Significant luminosity differences of two twin Type Ia supernovae
Significant luminosity differences of two twin Type Ia supernovae
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两颗孪生 Ia 型超新星的显着光度差异
DOI：
10.1093/mnras/stz3324
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发表时间：
2019
影响因子：
4.8
通讯作者：
Milne, Peter A.
中科院分区：
文献类型：
--
作者：
Foley, Ryan J.;Hoffmann, Samantha L.;Macri, Lucas M.;Riess, Adam G.;Brown, Peter J.;Filippenko, Alexei V.;Graham, Melissa L.;Milne, Peter A.
NGC 3972 中的 Ia 型超新星 (SNe Ia) 2011by 和 M101 中的 2011fe 是光学“双胞胎”，具有几乎相同的光学光曲线形状、颜色和接近最大亮度的光谱。然而，SN 2011fe 的紫外线（UV；1600 < λ < 2500 Å）通量明显高于 SN 2011by 之前和峰值光度时的通量。一些理论模型预测，具有较高前身金属丰度的超新星 Ia 应该 (1) 具有额外的紫外线不透明度，从而降低紫外线通量； (2) 具有基本不变的光谱能量分布； (3)具有相似的光学光曲线形状； (4)由于过量的中子，以放射性56 Ni为代价产生更稳定的Fe族元素，因此具有较低的峰值光度。根据这些预测，Foley 和 Kirshner 认为 SNe 2011by 和 2011fe 之间的紫外线通量差异是由于它们的前身具有显着不同的金属丰度的结果。他们还测量了超新星峰值绝对星等之间的巨大但微不足道的差异（ΔMV，峰值= 0.60 ± 0.36 星等），其中 SN 2011fe 更亮。我们提出了一种新的基于造父变星的 NGC 3972 距离，大大提高了 SN 2011by 的距离测量精度。利用这些新数据，我们确定超新星具有显着不同的峰值光度（ΔMV，峰值= 0.335 ± 0.069 mag）。因此，SN 2011fe 比 SN 2011by 多产生了 38% 的 56Ni，这与这些 SNe 的前体金属丰度差异的预测一致，尽管替代模型也可以解释这种差异。我们讨论了前身金属丰度差异如何影响光曲线形状校正的超新星光度的固有散射、使用“孪生”超新星测量距离，以及使用超新星 Ia 约束宇宙学参数的影响。
The Type Ia supernovae (SNe Ia) 2011by, hosted in NGC 3972, and 2011fe, hosted in M101, are optical ‘twins,’ having almost identical optical light-curve shapes, colours, and near-maximum-brightness spectra. However, SN 2011fe had significantly more ultraviolet (UV; 1600 < λ < 2500 Å) flux than SN 2011by before and at peak luminosity. Several theoretical models predict that SNe Ia with higher progenitor metallicity should (1) have additional UV opacity and thus lower UV flux; (2) have an essentially unchanged optical spectral-energy distribution; (3) have a similar optical light-curve shape; and (4) because of the excess neutrons, produce more stable Fe-group elements at the expense of radioactive56Ni and thus have a lower peak luminosity. Following these predictions, Foley and Kirshner suggested that the difference in UV flux between SNe 2011by and 2011fe was the result of their progenitors having significantly different metallicities. They also measured a large, but insignificant, difference between the peak absolute magnitudes of the SNe (ΔMV, peak= 0.60 ± 0.36 mag), with SN 2011fe being more luminous. We present a new Cepheid-based distance to NGC 3972, substantially improving the precision of the distance measurement for SN 2011by. With these new data, we determine that the SNe have significantly different peak luminosities (ΔMV, peak= 0.335 ± 0.069 mag). Consequently, SN 2011fe produced 38 per cent more56Ni than SN 2011by, consistent with predictions for progenitor metallicity differences for these SNe, although alternative models may also explain this difference. We discuss how progenitor metallicity differences can contribute to the intrinsic scatter for light-curve-shape-corrected SN luminosities, the use of ‘twin’ SNe for measuring distances, and implications for using SNe Ia for constraining cosmological parameters.
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DOI：
10.1111/j.1365-2966.2012.21928.x
发表时间：
2012-08
影响因子：
4.8
作者：
E. Walker;S. Hachinger;P. Mazzali;R. Ellis;M. Sullivan;A. Gal-yam;D. Howell
通讯作者：
E. Walker;S. Hachinger;P. Mazzali;R. Ellis;M. Sullivan;A. Gal-yam;D. Howell
DOI：
10.1111/j.1745-3933.2006.00165.x
发表时间：
2006-04
影响因子：
--
作者：
P. Mazzali;P. Podsiadlowski
通讯作者：
P. Mazzali;P. Podsiadlowski
附近超新星工厂 SN 2011fe 的分光光度时间序列
DOI：
10.1051/0004-6361/201221008
发表时间：
2013-02
期刊：
Astronomy & Astrophysics
影响因子：
--
作者：
Tao, C.;Taubenberger, S.;Tilquin, A.;Wu, C.
通讯作者：
Wu, C.
宇宙中的超新星
DOI：
--
发表时间：
2006
期刊：
影响因子：
--
作者：
Kohsuke Sumiyoshi;Shigehiro Nagataki;山田章一;Shoichi Yamada;Shoichi Yamada;Shoichi Yamada;山田章一;Shoichi Yamada
通讯作者：
Shoichi Yamada
DOI：
--
发表时间：
1999-05
期刊：
--
影响因子：
--
作者：
E. Lentz;E. Baron;D. Branch;P. Hauschildt;P. Nugent
通讯作者：
E. Lentz;E. Baron;D. Branch;P. Hauschildt;P. Nugent