| Autor: |
Araki, H., Brézin, E., Ehlers, J., Frisch, U., Hepp, K., Jaffe, R. L., Kippenhahn, R., Weidenmüller, H. A., Wess, J., Zittartz, J., Beiglböck, W., Winnewisser, Gisbert, Pelz, Guido C., Eckart, A., Genzel, R., Hofmann, R., Sams, B. J., Tacconi-Garman, L. E. |
| Zdroj: |
Physics & Chemistry of Interstellar Molecular Clouds; 1995, p41-49, 9p |
| Abstrakt: |
We present deep 1.6 (H) and 2.2μm (K) images of the central parsec of the Galaxy at a resolution of 0.15″. We also give a brief history of high spatial resolution imaging of the Galactic Center in the near-infrared. Our recent speckle imaging results are: Most of the flux in earlier seeing limited images comes from about 340 unresolved stellar sources with K magnitudes <14. Most of the fainter stars in the central parsec are likely to be M-rather than K-giants. The IRS 16 and 13 complexes are resolved into about 25 and 6 sources, many of which are probably luminous hot stars. We confirm the presence of a blue near infrared object (K≈13) at the position of the compact radio source Sgr A*. This source either has a ∼0.5" east-west size or it is multiple with its western component closest to Sgr A*. The spatial centroid of the number distribution of compact sources is consistent with the position of Sgr A* but not with a position in the IRS 16 complex. The stellar surface density is very well fitted by an isothermal cluster model with a core radius of 0.15±0.05 pc. If the 2μm emitting stars sample the overall mass distribution of the stellar cluster the stellar density is a few times 107 M⊙ pc−3. Buildup of massive stars by collisional merging of lower mass stars and collisional disruption of giant atmospheres are very probable processes in the central 0.2pc. [ABSTRACT FROM AUTHOR] |
| Databáze: |
Supplemental Index |
| Externí odkaz: |
|
