The double-peaked SN 2013ge: A type Ib/c SN with an asymmetric mass ejection or an extended progenitor envelope
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
- Astrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701 (United States)
- Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States)
- Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210 (United States)
- NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States)
- Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States)
- Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C (Denmark)
- Itagaki Astronomical Observatory, Teppo-cho, Yamagata, Yamagata 990-2492 (Japan)
- Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101 (United States)
- Boise State University, Department of Physics, 1910 University Drive, Boise, ID 83725 (United States)
- Department of Astronomy, University of Texas at Austin, Austin, TX 78712 (United States)
We present extensive multiwavelength (radio to X-ray) observations of the Type Ib/c supernova (SN Ib/c) SN 2013ge from −13 to +457 days relative to maximum light, including a series of optical spectra and Swift UV–optical photometry beginning 2–4 days post-explosion. This data set makes SN 2013ge one of the best-observed normal SNe Ib/c at early times—when the light curve is particularly sensitive to the progenitor configuration and mixing of radioactive elements—and reveals two distinct light curve components in the UV bands. The first component rises over 4–5 days and is visible for the first week post-explosion. Spectra of the first component have blue continua and show a plethora of moderately high velocity (∼15,000 km s{sup −1}) but narrow (∼3500 km s{sup −1}) spectroscopic features, indicating that the line-forming region is restricted. The explosion parameters estimated for the bulk explosion (M{sub ej} ∼ 2–3 M{sub ⊙}; E{sub K} ∼ (1–2) × 10{sup 51} erg) are standard for SNe Ib/c, and there is evidence for weak He features at early times—in an object that would have otherwise been classified as Type Ic. In addition, SN 2013ge exploded in a low-metallicity environment (∼0.5 Z{sub ⊙}), and we have obtained some of the deepest radio and X-ray limits for an SN Ib/c to date, which constrain the progenitor mass-loss rate to be M-dot < 4 × 10{sup −6} M{sub ⊙} yr{sup −1}. We are left with two distinct progenitor scenarios for SN 2013ge, depending on our interpretation of the early emission. If the first component is cooling envelope emission, then the progenitor of SN 2013ge either possessed an extended (≳30 R{sub ⊙}) envelope or ejected a portion of its envelope in the final ≲1 yr before core collapse. Alternatively, if the first component is due to outwardly mixed {sup 56}Ni, then our observations are consistent with the asymmetric ejection of a distinct clump of nickel-rich material at high velocities. Current models for the collision of an SN shock with a binary companion cannot reproduce both the timescale and luminosity of the early emission in SN 2013ge. Finally, the spectra of the first component of SN 2013ge are similar to those of the rapidly declining SN 2002bj.
- OSTI ID:
- 22890067
- Journal Information:
- Astrophysical Journal, Vol. 821, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Since 2009, the country of publication for this journal is the UK.; ISSN 0004-637X
- Country of Publication:
- United Kingdom
- Language:
- English
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