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Nakaoka, Tatsuya; Maeda, Keiichi; Yamanaka, Masayuki; Tanaka, Masaomi; Kawabata, Miho; Moriya, Takashi J.; Kawabata, Koji S.; Tominaga, Nozomu; Takagi, Kengo; Imazato, Fumiya; Morokuma, Tomoki; Sako, Shigeyuki; Ohsawa, Ryou; Nagao, Takashi; Jiang, Ji-an; Burgaz, Umut; Taguchi, Kenta; Uemura, Makoto; Akitaya, Hiroshi; Sasada, Mahito; Isogai, Keisuke; Otsuka, Masaaki; Maehara, Hiroyuki
Astrophysical journal/The Astrophysical journal, 05/2021, Letnik: 912, Številka: 1Journal Article
Abstract We present optical and near-infrared observations of SN 2019ehk, which was initially reported as a Type Ib supernova (SN). We show that it evolved to a Ca-rich transient according to its spectral properties and evolution in late phases. However, it shows a few properties distinct from those of the canonical Ca-rich transients: a short-duration first peak in the light curve, high peak luminosity, and association with a star-forming environment. Indeed, some of these features are shared with iPTF14gqr and iPTF16hgs, which are candidates for a special class of core-collapse SNe: the so-called ultra-stripped envelope SNe, i.e., a relatively low-mass He (or C+O) star explosion in a binary as a precursor of short-period double neutron star (NS) binaries. The estimated ejecta mass (0.4 M ⊙ ) and explosion energy (1.7 × 10 50 erg) are consistent with this scenario. The analysis of the first peak suggests the existence of dense circumstellar material in the vicinity of the progenitor, implying a CCSN origin. Based on this analysis, we suggest SN 2019ehk is another candidate for a low-mass He star explosion. It might create a double NS binary, but with a wide separation. These candidates for low-mass stripped envelope SNe, including ultra-stripped envelope SN candidates, seem to form a subpopulation among Ca-rich transients, associated with young population. We propose that the key to distinguishing this population is the early first peak in their light curves.
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