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Stellar Velocity Field in the Central Region of NGC 1068

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Abstract

We present the velocity field of the stars in the central 25″ × 22″ of NGC 1068 derived from 2-D spectroscopy of the Ca II triplet. A preliminary analysis provides evidence for two distinct stellar systems in the centre of NGC 1068. In the outer regions (say r > 10″), the mean stellar velocity field seems coupled to those of the ionized and molecular gas, indicating aproximately regular rotation with the kinematic minor axis at PA ~ 0°. However, in the inner region, the stars are rotating, whereas the ionized gas is outflowing in the NE-SW direction probably due to the effects of the nuclear activity, and the molecular gas is responding to the bar potential.

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Authors and Affiliations

  1. Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Canary Islands, Spain

    B. Garcia-Lorenzo, E. Mediavilla, S. Arribas & C. Del Burgo

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  1. B. Garcia-Lorenzo
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  2. E. Mediavilla
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  3. S. Arribas
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  4. C. Del Burgo
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Garcia-Lorenzo, B., Mediavilla, E., Arribas, S. et al. Stellar Velocity Field in the Central Region of NGC 1068. Astrophysics and Space Science 248, 43–49 (1997). https://doi.org/10.1023/A:1000576000419

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  • DOI: https://doi.org/10.1023/A:1000576000419

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