The counterrotating core and the black hole mass of IC1459

By M. Cappellari, E. Verolme, R. P. van der Marel, G. Kleijn, G. Illingworth, M. Franx, C. Carollo, P. de Zeeuw. 2002

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The E3 giant elliptical galaxy IC1459 is the prototypical galaxy with a fast counterrotating stellar core. We obtained one HST/STIS long-slit spectrum along the major axis of this galaxy and CTIO spectra along five position angles. We present self-consistent three-integral axisymmetric models of the stellar kinematics, obtained with Schwarzschild's numerical orbit superposition method. We study the dynamics of the kinematically decoupled core (KDC) in IC1459 and we find it consists of stars that are well-separated from the rest of the galaxy in phase space. The stars in the KDC counterrotate in a disk on orbits that are close to circular. We estimate that the KDC mass is ~0.5% of the total galaxy mass or ~3*10^9 Msun. We estimate the central black hole mass M_BH of IC1459 independently from both its stellar and its gaseous kinematics. Some complications probably explain why we find rather discrepant BH masses with the different methods. The stellar kinematics suggest that M_BH = (2.6 +/- 1.1)*10^9 Msun (3 sigma error). The gas kinematics suggests that M_BH ~ 3.5*10^8 Msun if the gas is assumed to rotate at the circular velocity in a thin disk. If the observed velocity dispersion of the gas is assumed to be gravitational, then M_BH could be as high as ~1.0*10^9 Msun. These different estimates bracket the value M_BH = (1.1 +/- 0.3)*10^9 Msun predicted by the M_BH-sigma relation. It will be an important goal for future studies to assess the reliability of black hole mass determinations with either technique. This is essential if one wants to interpret the correlation between the BH mass and other global galaxy parameters (e.g. velocity dispersion) and in particular the scatter in these correlations (believed to be only ~0.3 dex). [Abridged]

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/03a06df8aeba0f60eeee330c3c6261053ac45225

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THE BLACK HOLE MASS, STELLAR MASS-TO-LIGHT RATIO, AND DARK HALO IN M87 (2009, background): “Of those that do have both measures, the results can vary greatly: IC1459 has the gas measure 8 times larger than that of the stars (Cappellari et al. 2002) and CenA has the stellar measure 7 times larger than that of the gas (Silge et al. 2005, Neumayer et al. 2007,), although Cappellari et al.…”
Fundamental Planes and the Barless MBH-σ Relation for Supermassive Black Holes (2008, background): “IC 1459 is also excluded here due to the order of magnitude uncertainty on its SMBH mass (Cappellari et al. 2002).”
Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research (2004, background): “Only one, IC1459 (Cappellari et al. 2002) has been studied so far; we will return to IC1459 later in this section.”
A SAURON study of M32: measuring the intrinsic flattening and the central black hole mass (2002, methodology): “We have therefore adapted the axisymmetric Schwarzschild software to use MGE; the new algorithm was tested while modeling the dynamics of the counter-rotating core galaxy IC1459 (Cappellari et al. 2002).”
The ATLAS3D project XV: benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, fundamental plane and mass plane (2012, methodology): “…al. 1998) and has been widely used for determinations of masses of supermassive black holes (e.g. van der Marel et al. 1997; Gebhardt et al. 2000a; Cappellari et al. 2002; Valluri, Merritt & Emsellem 2004; Houghton et al. 2006), for galaxy mass determinations (e.g. Cappellari et al. 2006; Thomas…”
An Intermediate-Mass Black Hole in the Globular Cluster G1: Improved Significance from New Keck and Hubble Space Telescope Observations (2005, background): “These are now commonplace and standard (Gebhardt et al. 2000c, 2003; Cappellari et al. 2002; Krajnovic et al. 2005).”
The SAURON project – VIII. OASIS/CFHT integral-field spectroscopy of elliptical and lenticular galaxy centres (2006, methodology): “Whether or not components are actually decoupled in phase-space requires the application of dynamical models (such as Cappellari et al. 2002; Verolme etal.”
The Masses of Nuclear Black Holes in Luminous Elliptical Galaxies and Implications for the Space Density of the Most Massive Black Holes (2006, unknown): “…al. 2006; (2) Gebhardt et al. 2007; (3) Gebhardt et al. 2000a; (4) Gebhardt et al. 2003; (5) Ferrarese et al. 1996; (6) Bower et al. 1998; (7) Maciejewski & Binney 2001; (8) Macchetto et al. 1997; (9) van der Marel & van den Bosch 1998; (10) Verdoes Kleijn et al. 2000; (11) Cappellari et al. 2002.”
Difficulties with Recovering the Masses of Supermassive Black Holes from Stellar Kinematical Data (2002, background): “Another such restriction, common in the more recent studies, is to force the 3I f to be smooth (Cretton et al. 1999; Gebhardt et al. 2003; Cappellari et al. 2002; Verolme et al. 2002).”
Axisymmetric Dynamical Models of the Central Regions of Galaxies (2002, methodology): “Three of these are from the Leiden Group: M32 (van der Marel et al. 1998; Verolme et al. 2002), NGC 4342 (Cretton & van den Bosch 1999), and IC 1459 (Cappellari et al. 2002).”
Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies (2013, methodology): “In contrast, Cappellari et al. (2002) combine HST STIS spectroscopy with high-S/N ground-based spectroscopy (CTIO 4 m telescope; seeing FWHM ≈ 1.”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “…have provided most of the mass determinations of supermassive black holes in galaxies (e.g., some examples from different groups are van der Marel et al. 1998; Gebhardt et al. 2000b; Cappellari et al. 2002; Valluri et al. 2005; McConnell et al. 2011; van den Bosch et al. 2012; Rusli et al. 2013).”
Adaptive spatial binning of integral-field spectroscopic data using Voronoi tessellations (2003, methodology): “The kinematics extraction was performed in pixel-space using the method of Cappellari et al. (2002), and adopting a single K1 III template star observed with SAURON.”
The SAURON project - IV. The mass-to-light ratio, the virial mass estimator and the Fundamental Plane of elliptical and lenticular galaxies (2005, methodology): “The MGE fits were done by keeping the position angle (PA) for all Gaussian fixed and taking PSF convolution into account (our F814W MGE PSF is given in Table 3 of Cappellari et al. 2002).”