晚发的星周介质相互作用是罕见的：Ia型超新星的无偏见的GALEX观点
Late-Onset Circumstellar Medium Interactions are Rare: An Unbiased GALEX View of Type Ia Supernovae
摘要：
使用紫外光变曲线，我们限制1080 Ia型超新星（SNe Ia）的拱星环境内$z<0.5$从档案星系演化探测器（GALEX）的观测。所有的Ia型超新星都需要在爆炸前和爆炸后进行GALEX观测，以确保适当地减去宿主星系的流量。使用晚时间GALEX观测，我们期待从SN喷出物和拱星材料（CSM）之间的任何相互作用的紫外线过剩。四个超新星Ia检测到接近最大光，我们比较GALEX测光档案数据，但我们发现没有一个我们的目标显示令人信服的证据CSM相互作用。最近哈勃太空望远镜（HST）的一次巡天估计，Ia型超新星的$\sim6\%$可能与遥远的CSM相互作用，但由于样本量小和选择效应，统计推断变得复杂。通过将模型光变曲线注入到我们的数据中，然后恢复它们，我们根据CSM相互作用的开始时间和最大光度来约束广泛的CSM相互作用。结合我们的GALEX未检测与HST结果，我们将具有中度CSM相互作用的SNe Ia中迟发性CSM相互作用的发生限制为$90\%$置信度下发现后$0-500$天之间的$f_\text{CSM}\lesssim5.1\%$和发现后$500-1000$天之间的$\lesssim2.7\%$，与在PTF 11 kx中观察到的相似。对于与SN 2015 cp类似的较弱CSM相互作用，我们分别获得了相同时间范围内$\lesssim16\%$和$\lesssim4.8\%$的极限。
英文摘要：
Using ultraviolet (UV) light curves we constrain the circumstellar environments of 1080 Type Ia supernovae (SNe Ia) within $z<0.5$ from archival Galaxy Evolution Explorer (GALEX) observations. All SNe Ia are required to have pre- and post-explosion GALEX observations to ensure adequate subtraction of the host-galaxy flux. Using the late-time GALEX observations we look for the UV excess expected from any interaction between the SN ejecta and circumstellar material (CSM). Four SNe Ia are detected near maximum light and we compare the GALEX photometry to archival data, but we find none of our targets show convincing evidence of CSM interaction. A recent Hubble Space Telescope (HST) survey estimates that $\sim6\%$ of SNe Ia may interact with distant CSM, but statistical inferences are complicated by the small sample size and selection effects. By injecting model light curves into our data and then recovering them, we constrain a broad range of CSM interactions based on the CSM interaction start time and the maximum luminosity. Combining our GALEX non-detections with the HST results, we constrain occurrence of late-onset CSM interaction among SNe Ia with moderate CSM interaction, similar to that observed in PTF11kx, to $f_\text{CSM}\lesssim5.1\%$ between $0-500$ days after discovery and $\lesssim2.7\%$ between $500-1000$ days after discovery at $90\%$ confidence. For weaker CSM interactions similar to SN 2015cp, we obtain limits of $\lesssim16\%$ and $\lesssim4.8\%$, respectively, for the same time ranges.
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