Advertisement

CO-Line Rotation Curves, Deep Potential of Massive Cores, and High-density Molecular Nuclei

  • Yoshiaki Sofue
Conference paper
Part of the Astrophysics and Space Science Proceedings book series (ASSSP)

We review observational studies of central rotation curves of spiral galaxies using the Nobeyama mm-wave interferometer in the CO 2.6-mm line emission. The observed high-accuracy rotation curves show universal characteristics: RCs rise steeply in the nuclei, or they start at finite speed, and are flat toward the galaxy edges. Calculated mass distributions are similar to each other: spiral galaxies generally have a massive core of ~109M in the central 100 pc, bulge, disk and a dark halo. We found extremely high-density, single-peaked molecular gas nuclei in many galaxies, which are embedded in deep gravitational potential of the massive core. Although the molecular nuclei is as dense as that of a giant molecular cloud, the gas is kept gravitationally stable because of the high-velocity rotation.

Keywords

Rotation Curve Spiral Galaxy Massive Core Central Black Hole Dark Halo 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. 1.
    Sofue, Y. and Rubin, V.: ARAA 39, 137 (2001)CrossRefADSGoogle Scholar
  2. 2.
    Schinnerer, E., Maciejewski, W., Scoville, N.Z., Moustakas, L.A.: ApJ, 575, 826 (2002)CrossRefADSGoogle Scholar
  3. 3.
    Regan, M W., Thornley, M D., Helfer, T T., et al.: ApJ 561, 218 (2001)CrossRefADSGoogle Scholar
  4. 4.
    Schinnerer, E., Eckart, A., & Tacconi, L. J.: ApJ 524, L5 (1999)CrossRefADSGoogle Scholar
  5. 5.
    Sakamoto, K., Okumura, S. K., Ishizuki, S., and Scoville, N. Z.: ApJS 124, 403 (1999)CrossRefADSGoogle Scholar
  6. 6.
    Sofue, Y., Koda, J., Nakanishi, H., et al.: PASJ 55,17 (2003)ADSGoogle Scholar
  7. 7.
    Sofue, Y., Koda, J., Nakanishi, H., Onodera, S.: PASJ 55, 59 (2003)ADSGoogle Scholar
  8. 8.
    Nakanishi, H., et al.: PASJ 57, 965 (2006)Google Scholar
  9. 9.
    Onodera, S. et al.: PASJ 56, 439 (2004)ADSGoogle Scholar
  10. 10.
    Koda, J. and Sofue, Y.: PASJ 58, 299 (2006)ADSGoogle Scholar
  11. 11.
    Ferrarese, L., Freedman, W. L., Hill, R. J., et al.: ApJ. 464, 568 (1996)CrossRefADSGoogle Scholar
  12. 12.
    Takamiya, T, and Sofue, Y.: ApJL 576, L15 (2002)CrossRefADSGoogle Scholar
  13. 13.
    Takamiya, T, and Sofue, Y.: ApJ 534, 670 (2000)CrossRefADSGoogle Scholar
  14. 14.
    Sofue, Y.: PASJ 51, 445 (1999)ADSGoogle Scholar
  15. 15.
    Sofue, Y., Koda, J., Kohno, K., et al.: ApJL 547, L115 (2001)CrossRefADSGoogle Scholar
  16. 16.
    Koda, K., Sofue, Y., Kohno, K., et al.: ApJ 573, 105 (2002)CrossRefADSGoogle Scholar

Copyright information

© Springer Science+Business Media, LLC 2008

Authors and Affiliations

  • Yoshiaki Sofue
    • 1
  1. 1.Institute of AstronomyUniversity of TokyoMitakaJapan

Personalised recommendations