RUI: Charge Coupled Device (CCD) Observations of Supernovae, and Variable Stars

这项研究将包括利用韦尔斯利学院24英寸博勒和奇文斯望远镜上的NU200电荷耦合器件（CCD）相机对超新星、新星和变星进行BVRI观测。观测将在最晴朗的夜晚进行。图像还原和光度测量将使用IRAF软件数据还原包完成。进一步的分析将使用电子表格软件程序来完成。将保存一个观察结果的数据库。对于大多数天体，恒星会形成不同的光曲线。对于具有校准视场的天体，将计算观测到的天体的标准星等。这些观察是大约两年前开始的一个项目的延续。观测到的物体的光曲线将在适当的时候公布。本研究计划的目标是：1)提高超新星光曲线的采样量，特别是在R和I波段；2)，提供采样良好的星系新星多色光曲线；3)若干变星的正确分类和周期；4)提高对光曲线的认识，寻找共生星和RCB星的爆发或变暗；5)完善科学领域女性的人力资源基础。用标准的B、V、R和I滤光片观测到的超新星光曲线很少，因此有很好的采样光曲线。最近对超新星的观测，有很好的光曲线采样，似乎表明它们的光强度变化比以前认识到的要大。由于超新星经常被用作确定与其他星系距离的标准烛光，因此确定每一种超新星，并拥有各种类型的校准好的样本是很重要的。在变星总目录中列出的许多恒星都没有完整的信息。许多这样的恒星将被观察和监测。至少已经发现了两种错误的分类。重要的是监测共生恒星，以便了解恒星之间的相互作用，并在相互作用开始时捕捉它们的爆发，以便在爆发期间获得电磁频谱的其他波长的观测结果。同样，需要对RCB星进行监测，以便在尘埃事件发生时检测到它们。最后，许多观察将由韦尔斯利学院的女本科生进行。他们将学习使用IRAF软件进行数据采集和处理的程序，以及分析各种恒星和超新星的光曲线。虽然一些参与的学生可能不是科学专业的，但他们将学习如何进行科学研究。一个有科学素养的社会是有价值的。

9417359 Benson The research to be carried out will include making BVRI observations of supernovae, novae, and variable stars with a Photometrics NU200 Charged-Coupled Device (CCD) camera on the Wellesley College 24" Boller and Chivens telescope. Observations will be made on most clear nights. The image reduction and photometry will be done with the IRAF software data reduction package. Further analysis will be done by using spreadsheets software programs. A database of observations will be kept. For most objects, differential light curves will be made of the stars. For objects with calibrated fields, standard magnitudes of the objects observed will be calculated. These observations are a continuation of a program begun about two years ago. Light curves of the objects observed will be published when appropriate. The objectives of the research program are to 1), improve the quantity of well-sampled light curves of supernovae, especially in the R and I bands; 2), provide well-sampled multicolor light curves of galactic novae; 3), correct classifications and periods for several variable stars; 4), improve the knowledge of light curves and search for outbursts or dimming of symbiotic and RCB stars; and 5) improve the human resources base of women in science. There are very few supernovae light curves that have been observed with standard B, V, R, and I filters and thus have well-sampled light curves. Recent observations of supernovae, which have well sampled light curves, seem to indicate that there is more variation in intensity of their light than previously recognized. Since supernovae are often used as standard candles to determine the distances to other galaxies, it is important to identify each kind of supernova, and to have well-calibrated samples of the various types. Many stars listed in the General Catalog of Variable Stars have incomplete information about them. Many of these stars will be observed and monitored. At least two misclassificat ions have already been discovered. It is important to monitor symbiotic stars in order to understand the interactions between the stars as well as to catch outbursts from interactions as they begin, in order to obtain observations in other wavelengths of the electromagnetic spectrum during outbursts. Similarly, RCB stars need to be monitored in order to detect dust events when they occur. Lastly, many of the observations will be made by female undergraduates at Wellesley College. They will learn the procedures for data acquisition, processing by using the IRAF software, and analysis of the light curves of various stars and supernovae. Although some of the participating students may not be majoring in science, they will learn how science is done. It is valuable to have a scientific literate society.