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Nearby Early-type Galactic Nuclei at High Resolution: Dynamical Black Hole and Nuclear Star Cluster Mass Measurements

  • Authors: Dieu D. Nguyen, Anil C. Seth, Nadine Neumayer, Sebastian Kamann, Karina T. Voggel, Michele Cappellari, Arianna Picotti, Phuong M. Nguyen, Torsten Böker, Victor Debattista, Nelson Caldwell, Richard McDermid, Nathan Bastian, Christopher C. Ahn, and Renuka Pechetti

2018 The Astrophysical Journal 858 118.

  • Provider: AAS Journals

Caption: Figure 5.

Stellar kinematic maps derived from CO band-head spectroscopy from Gemini/NIFS (NGC 205) and VLT/SINFONI (NGC 5102 and NGC 5206) spectroscopic data. Radial velocity maps are shown in the left column and dispersion maps in the middle column. The radial velocity is shown relative to the systemic velocity of −241 ± 2 km s−1 (NGC 205), 472 ± 2 km s−1 (NGC 5102), and 573 ± 5 km s−1 (NGC 5206). The top plots show the NGC 205 stellar kinematics after removing individual bright stars (Section 5.2). White contours show the stellar continuum, and red arrows indicate the orientation. Kinematics are only plotted out to the radii where they are reliable; black pixels indicate data not used in the JAM modeling. In the right column, the top panel shows the ﹩{V}_{\mathrm{rms}}=\sqrt{{V}^{2}+{\sigma }^{2}}﹩ (gray diamonds), with the black circles showing the bi-weighted Vrms in the circular annuli. The error bars are 1σ deviations of the kinematic measurements of the Voronoi bins in the same annuli. The KINEMETRY decomposition (Krajnović et al. 2006) of the dispersion (squares) and rotation (triangles) curves is shown in the bottom panel.

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