تقرير
A puzzle solved after two decades: SN 2002gh among the brightest of superluminous supernovae
| العنوان: | A puzzle solved after two decades: SN 2002gh among the brightest of superluminous supernovae |
|---|---|
| المؤلفون: | Cartier, Régis, Hamuy, Mario, Contreras, Carlos, Anderson, Joseph P., Phillips, Mark M., Morrell, Nidia, Stritzinger, Maximilian D., Hueichapan, Emilio D., Clocchiatti, Alejandro, Roth, Miguel, Thomas-Osip, Joanna, González, Luis E. |
| سنة النشر: | 2021 |
| المجموعة: | Astrophysics |
| مصطلحات موضوعية: | Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Solar and Stellar Astrophysics |
| الوصف: | We present optical photometry and spectroscopy of the superluminous SN 2002gh from maximum light to $+204$ days, obtained as part of the Carnegie Type II Supernova (CATS) project. SN 2002gh is among the most luminous discovered supernovae ever, yet it remained unnoticed for nearly two decades. Using Dark Energy Camera archival images we identify the potential SN host galaxy as a faint dwarf galaxy, presumably having low metallicity, and in an apparent merging process with other nearby dwarf galaxies. We show that SN 2002gh is among the brightest hydrogen-poor SLSNe with $M_{V} = -22.40 \pm 0.02$, with an estimated peak bolometric luminosity of $2.6 \pm 0.1 \times 10^{44}$ erg s$^{-1}$. We discount the decay of radioactive nickel as the main SN power mechanism, and assuming that the SN is powered by the spin down of a magnetar we obtain two alternative solutions. The first case, is characterized by significant magnetar power leakage, and $M_{\mathrm{ej}}$ between 0.6 and 3.2 $M_{\odot}$, $P_{\mathrm{spin}} = 3.2$ ms, and $B = 5 \times 10^{13}$ G. The second case does not require power leakage, resulting in a huge ejecta mass of about 30 $M_{\odot}$, a fast spin period of $P_{\mathrm{spin}} \sim 1$ ms, and $B\sim 1.6 \times 10^{14}$ G. We estimate a zero-age main-sequence mass between 14 and 25 $M_{\odot}$ for the first case and of about 135 $M_{\odot}$ for the second case. The latter case would place the SN progenitor among the most massive stars observed to explode as a SN. Comment: 25 pages, 18 figures, accepted for publication in MNRAS |
| نوع الوثيقة: | Working Paper |
| DOI: | 10.1093/mnras/stac1371 |
| الوصول الحر: | http://arxiv.org/abs/2108.09828Test |
| رقم الانضمام: | edsarx.2108.09828 |
| قاعدة البيانات: | arXiv |
| DOI: | 10.1093/mnras/stac1371 |
|---|