The Astrophysical Journal (Jan 2024)
SN 2022oqm–A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material
- Ido Irani,
- Ping Chen,
- Jonathan Morag,
- Steve Schulze,
- Avishay Gal-Yam,
- Nora L. Strotjohann,
- Ofer Yaron,
- Erez A. Zimmerman,
- Amir Sharon,
- Daniel A. Perley,
- J. Sollerman,
- Aaron Tohuvavohu,
- Kaustav K. Das,
- Mansi M. Kasliwal,
- Rachel Bruch,
- Thomas G. Brink,
- WeiKang Zheng,
- Alexei V. Filippenko,
- Kishore C. Patra,
- Sergiy S. Vasylyev,
- Yi Yang,
- Matthew J. Graham,
- Joshua S. Bloom,
- Paolo Mazzali,
- Josiah Purdum,
- Russ R. Laher,
- Avery Wold,
- Yashvi Sharma,
- Leander Lacroix,
- Michael S. Medford
Affiliations
- Ido Irani
- ORCiD
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science , 234 Herzl Street, 7610001 Rehovot, Israel ; [email protected]
- Ping Chen
- ORCiD
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science , 234 Herzl Street, 7610001 Rehovot, Israel ; [email protected]
- Jonathan Morag
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science , 234 Herzl Street, 7610001 Rehovot, Israel ; [email protected]
- Steve Schulze
- ORCiD
- Department of Physics, The Oskar Klein Center, Stockholm University , AlbaNova, SE-10691 Stockholm, Sweden
- Avishay Gal-Yam
- ORCiD
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science , 234 Herzl Street, 7610001 Rehovot, Israel ; [email protected]
- Nora L. Strotjohann
- ORCiD
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science , 234 Herzl Street, 7610001 Rehovot, Israel ; [email protected]
- Ofer Yaron
- ORCiD
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science , 234 Herzl Street, 7610001 Rehovot, Israel ; [email protected]
- Erez A. Zimmerman
- ORCiD
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science , 234 Herzl Street, 7610001 Rehovot, Israel ; [email protected]
- Amir Sharon
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science , 234 Herzl Street, 7610001 Rehovot, Israel ; [email protected]
- Daniel A. Perley
- ORCiD
- Astrophysics Research Institute, Liverpool John Moores University , IC2 Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK
- J. Sollerman
- ORCiD
- Department of Astronomy, The Oskar Klein Center, Stockholm University , AlbaNova, SE-10691 Stockholm, Sweden
- Aaron Tohuvavohu
- ORCiD
- David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto , Toronto, ON, Canada
- Kaustav K. Das
- Division of Physics, Mathematics and Astronomy, California Institute of Technology , Pasadena, CA 91125, USA
- Mansi M. Kasliwal
- ORCiD
- Division of Physics, Mathematics and Astronomy, California Institute of Technology , Pasadena, CA 91125, USA
- Rachel Bruch
- ORCiD
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science , 234 Herzl Street, 7610001 Rehovot, Israel ; [email protected]
- Thomas G. Brink
- ORCiD
- Department of Astronomy, University of California , Berkeley, CA 94720-3411, USA
- WeiKang Zheng
- ORCiD
- Department of Astronomy, University of California , Berkeley, CA 94720-3411, USA
- Alexei V. Filippenko
- ORCiD
- Department of Astronomy, University of California , Berkeley, CA 94720-3411, USA
- Kishore C. Patra
- ORCiD
- Department of Astronomy, University of California , Berkeley, CA 94720-3411, USA
- Sergiy S. Vasylyev
- ORCiD
- Department of Astronomy, University of California , Berkeley, CA 94720-3411, USA
- Yi Yang
- ORCiD
- Department of Astronomy, University of California , Berkeley, CA 94720-3411, USA
- Matthew J. Graham
- ORCiD
- Division of Physics, Mathematics and Astronomy, California Institute of Technology , Pasadena, CA 91125, USA
- Joshua S. Bloom
- ORCiD
- Department of Astronomy, University of California , Berkeley, CA 94720-3411, USA; Lawrence Berkeley National Laboratory , 1 Cyclotron Road, MS 50B-4206, Berkeley, CA 94720, USA
- Paolo Mazzali
- ORCiD
- Astrophysics Research Institute, Liverpool John Moores University , IC2 Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK; Max-Planck Institute for Astrophysics , Garching, Germany
- Josiah Purdum
- ORCiD
- Division of Physics, Mathematics and Astronomy, California Institute of Technology , Pasadena, CA 91125, USA
- Russ R. Laher
- ORCiD
- IPAC , California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USA
- Avery Wold
- ORCiD
- IPAC , California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USA
- Yashvi Sharma
- ORCiD
- Division of Physics, Mathematics and Astronomy, California Institute of Technology , Pasadena, CA 91125, USA
- Leander Lacroix
- ORCiD
- LPNHE, Sorbonne-Université , Paris, France
- Michael S. Medford
- ORCiD
- Department of Astronomy, University of California , Berkeley, CA 94720-3411, USA; Lawrence Berkeley National Laboratory , 1 Cyclotron Road, MS 50B-4206, Berkeley, CA 94720, USA
- DOI
- https://doi.org/10.3847/1538-4357/ad04d7
- Journal volume & issue
-
Vol. 962,
no. 2
p. 109
Abstract
We present the discovery and analysis of SN 2022oqm, a Type Ic supernova (SN) detected <1 day after the explosion. The SN rises to a blue and short-lived (2 days) initial peak. Early-time spectral observations of SN 2022oqm show a hot (40,000 K) continuum with high ionization C and O absorption features at velocities of 4000 km s ^−1 , while its photospheric radius expands at 20,000 km s ^−1 , indicating a pre-existing distribution of expanding C/O material. After ∼2.5 days, both the spectrum and light curves evolve into those of a typical SN Ic, with line velocities of ∼10,000 km s ^−1 , in agreement with the evolution of the photospheric radius. The optical light curves reach a second peak at t ≈ 15 days. By t = 60 days, the spectrum of SN 2022oqm becomes nearly nebular, displaying strong Ca ii and [Ca ii ] emission with no detectable [O i ], marking this event as Ca-rich. The early behavior can be explained by 10 ^−3 M _⊙ of optically thin circumstellar material (CSM) surrounding either (1) a massive compact progenitor such as a Wolf–Rayet star, (2) a massive stripped progenitor with an extended envelope, or (3) a binary system with a white dwarf. We propose that the early-time light curve is powered by both the interaction of the ejecta with the optically thin CSM and shock cooling (in the massive star scenario). The observations can be explained by CSM that is optically thick to X-ray photons, is optically thick in the lines as seen in the spectra, and is optically thin to visible-light continuum photons that come either from downscattered X-rays or from the shock-heated ejecta. Calculations show that this scenario is self-consistent.
Keywords
