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

Verolme, E. K.; Cappellari, Michele; Copin, Y.; Marel, Roeland P. van der; Bacon, Roland; Bureau, Martin; Davies, Roger L.; Miller, Bryan; Zeeuw, P. T. de

doi:10.1046/j.1365-8711.2002.05664.x

Cited by 170 publications

(189 citation statements)

References 52 publications

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“…On the other hand, McLaughlin & King (2006) point out that feedback by stellar winds and supernovae may also be capable of reproducing the observed scaling relations without a direct connection between the nuclei and SBHs. And, as Ferrarese et al (2006b) note, there are at least some galaxies (such as M32) that contain both a central excess (Worthey 2004) and a SBH (Verolme et al 2002).…”

Section: Discussionmentioning

confidence: 99%

The ACS Fornax Cluster Survey. II. The Central Brightness Profiles of Early-Type Galaxies: A Characteristic Radius on Nuclear Scales and the Transition from Central Luminosity Deficit to Excess

Côté

Ferrarese

Jordán

et al. 2008

ApJ

112

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We analyze brightness profiles for 143 early-type galaxies in the Virgo and Fornax Clusters, observed with the Advanced Camera for Surveys on the Hubble Space Telescope. Sérsic models are found to provide accurate representations of the global profiles with a notable exception: the observed profiles deviate systematically inside a characteristic ''break'' radius of R b % 0:02 þ0:025 À0:01 R e , where R e is the effective radius of the galaxy. The sense of the deviation is such that bright galaxies (M B P À 20) typically show central light deficits with respect to the inward extrapolation of the Sérsic model, while the great majority of low-and intermediate-luminosity galaxies (À19:5 P M B P À 15) show central light excesses; galaxies of intermediate luminosities (À20 P M B P À 19:5) are generally well fitted by Sérsic models over all radii. We show that the slope, 0 , of the central surface brightness profiles, when measured at fixed fractions of R e , varies smoothly as a function of galaxy luminosity in a manner that depends sensitively on the choice of measurement radius. We find no evidence for a core/power-law dichotomy, and show that a recent claim of strong bimodality in 0 is likely an artifact of the biased galaxy selection function used in that study. To provide a more robust characterization of the inner regions of galaxies, we introduce a parameterwhere L g and L S are the integrated luminosities inside 0:02R e of the observed profile and of the inward extrapolation of the outer Sérsic model -to describe the central luminosity deficit (Á 0:02 < 0) or excess (Á 0:02 > 0). We find that Á 0:02 varies smoothly over the range of %720 in luminosity spanned by the sample galaxies, with again no evidence for a dichotomy. We argue that the central light excesses in M B k À 19 galaxies may be the analogs of the dense central cores predicted by some numerical simulations to form via gas inflows.

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Section: Discussionmentioning

confidence: 99%

The ACS Fornax Cluster Survey. II. The Central Brightness Profiles of Early-Type Galaxies: A Characteristic Radius on Nuclear Scales and the Transition from Central Luminosity Deficit to Excess

Côté

Ferrarese

Jordán

et al. 2008

ApJ

112

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“…M32 is the third galaxy in the Local Group known to possess a massive black hole; its mass, M BH = (2.5 ± 0.5) × 10 6 M ⊙ (Verolme et al 2002), is essentially identical to that of the Galactic Center. As mentioned in the Introduction, all previous studies have failed to detect emission unambiguously associated with accretion onto the central black hole.…”

Section: M32 In Contextmentioning

confidence: 99%

Detection of the “Active” Nucleus of M32

Terashima

Ulvestad

2003

ApJ

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M32 hosts a 2.5×10 6 M ⊙ central black hole, but signs of nuclear activity in this galaxy have long eluded detection. We report the first conclusive detection of the nucleus of M32 in X-rays, based on high-resolution, sensitive observations made with Chandra. The 2-10 keV luminosity is merely 9.4×10 35 erg s −1 , ∼ 3 × 10 −9 of the Eddington luminosity of the black hole. Weak diffuse emission, consistent with thermal gas at a temperature of 0.37 keV, is seen in an annular region ∼100 pc from the center. We also present a deep, moderately high-resolution (0. ′′ 9), radio continuum observation obtained with the Very Large Array, which places a tight upper bound on the nuclear radio power at 8.4 GHz. We combine these new measurements with upper limits at other wavelengths to discuss implications for the nature of accretion onto the central black hole.

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“…Verolme et al 2002) show that state-ofthe-art models combined with two-dimensional integral-field spectroscopic data are required to constrain precisely the global physical parameters of early-type galaxies, such as the inclination angle or the mass-to-light ratio, as well as the central characteristics for objects exhibiting features such as kinematically decoupled cores (e.g. the core mass of IC 1459, Cappellari et al 2002).…”

Section: For 15 Kdcs)mentioning

confidence: 99%

A 60 pc counter-rotating core in NGC 4621

Wernli

Emsellem

Copin

2002

A&A

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Abstract. We present adaptive optics assisted OASIS integral field spectrography of the S0 galaxy NGC 4621. Two-dimensional stellar kinematical maps (mean velocity and dispersion) reveal the presence of a ∼60 pc diameter counter-rotating core (CRC), the smallest observed to date. The OASIS data also suggests that the kinematic center of the CRC is slightly offset from the center of the outer isophotes. This seems to be confirmed by archival HST/STIS data. We also present the HST/WFPC2 V − I colour map, which exhibits a central elongated red structure, also slightly off-centered in the same direction as the kinematic centre. We then construct an axisymmetric model of NGC 4621: the two-integral distribution function is derived using the Multi-Gaussian Expansion and the Hunter & Qian (1993) formalisms. Although the stellar velocities are reasonably fitted, including the region of the counter-rotating core, significant discrepancies between the model and the observations demonstrate the need for a more general model (e.g. a three-integral model).

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

Cited by 170 publications

References 52 publications

The ACS Fornax Cluster Survey. II. The Central Brightness Profiles of Early-Type Galaxies: A Characteristic Radius on Nuclear Scales and the Transition from Central Luminosity Deficit to Excess

The ACS Fornax Cluster Survey. II. The Central Brightness Profiles of Early-Type Galaxies: A Characteristic Radius on Nuclear Scales and the Transition from Central Luminosity Deficit to Excess

Detection of the “Active” Nucleus of M32

A 60 pc counter-rotating core in NGC 4621

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