超新星是宇宙中最高能的现象之一。光变曲线作为超新星的一个观测性质，对宇宙学、超新星物理过程及恒星演化等研究十分重要。而获取大样本的超新星光变曲线对这些研究尤为重要。本文介绍利用清华-国家天文台望远镜（Tsinghua-NAOC Telescope，TNT）进行的超新星测光监测，以及相关数据处理和分析。我们从 2004 年 10 月底至 2016 年 12 月使用 TNT 监测了 398 颗超新星，获得 36647 幅图像，共计 3914 小时曝光时间。为了处理这些数据，我们开发了名为 ZrutyPhot 的自动测光程序，实现了对 TNT 图像的位置定标、模板相减、测光、流量定标等功能。我们使用 ZrutyPhot 对超新星图像进行处理，整理得到一个有 201 颗超新星的光变曲线样本。该样本中的超新星红移小于等于 0.102，类型覆盖了 Ia、Ib/c 和 II 型。样本共含有 18108 个光变曲线数据点，波段为 UBVRI。我们使用 SALT2 对样本中的 Ia 型超新星进行了光变曲线拟合，获得了它们的光极大时间和星等、形状参数、颜色等光变曲线基本参数。利用拟合得到的参数，我们绘制了一个含有 84 颗 Ia 型超新星的哈勃图。经过对比分析发现，我们的结果与 SDSS-II/SNLS3 Joint Light-Curve Analysis 的结果基本一致，而弥散仅比他们的结果略大。利用数据处理中的一些副产品，我们简要分析了兴隆观测基地的视宁度、夜天光背景亮度和大气消光系数等观测条件，分析的结果与前人工作基本一致，且发现这些条件在近年变化较小。
Supernova is one of the most energetic phenomenon in the cosmos. One of its observational property, light curve of supernova is important for studies of cosmology, physics of supernova, stellar evolution and so on. Requiring large samples of light curves of supernovae are especially important for those studies.This paper will introduce photometry monitoring of supernovae using Tsinghua-NAOC Telescope(TNT) and related data reduction and analysis.From the end of October 2004 to December 2016, we monitored 398 supernovae using TNT, required 36647 images with a total exposure time of 3914 hours. To reduce these data, we have developed a pipeline, named ZrutyPhot, which have implemented functions including astrometrical calibration, template subtraction, photometry and flux calibration for images of TNT. We have used ZrutyPhot to reduce the images of supernovae and acquired a sample of light curves of 201 supernovae. Type Ia, Ib/c or II, all supernovae in the sample have a redshift no more than 0.102. The sample contains light curve data points of a total number of 18108, with a band coverage of UBV RI.We have used SALT2 to fit light curves of type Ia supernovae in the sample and obtained their basic parameters of light curve, like peak magnitude and its epoch, shape parameters and color. Using these parameters, we have constructed a Hubble diagram containing 84 type Ia supernovae. Through comparison and analysis, we find that our result is consistent with the result of SDSS-II/SNLS3 Joint Light-Curve Analysis, while the scatter of our result is slightly larger than theirs.Using by-product of data reduction, we have briefly analyzed some observing conditions of Xinglong Station, including seeing, night sky brightness and atmospheric extinction coefficients. The analysis results are consistent with previous works of others and showing these conditions were changed little for the past few years.
