Report
Helium-rich Superluminous Supernovae From the Zwicky Transient Facility
| العنوان: | Helium-rich Superluminous Supernovae From the Zwicky Transient Facility |
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| المؤلفون: | Yan, Lin, Perley, D., Schulze, S., Lunnan, R., Sollerman, J., De, K., Chen, Z., Fremling, C., Gal-Yam, A., Taggart, K., Chen, T. W., Andreoni, I., Bellm, E. C., Cunningham, V., Dekany, R., Duev, D., Fransson, C., Laher, R., Hankins, M., Ho, A., Jencson, J., Kaye, S., Kulkarni, S., Kasliwal, M., Golkhou, V., Graham, M., Masci, F., Miller, A., Neill, J., Ofek, E., Porter, M., Mróz, P., Reiley, D., Riddle, R., Rigault, M, Rusholme, B., Shupe, D., Soumagnac, M., Smith, R., Tartaglia, L., Yao, Y., Yaron, O. |
| سنة النشر: | 2020 |
| المجموعة: | Astrophysics |
| مصطلحات موضوعية: | Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena |
| الوصف: | Helium is expected to be present in the ejecta of some hydrogen-poor superluminous supernovae (SLSN-I). However, so far only one event, PTF10hgi has been identified with He features in its photospheric spectra (Quimby et al. 2018). We present the discovery of a new He-rich SLSN-I, ZTF19aawfbtg (SN2019hge) at $z=0.0866$. This event has more than 10 optical spectra at phases from $-41$ to $+103$\,days relative to the peak, most of which match well with that of PTF10hgi. Confirmation comes from a near-IR spectrum taken at $+34$ days, revealing He I features with P-Cygni profiles at 1.083 and 2.058$\mu$m. Using the optical spectra of PTF10hgi and SN2019hge as templates, we examine 70 SLSN-I discovered by ZTF in the first two years of operation and found additional five SLSN-I with distinct He-features. The excitation of He\,I atoms in normal core collapse supernovae requires non-thermal radiation, as proposed by previous studies. These He-rich events can not be explained by traditional $^{56}$Ni mixing model because of their blue spectra, high peak luminosity and slow rising time scales. Magnetar models offer a possible solution since pulsar winds naturally generate high energy particles as sources of non-thermal excitation. An alternative model is ejecta interaction with H-poor CSM which may be supported by the observed light curve undulations. These six SLSN-Ib appear to have relatively low-peak luminosities (rest-frame $M_g = -20.06\pm0.16$ mag). Comment: 12 pages, 6 figures, Accepted for publication in ApJL. Matched with the published version |
| نوع الوثيقة: | Working Paper |
| DOI: | 10.3847/2041-8213/abb8c5 |
| URL الوصول: | http://arxiv.org/abs/2006.13758 |
| رقم الانضمام: | edsarx.2006.13758 |
| قاعدة البيانات: | arXiv |
| DOI: | 10.3847/2041-8213/abb8c5 |
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