Determination of masses of the central black holes in NGC 524 and 2549 using laser guide star adaptive optics

Abstract

We present observations of early‐type galaxies NGC 524 and 2549 with laser guide star adaptive optics (LGS AO) obtained at GEMINI North telescope using the Near‐infrared Integral Field Spectrograph (NIFS) integral field unit (IFU) in the K band. The purpose of these observations is to determine high spatial resolution stellar kinematics within the nuclei of these galaxies and, in combination with previously obtained large‐scale observations with the SAURON IFU, to determine the masses (M•) of the supermassive black holes (SMBH). The targeted galaxies were chosen to have central light profiles showing a core (NGC 524) and a cusp (NGC 2549), to probe the feasibility of using the galaxy centre as the natural guide source required for LGS AO. We employ an innovative technique where the focus compensation due to the changing distance to the sodium layer is made ‘open loop’, allowing the extended galaxy nucleus to be used only for tip‐tilt correction. The data have spatial resolution of 0.23 and 0.17 arcsec full‐width at half maximum (FWHM), where at least ∼40 per cent of flux comes within 0.2, showing that high quality LGS AO observations of these objects are possible. The achieved signal‐to‐noise ratio (S/N ∼ 50) is sufficiently high to reliably determine the shape of the line‐of‐sight velocity distribution. We construct axisymmetric three‐integral dynamical models which are constrained with both the NIFS and SAURON data. The best‐fitting models yield M•= (8.3+2.7−1.3) × 108 M⊙ and (M/L)I= 5.8 ± 0.4 for NGC 524 and M•= (1.4+0.2−1.3) × 107 M⊙ and (M/L)R= 4.7 ± 0.2 for NGC 2549 (all errors are at the 3σ level). We demonstrate that the wide‐field SAURON data play a crucial role in the M/L determination increasing the accuracy of M/L by a factor of at least 5, and constraining the upper limits on black hole masses. The NIFS data are crucial in constraining the lower limits of M• and in combination with the large‐scale data reducing the uncertainty by a factor of 2 or more. We find that the orbital structure of NGC 524 shows significant tangential anisotropy, while at larger radii both galaxies are consistent with having almost perfectly oblate velocity ellipsoids. Tangential anisotropy in NGC 524 coincides with the size of SMBH sphere of influence and the core region in the light profile. This agrees with predictions from numerical simulations where core profiles are the result of SMBH binaries evacuating the centre nuclear regions following a galaxy merger. However, being a disc dominated fast rotating galaxy, NGC 524 has probably undergone through a more complex evolution. We test the accuracy to which M• can be measured using seeings obtained from typical LGS AO observations, and conclude that for a typical conditions and M• the expected uncertainty is of the order of 50 per cent.

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

“…In addition, the comparison between the HST image and the collapsed data cubes allows for the center of the NIFS and PPAK apertures to be defined. The core of the NIFS PSF is larger than expected for AO observations (e.g., Krajnović et al 2009;Seth et al 2014), which is likely the result of using a fairly faint, off-axis tip-tilt star. In Section 7.1, we test the effect of our assumed NIFS PSF on the inferred black hole mass by instead estimating the PSF from NIFS observations we acquired of the tip-tilt star itself.…”

“…While this approach is commonly used in black hole mass measurement work (e.g., Krajnović et al 2009;Seth et al 2010;Walsh et al 2012), estimation of the PSF from AO observations is notoriously difficult owing to the constantly changing quality of the AO correction and the combination of data cubes from multiple nights. Therefore, we also estimated the PSF in a different manner in order to assess how strongly the adopted NIFS PSF affects M BH .…”

“…We note that the final uncertainty on the black hole mass we use is comparable to the formal 3σ statistical uncertainty. Some Krajnović et al 2009;Emsellem 2013) have suggested that 3σ statistical errors should be used in place of 1σ errors as a conservative way in which to account for the effect of unknown systematics on M BH . With a black hole mass of M 3.0 10 9  and adopting 276 km s −1 for the Figure 7.…”

A Black Hole Mass Determination for the Compact Galaxy Mrk 1216

“…The LOSVD was largely constrained by the strong 12 CO(2−0) and 12 CO(3−1) bandheads, which were contained within the 2.26 − 2.39 µm fitting region. We masked the Ca I absorption line because our template library does not include cool dwarf stars (e.g., Krajnović et al 2009), and further excluded a few artificial features, likely the result of imperfect sky subtraction or telluric correction. Example fits with pPXF to the observed galaxy spectra located at the nucleus, in an intermediate region, and in one of the outermost spatial bins are given in Figure 1.…”

“…Following past work (e.g., Krajnović et al 2009;Seth et al 2014), the MGE in Section 2 was convolved with the NIFS PSF and compared to the Mrk 1216 data cube, after collapsing along the wavelength axis. This resulted in best-fit values of 0.…”