Planetary camera observations of the central parsec of M32

Lauer, Tod R.; Faber, S. M.; Currie, D. G.; Ewald, S. P.; Groth, Edward J.; Hester, J. J.; Holtzman, Jon A.; Light, R. M.; O'Neill, Earl J.; Shaya, E.; Westphal, James A.

doi:10.1086/116254

Cited by 74 publications

(79 citation statements)

References 20 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The deprojection does not strongly constrain the central slope of the density profile. In Figure 2, we used F r Ϫ1.53 (Lauer et al 1992). However, we also calculated a set of models with F r Ϫ1.63 .…”

Section: Resultsmentioning

confidence: 99%

See 1 more Smart Citation

Improved Evidence for a 3 × 10[TSUP]6[/TSUP] [ITAL]M[/ITAL][TINF]⊙[/TINF] Black Hole in M32: Canada-France-Hawaii Telescope Spectroscopy with FWHM = 0[farcs]47 Resolution

Bender¹,

Kormendy²,

Dehnen³

1996

The Astrophysical Journal

View full text Add to dashboard Cite

We present improved spectroscopy of M32 with the Canada-France-Hawaii Telescope and Subarcsecond Imaging Spectrograph. Tip-tilt guiding provides a resolution of FWHM ϭ 0"47 or * ϭ 0"20 ( * ϭ Gaussian dispersion radius of the point-spread function). The observed central velocity dispersion, 3 92 H 5 km s Ϫ1 , and the maximum rotation velocity, V max ϭ 55 H 3 km s Ϫ1 , are larger than at lower resolution. In addition, the measured line-of-sight velocity distributions indicate the possible presence of broad wings at radii r = 0"2, with significant numbers of stars at ⌬V 3 200 km s Ϫ1 from the mean velocity. Two-integral dynamical models fit these data provided that M32 contains a central dark object, probably a black hole, of mass M q 3 (3.0 H 0.5) ϫ 10 6 M J . This confirms detections based on lower resolution spectra by Tonry, Dressler, Richstone, van der Marel, Dehnen, and collaborators. The available spatial resolution has now improved by a factor of 3 since Tonry's discovery observations; each improvement in resolution has strengthened the case for a black hole in M32.

show abstract

Section: Resultsmentioning

confidence: 99%

“…In this respect, M32 is a better than average case. Hubble Space Telescope photometry by Lauer et al (1992) shows that any core has a radius of less than 0.37 pc and that the stellar density reaches * Ͼ 3 ϫ 10 7 M J pc Ϫ3 . The relaxation and stellar collision times are short.…”

Section: Introductionmentioning

confidence: 99%

Improved Evidence for a 3 × 10[TSUP]6[/TSUP] [ITAL]M[/ITAL][TINF]⊙[/TINF] Black Hole in M32: Canada-France-Hawaii Telescope Spectroscopy with FWHM = 0[farcs]47 Resolution

Bender¹,

Kormendy²,

Dehnen³

1996

The Astrophysical Journal

View full text Add to dashboard Cite

show abstract

“…The Milky Way data are from the model by Genzel et al (1996). The Nuker parameters for M32 are taken from Lauer et al (1992). For M31 we ®tted the photometry ourselves using data from Lauer et al (1993) (r < 10 arcsec) and Kent (1987) (r > 10 arcsec), matching at r 10 arcsec.…”

Section: T H E N U K E R G a L A X I E Smentioning

confidence: 99%

Tidal disruption rates of stars in observed galaxies

Syer

Ulmer

1999

Monthly Notices of the Royal Astronomical Society

154

190

View full text Add to dashboard Cite

We derive the rates of capture, Ndot, of main sequence turn off stars by the central massive black hole in a sample of galaxies from Magorrian et al. 1998. The disruption rates are smaller than previously believed with Ndot ~ 10^-4 - 10^-7 per galaxy. A correlation between Ndot and black hole mass, M, is exploited to estimate the rate of tidal disruptions in the local universe. Assuming that all or most galaxies have massive black holes in their nuclei, this rate should be dominated by sub-Lstar galaxies. The rate of tidal disruptions could be high enough to be detected in supernova (or similar) monitoring campaigns---we estimate the rate of tidal disruptions to be 0.01 - 0.1 times the supernova rate. We have also estimated the rates of disruption of red giants, which may be significant (Ndot ~> 10^-4 y^-1 per galaxy) for M ~> 10^8 Msun, but are likely to be harder to observe---only of order 10^-4 times the supernova rate in the local universe. In calculating capture rates, we advise caution when applying scaling formulae by other authors, which are not applicable in the physical regime spanned by the galaxies considered here.Comment: MNRAS, Accepted; 9 pages, Late

show abstract

“…Ground-based kinematic measurements of this galaxy (Tonry 1984(Tonry , 1987 have already shown a steep gradient in the central velocity profile and a central dispersion peak, suggesting the presence of a central compact object, presumably a supermassive black hole. Since then, (spectroscopic) observations with increasing spatial resolution, both ground-based (Dressler & Richstone 1988;van der Marel et al 1994a;Bender, Kormendy & Dehnen 1996) and with HST (Lauer et al 1992;Joseph et al 2001), have strengthened the case for this black hole.…”

Section: Introductionmentioning

confidence: 97%

A SAURON study of M32: measuring the intrinsic flattening and the central black hole mass

Verolme

Cappellari

Copin

et al. 2002

Monthly Notices of the Royal Astronomical Society

169

170

View full text Add to dashboard Cite

We present dynamical models of the nearby compact elliptical galaxy M32, using high‐quality kinematic measurements, obtained with the integral‐field spectrograph SAURON mounted on the William Herschel Telescope on La Palma. We also include STIS data obtained previously by Joseph et al. We find a best‐fitting black hole mass of M•= (2.5 ± 0.5) × 106 M⊙ and a stellar I‐band mass‐to‐light ratio of (1.85 ± 0.15) M⊙/L⊙. For the first time, we are also able to constrain the inclination along which M32 is observed to 70°± 5°. Assuming that M32 is indeed axisymmetric, the averaged observed flattening of 0.73 then corresponds to an intrinsic flattening of 0.68 ± 0.03. These tight constraints are mainly caused by the use of integral‐field data. We show this quantitatively by comparing with models that are constrained by multiple slits only. We show the phase‐space distribution and intrinsic velocity structure of the best‐fitting model and investigate the effect of regularization on the orbit distribution.

show abstract

Planetary camera observations of the central parsec of M32

Cited by 74 publications

References 20 publications

Improved Evidence for a 3 × 10[TSUP]6[/TSUP] [ITAL]M[/ITAL][TINF]⊙[/TINF] Black Hole in M32: Canada-France-Hawaii Telescope Spectroscopy with FWHM = 0[farcs]47 Resolution

Improved Evidence for a 3 × 10[TSUP]6[/TSUP] [ITAL]M[/ITAL][TINF]⊙[/TINF] Black Hole in M32: Canada-France-Hawaii Telescope Spectroscopy with FWHM = 0[farcs]47 Resolution

Tidal disruption rates of stars in observed galaxies

A SAURON study of M32: measuring the intrinsic flattening and the central black hole mass

Contact Info

Product

Resources

About