D. A. Howell, A. Conley, M. Della Valle, P. E. Nugent, S. Perlmutter, G. H. Marion, K. Krisciunas, C. Badenes, P. Mazzali, G. Aldering, P. Antilogus, E. Baron, … 展开作者
D. A. Howell, A. Conley, M. Della Valle, P. E. Nugent, S. Perlmutter, G. H. Marion, K. Krisciunas, C. Badenes, P. Mazzali, G. Aldering, P. Antilogus, E. Baron, A. Becker, C. Baltay, S. Benetti, S. Blondin, D. Branch, E. F. Brown, S. Deustua, A. Ealet, R. S. Ellis, D. Fouchez, W. Freedman, A. Gal-Yam, S. Jha, D. Kasen, R. Kessler, A. G. Kim, D. C. Leonard, W. Li, M. Livio, D. Maoz, F. Mannucci, T. Matheson, J. D. Neill, K. Nomoto, N. Panagia, K. Perrett, M. Phillips, D. Poznanski, R. Quimby, A. Rest, A. Riess, M. Sako, A. M. Soderberg, L. Strolger, R. Thomas, M. Turatto, S. van Dyk, W. M. Wood-Vasey
In the next decade Type Ia supernovae (SNe Ia) will be used to test theories predicting changes in the Dark Energy equation of state with time. Ultimately this requires a dedicated space mission like JDEM. SNe Ia are mature cosmological probes --- their limitations are well characterized, and a path to improvement is clear. Dominant systematic errors include photometric calibration, selection effects, reddening, and population-dependent differences. Building on past lessons, well-controlled new surveys are poised to make strides in these areas: the Palomar Transient Factory, Skymapper, La Silla QUEST, Pan-STARRS, the Dark Energy Survey, LSST, and JDEM. They will obviate historical calibrations and selection biases, and allow comparisons via large subsamples. Some systematics follow from our ignorance of SN Ia progenitors, which there is hope of determining with SN Ia rate studies from 0<z<4.
Aside from cosmology, SNe Ia regulate galactic and cluster chemical evolution, inform stellar evolution, and are laboratories for extreme physics. Essential probes of SNe Ia in these contexts include spectroscopy from the UV to the IR, X-ray cluster and SN remnant observations, spectropolarimetry, and advanced theoretical studies. While there are an abundance of discovery facilities planned, there is a deficit of follow-up resources. Living in the systematics era demands deep understanding rather than larger statistics. NOAO ReSTAR initiative to build 2-4m telescopes would provide necessary follow-up capability. Finally, to fully exploit LSST, well-matched wide-field spectroscopic capabilities are desirable.
Supernova lightCURVE POPulation Synthesis I: including interacting binaries is key to understanding the diversity of type II supernova lightcurves
我们提出的超新星光变曲线人口合成的结果，预测可能的超新星光变曲线的范围所产生的人口的祖星，包括相互作用的二元系统。我们发现，已知的超新星光变曲线的多样性可以被解释为产生的二元相互作用。给出祖星的详细模型，我们能够确定这些恒星中的哪些参数决定了它们超新星光变曲线的形状。主要的因素是超新星喷出物的质量和最后祖先中氢的质量。我们发现，有一个连续的光变曲线的行为，从IIP型，IIL IIb超新星有关的氢和喷出物的质量范围。大多数IIb型超新星的初始质量范围相对较窄，从10到15 M $_{\odot}$。我们还发现了一些明显的光变曲线，这是恒星合并的结果。
