تقرير
The late-time light curve of the type Ia supernova SN 2011fe
| العنوان: | The late-time light curve of the type Ia supernova SN 2011fe |
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| المؤلفون: | Dimitriadis, G., Sullivan, M., Kerzendorf, W., Ruiter, A. J., Seitenzahl, I. R., Taubenberger, S., Doran, G. B., Gal-Yam, A., Laher, R. R., Maguire, K., Nugent, P., Ofek, E. O., Surace, J. |
| سنة النشر: | 2017 |
| المجموعة: | Astrophysics |
| مصطلحات موضوعية: | Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics |
| الوصف: | We present late-time optical $R$-band imaging data from the Palomar Transient Factory (PTF) for the nearby type Ia supernova SN 2011fe. The stacked PTF light curve provides densely sampled coverage down to $R\simeq22$ mag over 200 to 620 days past explosion. Combining with literature data, we estimate the pseudo-bolometric light curve for this event from 200 to 1600 days after explosion, and constrain the likely near-infrared contribution. This light curve shows a smooth decline consistent with radioactive decay, except over ~450 to ~600 days where the light curve appears to decrease faster than expected based on the radioactive isotopes presumed to be present, before flattening at around 600 days. We model the 200-1600d pseudo-bolometric light curve with the luminosity generated by the radioactive decay chains of $^{56}$Ni, $^{57}$Ni and $^{55}$Co, and find it is not consistent with models that have full positron trapping and no infrared catastrophe (IRC); some additional energy escape other than optical/near-IR photons is required. However, the light curve is consistent with models that allow for positron escape (reaching 75% by day 500) and/or an IRC (with 85% of the flux emerging in non-optical wavelengths by day 600). The presence of the $^{57}$Ni decay chain is robustly detected, but the $^{55}$Co decay chain is not formally required, with an upper mass limit estimated at 0.014 M$_{\odot}$. The measurement of the $^{57}$Ni/$^{56}$Ni mass ratio is subject to significant systematic uncertainties, but all of our fits require a high ratio >0.031 (>1.3 in solar abundances). Comment: 17 pages, 12 figures; accepted for publication in MNRAS |
| نوع الوثيقة: | Working Paper |
| DOI: | 10.1093/mnras/stx683 |
| URL الوصول: | http://arxiv.org/abs/1701.07267 |
| رقم الأكسشن: | edsarx.1701.07267 |
| قاعدة البيانات: | arXiv |
| DOI: | 10.1093/mnras/stx683 |
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