AI 中文总结
该研究通过JWST光谱等观测，确认SN 2010jl产生大量激波后尘埃，证实强星周物质相互作用可高效产尘，或对早期宇宙星系尘埃有重要贡献。
AI 中文摘要
我们呈现了SN 2010jl遗迹源的JWST中红外光谱与地基光学光谱，SN 2010jl是一颗相对邻近的超亮IIn型超新星，与星周物质（CSM）存在强相互作用。早期数据显示存在尘埃，其来源被解释为要么是预先存在的星周物质尘埃，要么是超新星抛射体及激波后区域中新形成的尘埃。爆炸后13年，JWST探测到来自暖尘埃的强中红外过量辐射，在10-15μm处有宽特征。我们的分析显示，尘埃质量最小值大于0.11倍太阳质量（$M_{\rm \text{⊙}}$），更可能为0.2倍太阳质量或更高，因为该尘埃是光学厚的。这是在未使用远红外/亚毫米数据的情况下测得的最大超新星产生尘埃质量之一，且远超爆炸后2-3年推算出的SN 2010jl尘埃质量。地基光学光谱证实SN位置存在年轻大质量星团，并确认持续到最晚时标的蓝移线轮廓源于激波后区域形成的尘埃，发射中红外的最暖尘埃可能就是导致蓝移的同一激波后尘埃。JWST光谱还显示硅酸盐吸收，可能源于沿退行激波视线方向的冷超新星抛射体尘埃。SN 2010jl的大量激波后尘埃表明，强星周物质相互作用可促进高效尘埃产生，且新形成的激波后尘埃能留存；若强相互作用超新星在早期宇宙中普遍存在，可能对幼年星系中的尘埃有重要贡献。
英文摘要
We present new JWST mid-IR spectra and ground-based optical spectra of the lingering source at the position of SN 2010jl, which was a relatively nearby superluminous Type IIn supernova having strong interaction with circumstellar material (CSM). Early-time data showed evidence of dust, interpreted as either pre-existing CSM dust, or as newly formed dust in the SN ejecta and post-shock region. At 13 yr post explosion, JWST reveals a strong MIR excess from warm dust, with broad features at 10-15 $μ$m. Our analysis reveals a minimum dust mass of $>$0.11 $M_{\odot}$, and a more likely value of 0.2 $M_{\odot}$ or more because the dust is optically thick. This is among the largest masses of SN-produced dust yet measured without far-IR/submm data, and greatly exceeds SN 2010jl's dust mass inferred around 2-3 yr post-explosion. Ground-based optical spectra confirm the presence of a young massive cluster at the SN position, and confirm that blueshifted line profiles persisting until the latest epochs arise from dust formed in the post-shock region. The warmest dust emitting in the MIR is likely to be the same post-shock dust causing the blueshift. The JWST spectrum also reveals silicate absorption, which may arise from cool SN ejecta dust along the line of sight to the receding shock. The large mass of post-shock dust in SN 2010jl suggests that strong CSM interaction promotes efficient dust production, where the new post-shock dust will survive. If strongly interacting SNe are common in the early Universe, this may contribute significantly to dust seen in infant galaxies.
CommentsAccepted by ApJ
