标题： 詹姆斯韦伯空间望远镜与地面观测对Iax型超新星SN 2024pxl和SN 2024vjm：弱爆燃爆炸的证据 显示英文标题

标题： JWST and Ground-based Observations of the Type Iax Supernovae SN 2024pxl and SN 2024vjm: Evidence for Weak Deflagration Explosions

摘要： 我们展示了针对中间亮度Iax型超新星（SN Iax）2024pxl和极低亮度SN Iax 2024vjm的全波段光学、$+$近红外（NIR）、$+$中红外（MIR）观测。JWST观测提供了SN Iax前所未有的MIR光谱，时间跨度从$+$到$+$天（最大光度之后）。我们在这些早期阶段于MIR中探测到了禁线发射线，而此时光学和NIR则以具有吸收成分的允许线为主导。因此，早期阶段的全波段光谱可以同时显示弥漫区和光球区的谱线，从而探测喷发物的内外层。 我们识别出在SN Iax中之前未见过的光谱线，包括[Mg II] 4.76 $\mu$m, [Mg II] 9.71 $\mu$m, [Ne II] 12.81 $\mu$m，以及追踪未燃烧物质的孤立O I 2.76 $\mu$m线。所有物种的禁戒发射线都呈现中心峰值，并具有相似的动力学分布，表明喷发物在这两种超新星（SN 2024pxl 和 SN 2024vjm）中混合良好，这是纯爆燃爆炸模型的一个标志。SN 2024pxl 的辐射转移建模显示与接近钱德拉塞卡质量白矮星的弱爆燃有很好的一致性，但为了匹配观测结果还需要额外的红外通量，这可能归因于幸存的残骸。尽管亮度差异很大，但我们倾向于认为SN 2024vjm 来源于弱爆燃，因为它的全波段光谱与SN 2024pxl 非常相似。然而，我们的比较模型都比SN 2024vjm 更亮且衰减更快；未来的建模应考虑更弱的爆炸和束缚残骸的贡献。我们的观测展示了全波段光谱在揭示热核超新星爆炸物理方面的诊断能力。 显示英文摘要

摘要： We present panchromatic optical $+$ near-infrared (NIR) $+$ mid-infrared (MIR) observations of the intermediate-luminosity Type Iax supernova (SN Iax) 2024pxl and the extremely low-luminosity SN Iax 2024vjm. JWST observations provide unprecedented MIR spectroscopy of SN Iax, spanning from $+$11 to $+$42 days past maximum light. We detect forbidden emission lines in the MIR at these early times while the optical and NIR are dominated by permitted lines with an absorption component. Panchromatic spectra at early times can thus simultaneously show nebular and photospheric lines, probing both inner and outer layers of the ejecta. We identify spectral lines not seen before in SN Iax, including [Mg II] 4.76 $\mu$m, [Mg II] 9.71 $\mu$m, [Ne II] 12.81 $\mu$m, and isolated O I 2.76 $\mu$m that traces unburned material. Forbidden emission lines of all species are centrally peaked with similar kinematic distributions, indicating that the ejecta are well mixed in both SN 2024pxl and SN 2024vjm, a hallmark of pure deflagration explosion models. Radiative transfer modeling of SN 2024pxl shows good agreement with a weak deflagration of a near-Chandrasekhar-mass white dwarf, but additional IR flux is needed to match the observations, potentially attributable to a surviving remnant. We favor a weak deflagration origin for SN 2024vjm because of its panchromatic spectral similarity to SN 2024pxl, despite the large difference in luminosity. However, our comparison weak deflagration models are all too luminous and rapidly fading compared to SN 2024vjm; future modeling should push to even weaker explosions and include the contribution of a bound remnant. Our observations demonstrate the diagnostic power of panchromatic spectroscopy for unveiling explosion physics in thermonuclear supernovae.