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

By E. Verolme, M. Cappellari, Y. Copin, R. P. van der Marel, R. Bacon, M. Bureau, Roger Davies, B. Miller, P. de Zeeuw. 2002

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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) × 10 6 Mand 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 in- vestigate the effect of regularization on the orbit distribution.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Quantifying the coexistence of massive black holes and dense nuclear star clusters (2009, background): “M32 Ferrarese et al. (2006a) suggest that M32 may contain both a nuclear star cluster (Smith 1935; Burbidge 1970; Worthey 2004) and a BH (Verolme et al. 2002, we present an I-band light profile which we have fitted with an inner nuclear component , plus a Sérsic bulge and an outer exponential…”
Triaxial orbit based galaxy models with an application to the (apparent) decoupled core galaxy NGC 4365 (2007, methodology): “The method described here uses many of the ideas and algorithms described in Rix et al. (1997), van der Marel et al. (1998), Cretton et al. (1999), Verolme et al. (2002) and Cappellari et al. (2006).”
HST STIS Spectroscopy of the Triple Nucleus of M31: Two Nested Disks in Keplerian Rotation around a Supermassive Black Hole (2005, background): “Considering, in addition to M31, only the two closest other supermassive BHs, i.e., M32 and the Galaxy, we get the following: M32 has bulge 75 km s 1, a predicted M ¼ 2:6 ; 106 M , and an observed M ¼ (2:9 0:6) ; 106 M (Verolme et al. 2002; corrected to distance 0.81 Mpc from Tonry et al. 2001).”
A Fundamental plane of black hole activity (2003, unknown): “…(2001); (64) Schödel et al. (2002); (65) Orosz & Bailyn (1997); (66) Greiner, Cuby & McCaughrean (2001); (67) Ho, Terashima & Ulvestad (2003); (68) Verolme et al. (2002); (69) Dolan (1992); (70) Hanson, Still & Fender (2000); (71) Filippenko & Chornock (2001); (72) Stirling et al. (2001), (73)…”
Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research (2004, methodology): “State of the art 3I models are now routinely applied to stellar kinematics (Verolme et al. 2002; Gebhardt et al. 2003).”
The dynamical distance and intrinsic structure of the globular cluster ω Centauri (2005, background): “…velocities, to avoid confusion with the decomposition of the proper motions in the plane of the sky into a radial and tangential component. galaxies (van der Marel et al. 1998; Cretton et al. 1999; Cappellari et al. 2002; Verolme et al. 2002; Gebhardt et al. 2003; Krajnović et al. 2005).”
The SAURON project – VIII. OASIS/CFHT integral-field spectroscopy of elliptical and lenticular galaxy centres (2006, background): “Spectros opy is required to establish dynamical black hole mass estimates, nd it has been shown that a single long slit is grossly insufficient to constrain fully general dynamical models (Verolme et al.2002; Cappellari & McDermid 2005).”
THE NGC 404 NUCLEUS: STAR CLUSTER AND POSSIBLE INTERMEDIATE-MASS BLACK HOLE (2010, methodology): “…follow-up observations, this BH would be the lowest mass dynamically detected BH at the center of a galaxy, with previous determinations of low mass BHs in M32 (2.5 ± 0.5 × 106 M⊙; Verolme et al. 2002) and Circinus (1.7 ± 0.3 × 106 M⊙; Greenhill et al. 2003) being significantly more massive.”
Difficulties with Recovering the Masses of Supermassive Black Holes from Stellar Kinematical Data (2002, methodology): “Since about 1999, it has been common practice in 3I modeling to include smoothness constraints on the orbital weights, in the form of maximum entropy or some other regularization scheme (e.g., Cretton et al. 1999; Gebhardt et al. 2000a; Verolme et al. 2002).”
Galaxy Masses: A Review (2013, methodology): “…has been used extensively to measure masses of supermassive black holes in galaxies (e.g. van der Marel et al. 1998; Cretton & van den Bosch 1999; Verolme et al. 2002; Gebhardt & et al. 2003; Valluri et al. 2004), to measure M/L or DM profiles (e.g. Cappellari et al. 2006; Thomas et al. 2007;…”
A Fundamental Relation between Compact Stellar Nuclei, Supermassive Black Holes, and Their Host Galaxies (2006, background): “There is no evidence for a SBH in either M33 (Merritt et al. 2001; Gebhardt et al. 2001) or NGC 205 (Valluri et al. 2003), yet M32 does appear to contain a SBH with MSBH ≈ 2.5×106M⊙ (Verolme et al. 2002).”
Axisymmetric Dynamical Models of the Central Regions of Galaxies (2002, methodology): “—Verolme et al. (2002) have used both STIS spectroscopy and high-S/N ground-based two-dimensional spectra to provide one of the best measured BH masses using orbit-based models.”
The Low End of the Supermassive Black Hole Mass Function: Constraining the Mass of a Nuclear Black Hole in NGC 205 via Stellar Kinematics (2005, background): “Below 107M only twomeasurements exist: in theMilky Way (MBH ¼ 4 ; 106 M ; Ghez et al. 2003; Schödel et al. 2003) and in M32 (MBH ¼ 2:5 ; 106 M ; Verolme et al. 2002; van der Marel et al. 1998).”
The SAURON project - IV. The mass-to-light ratio, the virial mass estimator and the Fundamental Plane of elliptical and lenticular galaxies (2005, methodology): “A similar approach was adopted by us and by other groups to measure the black hole (BH) masses in galaxy nuclei or to analyse the stellar orbital distribution (e.g. Cretton et al. 1999; Cappellari et al. 2002; Verolme et al. 2002; Gebhardt et al. 2003; Valluri et al. 2004; Thomas et al. 2004).”
Nuclear star clusters (2009, background): “Other nearby examples for black hole detections within NSCs are M 31 (Bacon et al. 1994; Bender et al. 2005) and M 32 (Verolme et al. 2002; Nguyen et al. 2018).”
REVISITING THE SCALING RELATIONS OF BLACK HOLE MASSES AND HOST GALAXY PROPERTIES (2012, unknown): “…Ghez et al. 2008) ; (2 = Gillessen et al. 2009) ; (3 = Dalla Bontà et al. 2009) ; (4 = Greenhill et al. 2003) ; (5 = Cappellari et al. 2002) ; (6 = Verolme et al. 2002) ; (7 = Bender et al. 2005) ; (8 = Krajnović et al. 2009) ; (9 = Schulze & Gebhardt 2011) ; (10 = Bower et al. 2001) ; (11 =…”
Secular Evolution and the Formation of Pseudobulges in Disk Galaxies (2004, background): “…& Schechter 1982; Kormendy & Illingworth 1982; Binney, Davies, & Illingworth 1990) and now beautifully shown by integralfield spectroscopy (de Zeeuw et al. 2002; Verolme et al. 2002, Bacon et al. 2002; Copin, Cretton, & Emsellem 2004; Falcón-Barroso et al. 2004; Krajnović et al. 2004).”
Central Masses and Broad-Line Region Sizes of Active Galactic Nuclei. II. A Homogeneous Analysis of a Large Reverberation-Mapping Database (2004, methodology): “In quiescent galaxies, dynamical mod- elling of either stellar kinematics (e.g., van der Marel 1994; van der Marel et al. 1998; Verolme et al. 2002; Gebhardt et al. 2003) or gas motions (e.g., Harms et al. 1994; Ford et al. 1994; Macchetto et al. 1997) is used to determine central masses.”