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V. Das (Georgia State University)
With new and improved spatial coverage of the entire narrow-line regions (NLRs) in NGC 4151 and NGC 1068, we present a study of the kinematics of the [O III] emission-line gas outflow using a 3D modeling technique. We used multiple long-slit spectra (with spatial resolution of 0.2 arcsec across and 0.1 arcsec along each slit) from the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope (HST). The G430M grating provided excellent spectral resolving power (~9000) which allowed velocity measurements accurate to about 30 km s-1. As a result, we detected multiple kinematic components of [O III] emission that we deconvolved using Gaussian fits. We then generated biconical outflow models to match the kinematic data and for comparison to previous models done for lower resolution observations. The general trend is an increase in radial velocity of the NLR clouds roughly proportional to distance out to 100 pc from the nucleus, followed by a linear decrease to the systemic velocity of the host galaxy. This is similar to the kinematics seen in other Seyfert galaxies, indicating common acceleration/deceleration mechanisms.
For comparison, we used existing high-resolution (0.014 arcsec pix-1) radio maps covering both NLRs from the Very Long Baseline Array (VLBA), the Very Large Array (VLA), and Merlin. These maps were used to examine the dependency of the NLR cloud velocities on the radio structure. The NLR clouds show a smooth transition across the radio knots in radial velocity and velocity dispersion plots. Thus, the NLR kinematics appear to be unaffected by the radio jets in both galaxies.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.