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J. Pinkney (UMich), K. Gebhardt (UCO/Lick), D. Richstone (UMich), Nuker Team
We have obtained STIS spectroscopy of NGC 4697 in two spectral ranges which allow independent mass measurements of the central dark object. The near-IR range allows stellar kinematics to be derived from the shape of the Ca triplet absorption lines. 3-integral modelling places this galaxy slightly above the Mbh -- \sigma relationship (Gebhardt et al. 2000) with Mbh=1.2\times 108 M\odot. The other spectral range contains prominent [NII] (6583 Å) emission. Assuming the emitting gas is coplanar with the nuclear dust disk, and in circular motion, we can constrain the BH mass. We model both the gas rotation curve and the shape of the emission lines to find a Mbh in good agreement with the stellar value.
We acknowledge support from HST grant GO-07388.01 and LTSA grant NAG5-8238 to D. Richstone.