Evidence for a Massive Black Hole in the S0 Galaxy NGC 4342

Cretton, Nicolas; Bosch, Frank C. van den

doi:10.1086/306971

Cited by 114 publications

(142 citation statements)

References 75 publications

Supporting

Mentioning

133

Contrasting

Order By: Relevance

“…NGC 4342.-Both the velocity dispersion and the black hole mass are from Cretton & van den Bosch (1999).…”

Section: Comments On Individual Galaxiesmentioning

confidence: 99%

“…- (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%

See 1 more Smart Citation

The Slope of the Black Hole Mass versus Velocity Dispersion Correlation

Tremaine

Gebhardt

Bender³

et al. 2002

ApJ

2,472

166

3,186

View full text Add to dashboard Cite

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.

show abstract

“…NGC 4342.-Both the velocity dispersion and the black hole mass are from Cretton & van den Bosch (1999).…”

Section: Comments On Individual Galaxiesmentioning

confidence: 99%

Section: Slope Estimationmentioning

confidence: 99%

The Slope of the Black Hole Mass versus Velocity Dispersion Correlation

Tremaine

Gebhardt

Bender³

et al. 2002

ApJ

2,472

166

3,186

View full text Add to dashboard Cite

show abstract

“…§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

View full text Add to dashboard Cite

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.

show abstract

“…Such host galaxy environments have not been extensively explored on the black hole-host galaxy relationships. Besides NGC 1277, only the compact galaxies NGC 1332 (Rusli et al 2011), NGC 4342 (Cretton & van den Bosch 1999), NGC 4486B (Kormendy et al 1997), and M60-UCD1 (Seth et al 2014) have dynamical black hole mass measurements, with NGC 1332 and NGC 4342 being most like NGC 1277. For these galaxies, the black hole mass measurements are in agreement with M BH -s  , given the intrinsic scatter of the relation, but are positive outliers from the M BH -L bul relation (Kormendy & Ho 2013).…”

Section: Introductionmentioning

confidence: 99%

The Black Hole in the Compact, High-Dispersion Galaxy NGC 1271

Walsh

Bosch

Gebhardt

et al. 2015

ApJ

View full text Add to dashboard Cite

Located in the Perseus cluster, NGC 1271 is an early-type galaxy with a small effective radius of 2.2 kpc and a large bulge stellar velocity dispersion of 276 km s −1 for its K-band luminosity of L 8.9 10 10  . We present a mass measurement for the black hole in this compact, high-dispersion galaxy using observations from the Near-infrared Integral Field Spectrometer on the Gemini North telescope assisted by laser guide star adaptive optics, large-scale integral field unit observations with PPAK at the Calar Alto Observatory, and Hubble Space Telescope WFC3 imaging observations. We are able to map out the stellar kinematics both on small spatial scales, within the black hole sphere of influence, and on large scales that extend out to four times the galaxy's effective radius. We find that the galaxy is rapidly rotating and exhibits a sharp rise in the velocity dispersion. Through the use of orbit-based stellar dynamical models, we determine that the black hole has a mass of M (3.0 ) 10 1.1 1.0 9 -+  and the H-band stellar mass-to-light ratio is 1.40 0.11 0.13 ¡ -+  (1s uncertainties). NGC 1271 occupies the sparsely populated upper end of the black hole mass distributionbut is very different from the brightest cluster galaxies (BCGs) and giant elliptical galaxies that are expected to host the most massive black holes. Interestingly, the black hole mass is an order of magnitude larger than expectations based on the galaxy's bulge luminositybut is consistent with the mass predicted using the galaxy's bulge stellar velocity dispersion. More compact, high-dispersion galaxies need to be studied using high spatial resolution observations to securely determine black hole masses, as there could be systematic differences in the black hole scaling relations between these types of galaxies and the BCGs/giant ellipticals, thereby implying different pathways for black hole and galaxy growth.

show abstract

Evidence for a Massive Black Hole in the S0 Galaxy NGC 4342

Cited by 114 publications

References 75 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

The Black Hole in the Compact, High-Dispersion Galaxy NGC 1271

Contact Info

Product

Resources

About