The Structure of the Broad-Line Region in Active Galactic Nuclei

活动星系核光谱中广泛发射线的可变性揭示了有关线发射区的结构和运动学以及中央源性质的基本信息，这些信息是任何其他方式都无法获得的。这个程序通过对有限数量的源的重复观测来确定活动星系核中宽线发射区的结构和运动学。我们利用为珀金斯1.8米望远镜开发的远程观测设备，大大提高了我们正在进行的监测项目的时间分辨率。此外，通过使用新的ccd光谱仪，个别观测的质量将大大提高。CCD光谱仪通过光纤馈电连接到望远镜上，这使我们能够在部分夜晚使用光谱仪，而不需要完全改变望远镜卡斯格伦焦点的仪器。这使我们能够经常地观察一些选定的来源，而对其他科学计划的影响最小。

The variability of the broad emission lines in the spectra of active galactic nuclei reveals fundamental information about the structure and kinematics of the line-emitting region and about the nature of the central source that cannot be obtained in any other way. This program determines the structure and kinematics of the broad-line emitting regions in active galactic nuclei through repeated observations of a limited number of sources. We greatly improve the temporal resolution of our on-going monitoring project by making use of a Remote Observing Facility which has been developed for use with the Perkins 1.8 m telescope. Furthermore, the quality of the individual observations will be greatly improved through the use of a new CCD spectrograph. The CCD spectrograph is interfaced to the telescope with a fiber- optic feed which enables us to use the spectrograph for partial nights without a complete change of instrumentation at the Casse- grain focus of the telescope. This allows us to observe a few selected sources frequently with minimal impact on other scien- tific programs.