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2.1. ISOCAM CVF observations of the Quintuplet and Object#17 clusters near the galactic center. diffuse components

Published online by Cambridge University Press:  25 May 2016

T. Nagata ,
K. Kawara ,
T. Onaka ,
Y. Kitamura  and
H. Okuda
T. Nagata
Affiliation:
Department of Physics, Nagoya University, Nagoya 464-01, Japan
K. Kawara
Affiliation:
Institute of Astronomy, University of Tokyo, Mitaka 181, Japan
T. Onaka
Affiliation:
Department of Astronomy, University of Tokyo, Tokyo 113, Japan
Y. Kitamura
Affiliation:
Institute of Space and Astronautical Science, Yoshinodai, Sagamihara 229, Japan
H. Okuda
Affiliation:
Institute of Space and Astronautical Science, Yoshinodai, Sagamihara 229, Japan

Extract

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There are two star clusters near the Galactic Center which might be similar to the central parsec cluster. One is the Quintuplet cluster at (l = 0.16°, b = −0.06°), and the other is the Object #17 cluster at (l = 0.12°, b = 0.02°). The Quintuplet, first found in a polarimetric survey by Kobayashi et al. (1983), includes five very bright stars whose color temperatures are in the range of 600-900K (Okuda et al. 1990; Nagata et al. 1990). Object #17 is a cluster of emission line stars (Nagata et al. 1993, 1995; Cotera et al. 1996; Morris & Serabyn 1996). Spectral features of these two objects observed with the ISOCAM (Kessler et al. 1996; Cesarsky et al. 1996) have been reported (Nagata et al., 1996); absorption features due to O-H (2.8μm) CO2(4.3μm), and CO (4.7μm) are present. In this paper, we report diffuse emission components detected in these two fields.

Type
Part I. Stellar Cluster, Star Formation
Information
Symposium - International Astronomical Union , Volume 184: The Central Regions of the Galaxy and Galaxies , 1998 , pp. 59 - 60
Copyright
Copyright © Kluwer 1998 

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