UNCOVERING THE PUTATIVE B-STAR BINARY COMPANION OF THE SN 1993J PROGENITOR
UNCOVERING THE PUTATIVE B-STAR BINARY COMPANION OF THE SN 1993J PROGENITOR
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DOI：
10.1088/0004-637x/790/1/17
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发表时间：
2014-05
期刊：
影响因子：
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通讯作者：
O. Fox;K. Azalee Bostroem;S. V. van Dyk;A. Filippenko;C. Fransson;T. Matheson;S. Bradley Cenko;P. Chandra;V. Dwarkadas;Weidong Li;A. Parker;N. Smith
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文献类型：
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作者：
O. Fox;K. Azalee Bostroem;S. V. van Dyk;A. Filippenko;C. Fransson;T. Matheson;S. Bradley Cenko;P. Chandra;V. Dwarkadas;Weidong Li;A. Parker;N. Smith
IIb型超新星（SN）1993 J是仅有的几颗在爆炸前的图像中发现了一颗祖星星的剥离包层超新星之一。SN IIb模型通常通过二元系统中的传质调用H包络剥离。对于SN 1993J的情况，模型表明伴星增长到22 M的辐射，并成为紫外线（UV）过剩的来源。SN 1993 J位于M81，距离只有3.6 Mpc，提供了探测推定伴星和测试祖先模型的最佳机会。先前在2004年发表的近紫外光谱显示出与热（B2 Ia）星星相一致的吸收线的证据，但该领域是拥挤的，并由来自SN的通量主导。在这里，我们介绍了哈勃太空望远镜宇宙起源光谱仪和宽视场相机3从2012年开始对SN 1993J的观测，当时SN的通量已经足够褪色，可以潜在地测量来自推定伴星的紫外连续谱特性。由此产生的紫外光谱与来自热B星星和SN的贡献一致，尽管我们不能排除视线重合。
The Type IIb supernova (SN) 1993J is one of only a few stripped-envelope SNe with a progenitor star identified in pre-explosion images. SN IIb models typically invoke H envelope stripping by mass transfer in a binary system. For the case of SN 1993J, the models suggest that the companion grew to 22 M☉ and became a source of ultraviolet (UV) excess. Located in M81, at a distance of only 3.6 Mpc, SN 1993J offers one of the best opportunities to detect the putative companion and test the progenitor model. Previously published near-UV spectra in 2004 showed evidence for absorption lines consistent with a hot (B2 Ia) star, but the field was crowded and dominated by flux from the SN. Here we present Hubble Space Telescope Cosmic Origins Spectrograph and Wide-Field Camera 3 observations of SN 1993J from 2012, at which point the flux from the SN had faded sufficiently to potentially measure the UV continuum properties from the putative companion. The resulting UV spectrum is consistent with contributions from both a hot B star and the SN, although we cannot rule out line-of-sight coincidences.