Evidence for a Supermassive Black Hole in the S0 Galaxy NGC 3245

Barth, Aaron J.; Sarzi, Marc; Rix, H. W.; Ho, Luis C.; Filippenko, A. V.; Sargent, W. L. W.

doi:10.1086/321523

Cited by 134 publications

(230 citation statements)

References 47 publications

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“…- (1 Gebhardt et al 2002;(7) J. Pinkney et al 2002, in preparation;(8) Bower et al 2001;(9) Greenhill & Gwinn 1997;(10) Sarzi et al 2001;(11) Kormendy et al 1996a;(12) Barth et al 2001b;(13) Kormendy et al 1998;(14) Gebhardt et al 2000b;(15) Herrnstein et al 1999;(16) Ferrarese, Ford, & Jaffe 1996;(17) Cretton & van den Bosch 1999;(18) Harms et al 1994;(19) Macchetto et al 1997;(20) M. E. Kaiser et al 2002, in preparation;(21) Ferrarese & Ford 1999;(22) (23) Cappellari et al 2002. the Milky Way (see x 4.3) and 5% uncertainties in the dispersions of external galaxies (see x 4.1), although the uncertainties in the dispersions of a few galaxies that we have not observed ourselves may be larger. Initially, we assume 0.33 dex rms uncertainties in the black hole masses, which yields 2 per degree of freedom of unity.…”

Section: Slope Estimationmentioning

confidence: 99%

The Slope of the Black Hole Mass versus Velocity Dispersion Correlation

Tremaine

Gebhardt

Bender³

et al. 2002

ApJ

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2,472

166

3,186

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Observations of nearby galaxies reveal a strong correlation between the mass of the central dark object M BH and the velocity dispersion of the host galaxy, of the form logðM BH =M Þ ¼ þ logð = 0 Þ; however, published estimates of the slope span a wide range (3.75-5.3). Merritt & Ferrarese have argued that low slopes (d4) arise because of neglect of random measurement errors in the dispersions and an incorrect choice for the dispersion of the Milky Way Galaxy. We show that these explanations and several others account for at most a small part of the slope range. Instead, the range of slopes arises mostly because of systematic differences in the velocity dispersions used by different groups for the same galaxies. The origin of these differences remains unclear, but we suggest that one significant component of the difference results from Ferrarese & Merritt's extrapolation of central velocity dispersions to r e =8 (r e is the effective radius) using an empirical formula. Another component may arise from dispersion-dependent systematic errors in the measurements. A new determination of the slope using 31 galaxies yields ¼ 4:02 AE 0:32, ¼ 8:13 AE 0:06 for 0 ¼ 200 km s À1 . The M BH -relation has an intrinsic dispersion in log M BH that is no larger than 0.25-0.3 dex and may be smaller if observational errors have been underestimated. In an appendix, we present a simple kinematic model for the velocity-dispersion profile of the Galactic bulge.

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Section: Slope Estimationmentioning

confidence: 99%

The Slope of the Black Hole Mass versus Velocity Dispersion Correlation

Tremaine

Gebhardt

Bender³

et al. 2002

ApJ

Self Cite

2,472

166

3,186

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“…§3) were consistent for these objects. In addition, we took the bulge masses for NGC1023 from Bower et al (2001), for NGC3245 from Barth et al (2001), for NGC4342 from Cretton and van den Bosch (1999) and for NGC3384, for NGC4697, for NGC5845 and for NGC7457 from Gebhardt et al (2003). The Milky Way is a special case, since the black hole mass is by far the most secure but the uncertainty in the bulge mass (mostly conceptual) is yet quite high.…”

Section: The Samplementioning

confidence: 99%

On the Black Hole Mass-Bulge Mass Relation

Haering¹,

Rix²

2004

ApJ

1,579

174

1,931

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We have re-examined the relation between the mass of the central black holes in nearby galaxies, M bh , and the stellar mass of the surrounding spheroid or bulge, M bulge . For a total of 30 galaxies bulge masses were derived through Jeans equation modeling or adopted from dynamical models in the literature. In stellar mass-to-light ratios the spheroids and bulges span a range of a factor of eight. The bulge masses were related to well-determined black hole masses taken from the literature. With these improved values for M bh , compared to Magorrian et al. (1998), and our redetermination of M bulge , we find the M bh − M bulge relation becomes very tight. We find M bh ∼ M 1.12±0.06 bulge with an observed scatter of 0.30 dex, a fraction of which can be attributed to measurement errors. The scatter in this relation is therefore comparable to the scatter in the relations of M bh with σ and the stellar concentration. These results confirm and refine the work of Marconi and Hunt (2003). For M bulge ∼ 5 × 10 10 M ⊙ the median black hole mass is 0.14% ± 0.04% of the bulge mass.

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“…If the velocity dispersion indeed provides support against gravity, the dispersion-supported mass would not be negligible since σ int ∼ V rot . In this case, unfortunately, it is not possible to apply simple recipes such as the asymmetric drift correction (see, e.g., Barth et al 2001), and we therefore rely only on a virial estimate. With σ int 200 km s −1 and r 0 = 2.8 kpc the dispersion-supported mass is M SMG,disp σ 2 int r 0 /G = 2.6×10 10 M , similar to the rotation-supported mass, as expected.…”

Section: The Submillimeter Galaxy Br 1202 Northmentioning

confidence: 99%

Strongly star-forming rotating disks in a complex merging system atz= 4.7 as revealed by ALMA

Carniani

Marconi

Biggs

et al. 2013

A&A

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We performed a kinematical analysis of the [CII] line emission of the BR 1202-0725 system at z ∼ 4.7 using ALMA science verification observations. The most prominent sources of this system are a quasar (QSO) and a submillimeter galaxy (SMG), separated by a projected distance of about ∼24 kpc and characterized by very high star formation rates, higher than ∼1000 M yr −1 . However, the ALMA observations reveal that these galaxies apparently have undisturbed rotating disks, which is at variance with the commonly accepted scenario in which strong star formation activity is induced by a major merger. We also detected faint components which, after spectral deblending, were spatially resolved from the main QSO and SMG emissions. The relative velocities and positions of these components are compatible with orbital motions within the gravitational potentials generated by the QSO host galaxy and the SMG, suggesting that they are smaller galaxies in interaction or gas clouds in accretion flows of tidal streams. Moreover, we did not find any clear spectral evidence for outflows caused by active galactic nuclei or stellar feedback. This suggests that the high star formation rates might be induced by interactions or minor mergers with these companions, which do not affect the large-scale kinematics of the disks, however. Alternatively, the strong star formation may be fueled by the accretion of pristine gas from the host halo. Our kinematical analysis also indicates that the QSO and the SMG have similar dynamical masses, mostly in the form of molecular gas, and that the QSO host galaxy and the SMG are seen close to face-on with slightly different disk inclinations: the QSO host galaxy is seen almost face-on (i ∼ 15 • ), while the SMG is seen at higher inclinations (i ∼ 25 • ). Finally, the ratio between the black hole mass of the QSO, obtained from new X-shooter spectroscopy, and the dynamical mass of the host galaxy is similar to value found in very massive local galaxies, suggesting that the evolution of black hole galaxy relations is probably better studied with dynamical than with stellar host galaxy masses.

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Evidence for a Supermassive Black Hole in the S0 Galaxy NGC 3245

Cited by 134 publications

References 47 publications

The Slope of the Black Hole Mass versus Velocity Dispersion Correlation

The Slope of the Black Hole Mass versus Velocity Dispersion Correlation

On the Black Hole Mass-Bulge Mass Relation

Strongly star-forming rotating disks in a complex merging system atz= 4.7 as revealed by ALMA

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