Ia型超新星及其环境中的窄吸收线：III
Narrow absorption lines from intervening material in supernovae: III. Supernovae and their environments
AI总结：
研究Ia型超新星在静止环境中窄吸收线强度较低，揭示其星际气体含量较低，同时发现II型超新星的钠I D等效宽度分布低于Ia-SF和剥离包层超新星，暗示吸收来源可能来自爆炸附近物质。
摘要：
Ia型超新星（SNe Ia）在静止星系中表现出显著较弱的窄星际吸收特征，相比核心坍缩型超新星（CC-SNe）和Ia-SF型超新星，表明静止环境中星际气体含量较低。在恒星形成宿主中，II型超新星的钠I D等效宽度分布低于Ia-SF和剥离包层超新星（SE-SNe）。这一结果令人意外，因为CC-SNe通常与恒星形成区域相关，位于银河盘内更深处，应有更强的视线消光。这表明观察到的行为不能仅由视线方向的积分星际介质（ISM）吸收解释。若部分吸收来自爆炸附近的物质，Ia-SF和SE-SNe的钠I D EW分布相似性暗示不同前身路径可能产生相似吸收特征。可能的解释包括：(a) 前身系统爆炸前释放的 circumstellar 物质 (CSM)，或 (b) 超新星辐射与附近斑驳的ISM云相互作用。本研究强调星际吸收特征在揭示超新星多样环境和前身路径中的诊断作用。
英文摘要：
Narrow interstellar absorption features in supernova (SN) spectra serve as valuable diagnostics for probing dust extinction and the presence of circumstellar or interstellar material. In this third paper in a series, we investigate how the strength of narrow interstellar absorption lines in low-resolution spectra varies with SN type and host galaxy properties, both on local and global scales. Using a dataset of over 10000 spectra from $\sim1800$ low-redshift SNe, we find that Type Ia SNe (SNe Ia) in passive galaxies exhibit significantly weaker narrow absorption features compared to CC-SNe and SNe Ia in star-forming hosts (SNe Ia-SF), suggesting lower interstellar gas content in quiescent environments. Within the star-forming hosts, the Na I D equivalent-width distribution of SNe II is much lower than that of both SNe Ia-SF and stripped-envelope SNe (SE-SNe). This result is somewhat unexpected, since CC-SNe are generally associated with star-forming regions and occur deeper within galactic disks, where stronger line-of-sight extinction would be anticipated. This suggests that the observed behaviour cannot be explained solely by absorption from the integrated interstellar medium (ISM) along the line of sight. Instead, if part of the absorption arises from material near the explosion, the similarity between the Na I D EW distributions of SNe Ia-SF and SE-SNe implies that comparable absorption signatures can emerge from distinct progenitor pathways. Possible explanations include (a) circumstellar material (CSM) expelled by the progenitor system before explosion, or (b) interaction of SN radiation with nearby patchy ISM clouds. Our results highlight the diagnostic power of interstellar absorption features in revealing the diverse environments and progenitor pathways of SNe.
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