Abstrakti
We present photometric, spectroscopic, and polarimetric observations of the intermediate-luminosity Type IIP supernova (SN) 2021gmj from 1 to 386 d after the explosion. The peak absolute V-band magnitude of SN 2021gmj is −15.5 mag, which is fainter than that of normal Type IIP SNe. The spectral evolution of SN 2021gmj resembles that of other sub-luminous SNe: The optical spectra show narrow P-Cygni profiles, indicating a low expansion velocity. We estimate the progenitor mass to be about 12 M⊙ from the nebular spectrum and the 56Ni mass to be about 0.02 M⊙ from the bolometric light curve. We also derive the explosion energy to be about 3 × 1050 erg by comparing numerical light-curve models with the observed light curves. Polarization in the plateau phase is not very large, suggesting nearly spherical outer envelope. The early photometric observations capture the rapid rise of the light curve, which is likely due to the interaction with a circumstellar material (CSM). The broad emission feature formed by highly ionized lines on top of a blue continuum in the earliest spectrum gives further indication of the CSM at the vicinity of the progenitor. Our work suggests that a relatively low-mass progenitor of an intermediate-luminosity Type IIP SN can also experience an enhanced mass-loss just before the explosion, as suggested for normal Type IIP SNe.
| Alkuperäiskieli | Englanti |
|---|---|
| Sivut | 4209-4227 |
| Sivumäärä | 19 |
| Julkaisu | Monthly Notices of the Royal Astronomical Society |
| Vuosikerta | 528 |
| Numero | 3 |
| DOI - pysyväislinkit | |
| Tila | Julkaistu - 1 maalisk. 2024 |
| OKM-julkaisutyyppi | A1 Alkuperäisartikkeli tieteellisessä aikakauslehdessä |
Rahoitus
We extend our thanks to Anders Jerkstrand for providing theoretical models. The data from the Seimei and Kanata telescopes were taken under the KASTOR (Kanata And Seimei Transient Observation Regime) project (Seimei program IDs: 21A-N-CT02, 21A-K-0001, 21A-K-0002, 21A-O-0004, 21B-N-CT09, 21B-K-0004, 22A-N-CT09, 22A-K-004). The Seimei telescope at the Okayama Observatory is jointly operated by Kyoto University and the Astronomical Observatory of Japan (NAOJ), with assistance provided by the Optical and Near-Infrared Astronomy Inter-University Cooperation Program. The authors thank the TriCCS developer team (which has been supported by the JSPS KAKENHI grant Nos. JP18H05223, JP20H00174, and JP20H04736, and by NAOJ Joint Development Research). This work is partly based on observations made under program IDs P63-016 and P65-005 with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. We thank the staff of IAO, Hanle, and CREST, Hosakote that made HCT observations possible. The facilities at IAO and CREST are operated by the Indian Institute of Astrophysics, Bangalore. DKS acknowledges the support provided by DST-JSPS under grant number DST/INT/JSPS/P 363/2022. This research is partially supported by the Optical and Infrared Synergetic Telescopes for Education and Research program funded by the MEXT of Japan. The authors acknowledge the support by JSPS KAKENHI grant JP21H04997, JP23H00127, JP23H04894 (MT), JP20H00174 (KM), and by the JSPS Open Partnership Bilateral Joint Research Project between Japan and Finland JPJSBP120229923 (KM).
Sormenjälki
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Metsähovin radiotutkimusasema
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