The Astrophysical Journal (Jan 2023)
Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
- Kaustav K. Das,
- Mansi M. Kasliwal,
- Christoffer Fremling,
- Sheng Yang,
- Steve Schulze,
- Jesper Sollerman,
- Tawny Sit,
- Kishalay De,
- Anastasios Tzanidakis,
- Daniel A. Perley,
- Shreya Anand,
- Igor Andreoni,
- C. Barbarino,
- K. Brudge,
- Andrew Drake,
- Avishay Gal-Yam,
- Russ R. Laher,
- Viraj Karambelkar,
- S. R. Kulkarni,
- Frank J. Masci,
- Michael S. Medford,
- Abigail Polin,
- Harrison Reedy,
- Reed Riddle,
- Yashvi Sharma,
- Roger Smith,
- Lin Yan,
- Yi Yang,
- Yuhan Yao
Affiliations
- Kaustav K. Das
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Mansi M. Kasliwal
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Christoffer Fremling
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Sheng Yang
- ORCiD
- The Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-10691 Stockholm, Sweden
- Steve Schulze
- ORCiD
- The Oskar Klein Centre, Department of Physics, Stockholm University , AlbaNova, SE-10691 Stockholm, Sweden
- Jesper Sollerman
- ORCiD
- The Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-10691 Stockholm, Sweden
- Tawny Sit
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Kishalay De
- ORCiD
- MIT-Kavli Institute for Astrophysics and Space Research , 77 Massachusetts Avenue, Cambridge, MA 02139, USA
- Anastasios Tzanidakis
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Daniel A. Perley
- ORCiD
- Astrophysics Research Institute, Liverpool John Moores University , IC2, Liverpool Science Park, Liverpool L3 5RF, UK
- Shreya Anand
- ORCiD
- Division of Physics, Mathematics and Astronomy, California Institute of Technology , Pasadena, CA 91125, USA
- Igor Andreoni
- ORCiD
- Joint Space-Science Institute, University of Maryland , College Park, MD 20742, USA; Department of Astronomy, University of Maryland , College Park, MD 20742, USA; Astrophysics Science Division, NASA Goddard Space Flight Center , Mail Code 661, Greenbelt, MD 20771, USA
- C. Barbarino
- ORCiD
- The Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-10691 Stockholm, Sweden
- K. Brudge
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Andrew Drake
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Avishay Gal-Yam
- ORCiD
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science , 234 Herzl Street, 76100 Rehovot, Israel
- Russ R. Laher
- ORCiD
- IPAC, California Institute of Technology , 1200 E. California Boulevard, Pasadena, CA 91125, USA
- Viraj Karambelkar
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- S. R. Kulkarni
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Frank J. Masci
- ORCiD
- IPAC, California Institute of Technology , 1200 E. California Boulevard, Pasadena, CA 91125, USA
- Michael S. Medford
- ORCiD
- Department of Astronomy, University of California , Berkeley, CA 94720, USA; Lawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720, USA
- Abigail Polin
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Harrison Reedy
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Reed Riddle
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Yashvi Sharma
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Roger Smith
- ORCiD
- Caltech Optical Observatories, California Institute of Technology , Pasadena, CA 91125, USA
- Lin Yan
- ORCiD
- Caltech Optical Observatories, California Institute of Technology , Pasadena, CA 91125, USA
- Yi Yang
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- Yuhan Yao
- ORCiD
- Cahill Center for Astrophysics, California Institute of Technology , MC 249-17, 1200 E. California Boulevard, Pasadena, CA 91125, USA ; [email protected]
- DOI
- https://doi.org/10.3847/1538-4357/acfeeb
- Journal volume & issue
-
Vol. 959,
no. 1
p. 12
Abstract
The fate of stars in the zero-age main-sequence (ZAMS) range ≈8–12 M _⊙ is unclear. They could evolve to form white dwarfs or explode as electron-capture supernovae (SNe) or iron core-collapse SNe (CCSNe). Even though the initial mass function indicates that this mass range should account for over 40% of all CCSN progenitors, few have been observationally confirmed, likely due to the faintness and rapid evolution of some of these transients. In this paper, we present a sample of nine Ca-rich/O-poor Type IIb SNe detected by the Zwicky Transient Facility with progenitors likely in this mass range. These sources have a [Ca ii ] λ λ 7291, 7324/[O i ] λ λ 6300, 6364 flux ratio of ≳2 in their nebular spectra. Comparing the measured [O i ] luminosity (≲10 ^39 erg s ^−1 ) and derived oxygen mass (≈0.01 M _⊙ ) with theoretical models, we infer that the progenitor ZAMS mass for these explosions is less than 12 M _⊙ . The ejecta properties ( M _ej ≲ 1 M _⊙ and E _kin ∼ 10 ^50 erg) are also consistent. The low ejecta mass of these sources indicates a class of strongly-stripped SNe that is a transition between the regular stripped-envelope SNe and ultra-stripped SNe. The progenitor could be stripped by a main-sequence companion and result in the formation of a neutron star−main sequence binary. Such binaries have been suggested to be progenitors of neutron star−white dwarf systems that could merge within a Hubble time and be detectable with LISA.
Keywords
