Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA.
SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USA.
Science. 2015 Mar 27;347(6229):1459-62. doi: 10.1126/science.1261475.
The luminosities of type Ia supernovae (SNe), the thermonuclear explosions of white-dwarf stars, vary systematically with their intrinsic color and the rate at which they fade. From images taken with the Galaxy Evolution Explorer (GALEX), we identified SNe Ia that erupted in environments that have high ultraviolet surface brightness and star-formation surface density. When we apply a steep model extinction law, we calibrate these SNe using their broadband optical light curves to within ~0.065 to 0.075 magnitude, corresponding to <4% in distance. The tight scatter, probably arising from a small dispersion among progenitor ages, suggests that variation in only one progenitor property primarily accounts for the relationship between their light-curve widths, colors, and luminosities.
Ia 型超新星（SN）是白矮星热核爆炸的产物，其光度与其固有颜色和衰减率呈系统性变化。我们利用 Galaxy Evolution Explorer（GALEX）拍摄的图像，鉴定出在具有高紫外表面亮度和恒星形成表面密度的环境中爆发的 Ia 型超新星。当我们应用严格的模型消光定律时，我们使用它们的宽带光学光曲线对这些 SN 进行校准，精度在~0.065 到 0.075 星等之间，对应于距离上的<4%。这种紧密的分散，可能是由于前身星年龄的微小差异引起的，表明只有一个前身星特性的变化主要解释了它们的光曲线宽度、颜色和光度之间的关系。
