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Title: A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary

Journal Article · · Science
ORCiD logo [1]; ORCiD logo [1];  [2]; ORCiD logo [3];  [4];  [5]; ORCiD logo [6]; ORCiD logo [1]; ORCiD logo [1];  [7]; ORCiD logo [8];  [2]; ORCiD logo [9]; ORCiD logo [1];  [1]; ORCiD logo [8];  [2];  [1]; ORCiD logo [10]; ORCiD logo [11] more »; ORCiD logo [12]; ORCiD logo [13];  [14];  [15]; ORCiD logo [8]; ORCiD logo [16]; ORCiD logo [8] « less
  1. California Inst. of Technology (CalTech), Pasadena, CA (United States)
  2. The Weizmann Inst. of Science, Rehovot (Israel)
  3. National Institutes of Natural Sciences, Tokyo (Japan)
  4. Las Cumbres Observatory, Goleta, CA (United States); Univ. of California, Santa Barbara, CA (United States)
  5. Univ. of Washington, Seattle, WA (United States)
  6. NASA Goddard Space Flight Center (GSFC), Greenbelt, MD (United States); Univ. of Maryland, College Park, MD (United States)
  7. Univ. of Oxford, Oxford (United Kingdom)
  8. Stockholm Univ., Stockholm (Sweden)
  9. The Hebrew Univ. of Jerusalem, Jerusalem (Israel)
  10. Liverpool John Moores Univ., Liverpool (United Kingdom); Max-Planck-Institut für Astrophysik, Garching bei Munchen (Germany)
  11. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States); Univ. of California, Berkeley, CA (United States)
  12. Liverpool John Moores Univ., Liverpool (United Kingdom)
  13. Stockholm Univ., Stockholm (Sweden); Univ. of Nova Gorica, Ajdovščina (Slovenia)
  14. The Observatories of the Carnegie Institution for Science, Pasadena, CA (United States)
  15. Astrophysics Group, Cavendish Lab., Cambridge (United Kingdom)
  16. Univ. of Southampton, Southampton (United Kingdom)

Compact neutron star binary systems are produced from binary massive stars through stellar evolution involving up to two supernova explosions. The final stages in the formation of these systems have not been directly observed. Here, we report the discovery of iPTF 14gqr (SN 2014ft), a type Ic supernova with a fast-evolving light curve indicating an extremely low ejecta mass (≈0.2 solar masses) and low kinetic energy (≈2 × 1050ergs). Early photometry and spectroscopy reveal evidence of shock cooling of an extended helium-rich envelope, likely ejected in an intense pre-explosion mass-loss episode of the progenitor. Taken together, we interpret iPTF 14gqr as evidence for ultra-stripped supernovae that form neutron stars in compact binary systems.

Research Organization:
Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)
Sponsoring Organization:
USDOE Office of Science (SC)
Grant/Contract Number:
AC02-05CH11231
OSTI ID:
1526545
Journal Information:
Science, Vol. 362, Issue 6411; ISSN 0036-8075
Publisher:
AAASCopyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 74 works
Citation information provided by
Web of Science

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Formation of Double Neutron Star systems as implied by observations text January 2015
PTF12os and iPTF13bvn. Two stripped-envelope supernovae from low-mass progenitors in NGC 5806 text January 2016
The Swift X-ray Telescope text January 2005
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Presto-Color: A Photometric Survey Cadence for Explosive Physics & Fast Transients text January 2018
The Evolution of Massive Helium Stars Including Mass Loss text January 2019
SN 2017czd: A Rapidly Evolving Supernova from a Weak Explosion of a Type IIb Supernova Progenitor text January 2019
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