Kinematics of Late-Type Stars in the Central 10 Parsecs of the Galaxy

霍尔、塞尔格伦和贝克林博士将在近- 红外波长，以表征运动和 晚型星的星群亮度在5 银河系中心的秒差距半径 这将考验 一个大质量凝聚体存在的假设 它将提供独特的运动学数据， 可以应用于我们对其他原子核的理解 星系 我们银河系的中心提供了一个独特的机会来研究 星系核的空间尺度小到百分之几， 一个秒差距，并获得个别恒星的观测范围内， 地区 对我们银河系核心的详细研究 在解释其他方面证明至关重要，更多 高能星系核 由于灰尘的严重遮蔽， 银河系的中心在可见光波段是不可观测的。 然而，它可以在红外线和更长的波长下进行研究， 以及光谱仪器和阵列探测器的进步 使近红外线的详细研究成为可能。

Drs. Hall, Sellgren, and Becklin will make observations at near- infrared wavelengths in order to characterize the motions and the brightness of the population of late type stars located within a 5 parsec radius of the Galactic Center. This will test the hypothesis of the existence of a massive condensed object at the Galactic Center, and it will provide unique kinematic data which can be applied to our understanding of the nuclei of other galaxies. The center of our Galaxy provides a unique opportunity to study a galactic nucleus at spatial scales as small as a few hundredths of a parsec and to obtain observations of individual stars within the region. Detailed studies of the nucleus of our own Galaxy may prove vitally important in the interpretation of other, more energetic galactic nuclei. Because of heavy obscuration by dust, the center of the Galaxy is not observable at visible wavelengths. It can be studied, however, at infrared and longer wavelengths, and advances in spectroscopic instrumentation and array detectors now make possible detailed studies in the near infrared.