THE FIRST MAXIMUM-LIGHT ULTRAVIOLET THROUGH NEAR-INFRARED SPECTRUM OF A TYPE Ia SUPERNOVA,
THE FIRST MAXIMUM-LIGHT ULTRAVIOLET THROUGH NEAR-INFRARED SPECTRUM OF A TYPE Ia SUPERNOVA,
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DOI：
10.1088/2041-8205/753/1/l5
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发表时间：
2012-02
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影响因子：
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通讯作者：
R. Foley;M. Kromer;G. H. Marion;G. Pignata;M. Stritzinger;S. Taubenberger;P. Challis;A. Filippenko;G. Folatelli;W. Hillebrandt;E. Hsiao;R. Kirshner;Weidong Li;N. Morrell;F. Roepke;F. Ciaraldi-Schoolmann;I. Seitenzahl;J. Silverman;R. Simcoe;Z. K. Berta;K. Ivarsen;E. Newton;M. Nysewander;D. Reichart
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文献类型：
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作者：
R. Foley;M. Kromer;G. H. Marion;G. Pignata;M. Stritzinger;S. Taubenberger;P. Challis;A. Filippenko;G. Folatelli;W. Hillebrandt;E. Hsiao;R. Kirshner;Weidong Li;N. Morrell;F. Roepke;F. Ciaraldi-Schoolmann;I. Seitenzahl;J. Silverman;R. Simcoe;Z. K. Berta;K. Ivarsen;E. Newton;M. Nysewander;D. Reichart
我们给出了第一个通过近红外(NIR)的Ia型超新星(SN Ia)的最大光紫外线(UV)光谱。SN2011IV的这一光谱是由哈勃太空望远镜在紫外/光学波长和麦哲伦·巴德望远镜在近红外波长几乎同时获得的。这些数据提供了检查整个最大光强Sn Ia光谱能量分布的机会。由于锡Ia光谱的紫外区对爆炸外层的成分极其敏感，而外层在较长的波长下是透明的，这一史无前例的光谱可以对锡抛射物的成分提供强有力的限制，同样地，锡爆炸和前驱系统也是如此。SN2011iv在光谱上是正常的，但有相对较快的下降(ΔM15(B)=1.69±0.05mag)。我们比较了SN2011IV和其他SNE Ia的紫外光谱接近最大光，并检查了UV光谱特性、光曲线形状和喷出速度之间的趋势。我们初步发现，具有相似的光曲线形状但不同的抛射速度的SNE具有相似的紫外光谱，而具有相似的抛射速度但不同的光曲线形状的SNE具有非常不同的紫外光谱。通过与爆炸模型的比较，我们发现太阳金属丰度W7和零金属丰度延迟爆轰模型对SN2011IV从紫外到近红外的光谱都提供了合理的拟合。
We present the first maximum-light ultraviolet (UV) through near-infrared (NIR) Type Ia supernova (SN Ia) spectrum. This spectrum of SN 2011iv was obtained nearly simultaneously by the Hubble Space Telescope at UV/optical wavelengths and the Magellan Baade telescope at NIR wavelengths. These data provide the opportunity to examine the entire maximum-light SN Ia spectral energy distribution. Since the UV region of an SN Ia spectrum is extremely sensitive to the composition of the outer layers of the explosion, which are transparent at longer wavelengths, this unprecedented spectrum can provide strong constraints on the composition of the SN ejecta, and similarly the SN explosion and progenitor system. SN 2011iv is spectroscopically normal, but has a relatively fast decline (Δm15(B) = 1.69 ± 0.05 mag). We compare SN 2011iv to other SNe Ia with UV spectra near maximum light and examine trends between UV spectral properties, light-curve shape, and ejecta velocity. We tentatively find that SNe with similar light-curve shapes but different ejecta velocities have similar UV spectra, while those with similar ejecta velocities but different light-curve shapes have very different UV spectra. Through a comparison with explosion models, we find that both a solar-metallicity W7 and a zero-metallicity delayed-detonation model provide a reasonable fit to the spectrum of SN 2011iv from the UV to the NIR.