, and 1.3 +0.5 −0.4 × 10 9 M for NGC 7768, with errors representing 68% confidence limits. For NGC 2832, we report an upper limit of M • < 9.0 × 10 9 M . Our models of each galaxy include a dark matter halo, and we have tested the dependence of M • on the model dark matter profile. Stellar orbits near the center of each galaxy are tangentially biased, on comparable spatial scales to the galaxies' photometric cores. We find possible photometric and kinematic evidence for an eccentric torus of stars in NGC 4889, with a radius of nearly 1 kpc. We compare our measurements of M • to the predicted black hole masses from various fits to the relations between M • and stellar velocity dispersion (σ ), luminosity (L), or stellar mass (M ). Still, the black holes in NGC 4889 and NGC 3842 are significantly more massive than all σ -based predictions and most L-based predictions. The black hole in NGC 7768 is consistent with a broader range of predictions.
The Astronomical Journal, 1998
This paper is a study of the mass distribution in the central 35 ′′ ≃ 1.7 kpc of the E5 galaxy NGC 3377. Stellar rotation velocity and velocity dispersion profiles (seeing σ * = 0. ′′ 20-0. ′′ 56) and V-band surface photometry (σ * = 0. ′′ 20-0. ′′ 26) have been obtained with the Canada-France-Hawaii Telescope. NGC 3377 is kinematically similar to M 32: the central kinematic gradients are steep. There is an unresolved central rise in rotation velocity to V = 110 ± 3 km s −1 (internal error) at r = 1. ′′ 0. The apparent velocity dispersion rises from 95 ± 2 km s −1 at 1. ′′ 0 ≤ r < 4 ′′ to 178 ± 10 km s −1 at the center. To search for a central black hole, we derive three-dimensional velocity and velocity dispersion fields that fit the above observations and Hubble Space Telescope surface photometry after projection and seeing convolution. Isotropic models imply that the mass-to-light ratio rises by a factor of ∼ 4 at r < 2 ′′ to M/L V > ∼ 10. If the mass-to-light ratio of the stars, M/L V = 2.4 ± 0.2, is constant with radius, then NGC 3377 contains a central massive dark object (MDO), probably a black hole, of mass M • ≃ (1.8 ± 0.8) × 10 8 M ⊙. Several arguments suggest that NGC 3377 is likely to be nearly isotropic. However, flattened, anisotropic maximum entropy models can fit the present data without an MDO. Therefore the MDO detection in NGC 3377 is weaker than those in M 31, M 32, and NGC 3115. The above masses are corrected for the E5 shape of the galaxy and for the difference between velocity moments and velocities given by Gaussian fits to the line profiles. We show that the latter correction does not affect the strength of the MDO detection, but it slightly reduces M
Monthly Notices of the Royal Astronomical Society, 2006
We combine Hubble Space Telescope spectroscopy and ground-based integral-field data from the SAURON and OASIS instruments to study the central black hole in the nearby elliptical galaxy NGC 3379. From these data, we obtain kinematics of both the stars and the nuclear gaseous component. Axisymmetric three-integral models of the stellar kinematics find a black hole of mass 1.4 +2.6 −1.0 × 10 8 M (3σ errors). These models also probe the velocity distribution in the immediate vicinity of the black hole and reveal a nearly isotropic velocity distribution throughout the galaxy and down to the black hole sphere of influence R BH . The morphology of the nuclear gas disc suggests that it is not in the equatorial plane; however the core of NGC 3379 is nearly spherical. Inclined thin-disc models of the gas find a nominal black hole of mass (2.0 ± 0.1) × 10 8 M (3σ errors), but the model is a poor fit to the kinematics. The data are better fit by introducing a twist in the gas kinematics (with the black hole mass assumed to be 2.0 × 10 8 M ), although the constraints on the nature and shape of this perturbation are insufficient for more detailed modelling. Given the apparent regularity of the gas disc appearance, the presence of such strong non-circular motion indicates that caution must be used when measuring black hole masses with gas dynamical methods alone.
A Comparison of Supermassive Black Hole Mass of NGC 4151 Using Different Methods
passer
We found a new value of supermassive black hole (SMBH) mass in the middle of type 1 Seyfert, NGC 4151 galaxy. In this Study, the image of NGC 4151 galaxy was deprojected to face-on, using spiral galaxy of face-on, and applied IRAF to calculate the ellipticity and position angle of major-axis. A two-dimensional (2D) Fast Fourier Transform (FFT) applied to the deprojected image to calculate the spiral arm of NGC 4151 galaxy, and, in that way, find a central mass AGN 4151 galaxy. We compared our results of the mass of SMBH in in the center of NGC 4151 galaxy with the mass of SMBH calculated using different methods ((direct method: stellar dynamics, gas dynamics, reverberation mapping), and indirect method: MBH-σ*, MBH-Vrot, MBH-n, MBH-Lbulge, and MBH-P correlations). We concluded that the results of mass for these methods are in agreement with the estimated ones, i.e. using direct methods.
Mon Notic Roy Astron Soc, 2005
We present Space Telescope Imaging Spectrograph emission-line spectra of the central regions of the spiral galaxies NGC 1300 and NGC 2748. From the derived kinematics of the nuclear gas we have found evidence for central supermassive black holes in both galaxies. The estimated mass of the black hole in NGC 1300 is 6.6 (+6.3, -3.2) x 10^7 solar masses and in NGC 2748 is 4.4 (+3.5, -3.6) x 10^7 solar masses (both at the 95% confidence level). These two black hole mass estimates contribute to the poorly sampled low-mass end of the nuclear black hole mass spectrum.
The Black Hole Mass and Extreme Orbital Structure in NGC 1399
The Astrophysical Journal, 2007
The largest galaxies, and in particular central galaxies in clusters, offer unique insight into understanding the mechanism for the growth of nuclear black holes. We present Hubble Space Telescope kinematics for NGC 1399, the central galaxy in Fornax. We find the best-fit model contains a black hole of (5.1 ± 0.7) × 10 8 M ⊙ (at a distance of 21.1 Mpc), a factor of over 2 below the correlation of black hole mass and velocity dispersion. We also find a dramatic signature for central tangential anisotropy. The velocity profiles on adjacent sides 0.5 ′′ away from the nucleus show strong bimodality, and the central spectrum shows a large drop in the dispersion. Both of these observations point to an orbital distribution that is tangentially biased. The best-fit orbital model suggests a ratio of the tangential to radial internal velocity dispersions of three. This ratio is the largest seen in any galaxy to date and will provide an important measure for the mode by which the central black hole has grown.
The Astrophysical Journal, 2007
Black hole masses predicted from the M • − σ relationship conflict with those predicted from the M • − L relationship for the most luminous galaxies, such as brightest cluster galaxies (BCGs). This is because stellar velocity dispersion, σ, increases only weakly with luminosity for BCGs and other giant ellipticals. The M • − L relationship predicts that the most luminous BCGs may harbor black holes with M • approaching 10 10 M ⊙ , while the M • − σ relationship always predicts M • < 3 × 10 9 M ⊙ . Lacking direct determination of M • in a sample of the most luminous galaxies, we advance arguments that the M • − L relationship is a plausible or even preferred description for BCGs and other galaxies of similar luminosity. Under the hypothesis that cores in central stellar density are formed by binary black holes, the inner-core cusp radius, r γ , may be an independent witness of M • . Using central structural parameters derived from a large sample of early-type galaxies observed by HST, we argue that L is superior to σ as an indicator of r γ in luminous galaxies. Further, the observed r γ − M • relationship for 11 core galaxies with measured M • appears to be consistent with the M • − L relationship for BCGs. BCGs have large cores appropriate for their large luminosities that may be difficult to generate with the more modest black hole masses inferred from the M • − σ relationship. M • ∼ L may be expected to hold for BCGs, if they were formed in dissipationless mergers, which should preserve ratio of black hole to stellar mass. This picture appears to be consistent with the slow increase in σ with L and the more rapid increase in effective radii, R e , with L seen in BCGs as compared to less luminous galaxies. If BCGs have large BHs commensurate with their high luminosities, then the local black hole mass function for M • > 3 × 10 9 M ⊙ may be nearly an order of magnitude richer than what would be inferred from the M • − σ relationship. The volume density of the most luminous QSOs at earlier epochs may favor the predictions from the M • − L relationship.