红色和变红：通过近红外观测Ia型超新星2017 erp的紫外线
Red and Reddened: Ultraviolet through Near-Infrared Observations of Type Ia Supernova 2017erp
摘要：
我们提出了空间为基础的紫外/光学光度学和光谱学与斯威夫特紫外/光学望远镜和哈勃太空望远镜，分别与地面为基础的光学光度学和光谱学和近红外光谱的超新星SN 2017 erp。它的光学光变曲线和光谱与正常的Ia型超新星（SN Ia）一致。与以前的近紫外（NUV）光度样本相比，SN 2017 erp在校正银河系和宿主尘埃变红后具有类似于NUV红色类别的颜色。我们发现SN 2017 erp和NUV-蓝SN 2011 fe之间的差异与单独的尘埃红化不一致，但类似于SALT颜色定律，来自更高红移的SNe Ia的静止帧紫外光度法。这种色差主要由紫外线的内在差异决定，只有一小部分来自预期的尘埃变红。区分这两个可以有重要的后果，确定宇宙学距离与静止框架紫外测光。这个光谱系列对于分析具有本质上更红的NUV颜色的SNe Ia是重要的。我们还展示了模型比较，表明金属丰度可能是NUV-蓝色和NUV-红色SNe Ia之间的物理差异，来自3000埃附近的反向荧光的发射峰意味着SN 2017 erp上层的金属丰度比SN 2011 fe高10倍。然而，金属丰度估计值非常依赖于模型，并且在紫外线中存在多种效应。需要进一步的模型和Ia超新星的紫外光谱来探索Ia超新星的多样性，这些模型和光谱在近紫外峰和中紫外通量水平上显示出看似独立的差异。
英文摘要：
We present space-based ultraviolet/optical photometry and spectroscopy with the Swift Ultra-Violet/Optical Telescope and Hubble Space Telescope, respectively, along with ground-based optical photometry and spectroscopy and near-infrared spectroscopy of supernova SN2017erp. The optical light curves and spectra are consistent with a normal Type Ia supernova (SN Ia). Compared to previous photometric samples in the near-ultraviolet (NUV), SN2017erp has colors similar to the NUV-red category after correcting for Milky Way and host dust reddening. We find the difference between SN2017erp and the NUV-blue SN2011fe is not consistent with dust reddening alone but is similar to the SALT color law, derived from rest-frame UV photometry of higher redshift SNe Ia. This chromatic difference is dominated by the intrinsic differences in the UV and only a small contribution from the expected dust reddening. Differentiating the two can have important consequences for determining cosmological distances with rest-frame UV photometry. This spectroscopic series is important for analyzing SNe Ia with intrinsically redder NUV colors. We also show model comparisons suggesting that metallicity could be the physical difference between NUV-blue and NUV-red SNe Ia, with emission peaks from reverse fluorescence near 3000 Angstroms implying a factor of ten higher metallicity in the upper layers of SN2017erp compared to SN~2011fe. Metallicity estimates are very model dependent however, and there are multiple effects in the UV. Further models and UV spectra of SNe Ia are needed to explore the diversity of SNe Ia which show seemingly independent differences in the near-UV peaks and mid-UV flux levels.
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