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• W3100798731 abstract "We have measured the stellar kinematic profiles of NGC 3379 along four position angles using the MMT. The data extend 90 from the center, at essentially seeing-limited resolution out to 17. The mean velocities and dispersions have total errors better than 10 km/s (frequently better than 5 km/s) out to 55. We find very weak (3 km/s) rotation on the minor axis interior to 12, and no detectable rotation above 6 km/s from 12 to 50 or above 16 km/s out to 90 (95% confidence). However, a Fourier reconstruction of the mean velocity field from all 4 sampled PAs does indicate a 5 degree twist of the kinematic major axis, opposite to the known isophotal twist. The h_3 and h_4 parameters are small over the entire observed region. The azimuthally-averaged dispersion profile joins smoothly at large radii with the dispersions of planetary nebulae. Unexpectedly, we find sharp bends in the major-axis rotation curve, also visible (though less pronounced) on the diagonal position angles. The outermost bend coincides in position with other sharp kinematic features: an abrupt flattening of the dispersion profile, and local peaks in h_3 and h_4. All of these features are in a region where the surface brightness profile departs significantly from a de Vaucouleurs law. Features such as these are not generally known in ellipticals owing to a lack of data at comparable resolution; however, very similar behavior is seen the kinematics of the edge-on S0 NGC 3115. We discuss the suggestion that NGC 3379 could be a misclassified S0; preliminary results from dynamical modeling indicate that it may be a flattened, weakly triaxial system seen in an orientation that makes it appear round." @default.
• W3100798731 created "2020-11-23" @default.
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• W3100798731 date "1999-02-01" @default.
• W3100798731 modified "2023-10-18" @default.
• W3100798731 title "The Stellar Kinematic Fields of NGC 3379" @default.
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• W3100798731 doi "https://doi.org/10.1086/300745" @default.
• W3100798731 hasPublicationYear "1999" @default.
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