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

RUI：超新星和变星的电荷耦合器件 (CCD) 观测

• 批准号: 9417359
• 负责人: Priscilla Benson
• 金额: $ 13.1万
• 依托单位: Wellesley College
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 1995
• 资助国家: 美国
• 起止时间: 1995-06-01 至 2000-05-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9417359&HistoricalAwards=false
• 关键词: RUI; Charge; Coupled; Device; CCD

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.

小行星9417359 将要进行的研究将包括用韦尔斯利学院24”Boller和Chivens望远镜上的NU 200电荷耦合器件照相机对超新星、新星和变星进行BVRI观测。 将在最晴朗的夜晚进行观测。 将使用IRAF软件数据缩减包进行图像缩减和测光。 将使用电子表格软件程序进行进一步分析。 将建立一个观察数据库。 对于大多数物体，微分光变曲线将由恒星组成。 对于具有校准场的物体，将计算所观察到的物体的标准星等。 这些观测是大约两年前开始的一个项目的延续。 观测到的物体的光变曲线将在适当的时候公布。 该研究计划的目标是：1）提高超新星，特别是R和I波段的光变曲线的采样质量; 2）提供银河新星的光变曲线的采样质量; 3）对几颗变星进行正确的分类和周期; 4）提高对光变曲线的认识，寻找共生星和RCB星的爆发或变暗;（5）改善妇女在科学领域的人力资源基础。 很少有超新星的光变曲线是用标准的B、V、R和I滤光片观测到的，因此有很好的光变曲线采样。 最近对超新星的观测，有很好的采样光变曲线，似乎表明它们的光强度比以前认识到的有更多的变化。 由于超新星经常被用作标准烛光来确定到其他星系的距离，因此识别每种超新星并获得各种类型的校准样本是很重要的。 许多列在变星总表中的恒星都有不完整的信息。 其中许多恒星将被观测和监测。 至少已经发现了两个错误的分类。 重要的是监测共生星，以便了解恒星之间的相互作用，并在相互作用开始时捕捉爆发，以便在爆发期间获得电磁频谱其他波长的观测。 同样，RCB星需要被监测，以便在尘埃事件发生时检测它们。 最后，韦尔斯利学院的女本科生将提出许多意见。 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变曲线。 虽然一些参与的学生可能不是主修科学，他们将学习科学是如何做的。 拥有一个有科学素养的社会是很有价值的。