Bump Morphology of the CMAGIC Diagram
Bump Morphology of the CMAGIC Diagram
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DOI：
10.3847/1538-4357/acad78
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发表时间：
2022-10
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通讯作者：
L. Aldoroty;L. Wang;P. Hoeflich;J. Yang;N. Suntzeff;G. Aldering;P. Antilogus;C. Aragon;S. Bailey;C. Baltay;S. Bongard;Kyle Boone;C. Buton;Y. Copin;S. Dixon;D. Fouchez;E. Gangler;R. Gupta;B. Hayden;Mitchell Karmen;A. Kim;M. Kowalski;D. Kusters;P. L'eget;F. Mondon;J. Nordin;R. Pain;E. Pecontal;R. Pereira;S. Perlmutter;K. Ponder;D. Rabinowitz;M. Rigault;D. Rubin;K. Runge;C. Saunders;G. Smadja;N. Suzuki;C. Tao;R. Thomas;M. Vincenzi
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作者：
L. Aldoroty;L. Wang;P. Hoeflich;J. Yang;N. Suntzeff;G. Aldering;P. Antilogus;C. Aragon;S. Bailey;C. Baltay;S. Bongard;Kyle Boone;C. Buton;Y. Copin;S. Dixon;D. Fouchez;E. Gangler;R. Gupta;B. Hayden;Mitchell Karmen;A. Kim;M. Kowalski;D. Kusters;P. L'eget;F. Mondon;J. Nordin;R. Pain;E. Pecontal;R. Pereira;S. Perlmutter;K. Ponder;D. Rabinowitz;M. Rigault;D. Rubin;K. Runge;C. Saunders;G. Smadja;N. Suzuki;C. Tao;R. Thomas;M. Vincenzi
我们应用色星等截距校准方法（CMAGIC）的近超新星工厂SNe Ia分光光度数据集。目前存在的CMAGIC参数是拟合颜色-星等图中线性区域的直线的斜率和截距，其发生在最大亮度之后大约30天的跨度内。我们定义了一个新的参数ω XY，即任意滤波器X和Y的最大亮度附近的“凸起”特征的大小。我们发现CMAGIC图中线性区域的斜率β XY与ω XY之间存在显著的相关性。这些结果可以用于我们的优势，因为它们比定义为时间函数的参数受消光的影响更小。此外，ω XY是独立于模板计算的。我们发现，目前的经验模板是成功的复制在这项工作中描述的功能，特别是SALT 3，它正确地展示了我们的数据中看到的斜率和“凸点”大小之间的负相关性。在1D模拟中，我们表明，“凸点”特征的大小和β XY之间的相关性可以理解为由于大尺度瑞利-泰勒不稳定性引起的化学混合的结果。
We apply the color–magnitude intercept calibration method (CMAGIC) to the Nearby Supernova Factory SNe Ia spectrophotometric data set. The currently existing CMAGIC parameters are the slope and intercept of a straight line fit to the linear region in the color–magnitude diagram, which occurs over a span of approximately 30 days after maximum brightness. We define a new parameter, ω XY , the size of the “bump” feature near maximum brightness for arbitrary filters X and Y. We find a significant correlation between the slope of the linear region, β XY , in the CMAGIC diagram and ω XY . These results may be used to our advantage, as they are less affected by extinction than parameters defined as a function of time. Additionally, ω XY is computed independently of templates. We find that current empirical templates are successful at reproducing the features described in this work, particularly SALT3, which correctly exhibits the negative correlation between slope and “bump” size seen in our data. In 1D simulations, we show that the correlation between the size of the “bump” feature and β XY can be understood as a result of chemical mixing due to large-scale Rayleigh–Taylor instabilities.