标题： II型超新星2010jl的候选前体不是光学明亮的恒星 显示英文标题

标题： The Candidate Progenitor of the Type IIn SN 2010jl is Not an Optically Luminous Star

摘要： IIn型超新星（SN）子类的前身星（或系统）的性质仍然不确定。 虽然至少有四颗IIn型超新星的前身星有直接成像限制，其中一个是SN 2010jl，但在不稳定前身星和爆炸事件本身的解释上仍存在歧义。 在爆炸前的HST/WFPC2图像中有一个蓝色源位于SN 2010jl爆炸后的地面成像所得到的5 sigma天体测量误差圆内。 然而，在地面天体测量结果发表时，SN尚未暗淡到足以让爆炸后的HST后续观测确定更精确的天体测量解和/或确认爆炸前的源是否消失，这两点对于最终区分可能的前身星情景是必要的。 在这里，我们展示了2014年和2015年获得的SN 2010jl区域的HST/WFC3成像，此时SN已经足够暗淡，可以对前身星提出新的限制。 新图像中仍然检测到SN，它与贡献了至少部分甚至全部的蓝色源（之前在WFPC2数据中被建议为候选前身星）的底层和扩展发射源相比偏移了0.099 +/- 0.008（24 +/- 2 pc）。 仅这一点就排除了爆炸前图像中的蓝色源是爆炸恒星的可能性，但可能表明与一个年轻（<5-6 Myr）的星团有关，并且仍然支持一个质量大于30倍太阳质量的前身星。 我们获得了在爆炸前的WFPC2和Spitzer/IRAC图像中位于SN位置的单个恒星的通量新上限，这些上限最终可用于限制前身星特性。 显示英文摘要

摘要： The nature of the progenitor star (or system) for the Type IIn supernova (SN) subclass remains uncertain. While there are direct imaging constraints on the progenitors of at least four Type IIn supernovae, one of them being SN 2010jl, ambiguities remain in the interpretation of the unstable progenitors and the explosive events themselves. A blue source in pre-explosion HST/WFPC2 images falls within the 5 sigma astrometric error circle derived from post-explosion ground-based imaging of SN 2010jl. At the time the ground-based astrometry was published, however, the SN had not faded sufficiently for post-explosion HST follow-up observations to determine a more precise astrometric solution and/or confirm if the pre-explosion source had disappeared, both of which are necessary to ultimately disentangle the possible progenitor scenarios. Here we present HST/WFC3 imaging of the SN 2010jl field obtained in 2014 and 2015, when the SN had faded sufficiently to allow for new constraints on the progenitor. The SN, which is still detected in the new images, is offset by 0."099 +/- 0."008 (24 +/- 2 pc) from the underlying and extended source of emission that contributes at least partially, if not entirely, to the blue source previously suggested as the candidate progenitor in the WFPC2 data. This point alone rules out the possibility that the blue source in the pre-explosion images is the exploding star, but may instead suggest an association with a young (<5-6 Myr) cluster and still argues for a massive (>30 solar masses) progenitor. We obtain new upper limits on the flux from a single star at the SN position in the pre-explosion WFPC2 and Spitzer/IRAC images that may ultimately be used to constrain the progenitor properties.