SNR 0519-69.0
SNR 0519-69.0 in X-ray (blue) and visible light (red) | |
| Event type | Supernova |
|---|---|
| Ia[1] | |
| Date | c. 1355 (± 70 yrs)[1] |
| Constellation | Dorado |
| Right ascension | 05h 19m 34.29s[1] |
| Declination | −69° 02′ 5.86″[1] |
| Epoch | J2000 |
| Distance | 163,000 light-years (49.97 kpc)[2] |
| Host | Large Magellanic Cloud |
| Progenitor | Double degenerate progenitor (?)[3] |
| Progenitor type | Type Ia Supernova |
| Peak apparent magnitude | ? |
| Other designations | SNR B0519-69.0, 2E 1257, 1ES 0519-69.0, CAL 26, LMC RASS 183, RBS 638, [FHW95] LMC B0519-6905, [FPH98] LMC 21, [FS2003] 0259, [HP99] 789, [SHP2000] LMC 97, 1RXS J051934.7-690202, 2E 0519.9-6905, WHHW 0519.9-6905, [BMD2010] SNR J0519.6-6902, MCSNR J0519-6902 |
| Related media on Commons | |
SNR 0519-69.0 (or SNR 0519) is a supernova remnant (SNR) in the Large Magellanic Cloud. The supernova occurred around 163,000 light-years away in the constellation Dorado approximately 670 years ago.[1][2] The progenitor of this supernova was likely a star system composed of two white dwarfs.[3] Since then, the nebula has been heavily researched and photographed by astronomers.
Observations
SNR 0519 was first discovered in 1981 by astronomers Knox S. Long, David J. Helfand, and David A. Grabelsky during a soft X-ray study of the Large Magellanic Cloud.[4] The SNR nature was verified in 1982, and a Supernova origin type of Ia was additionally proposed.[5] In X-ray observations, SNR 0519 was discovered to be oxygen-poor and iron-rich, cementing it as a type Ia supernova.[6]
SNR 0519's progenitor is a topic of debate in astronomy, though many accept the theory of it being a star system composed of two white dwarves.[3] However, although many searches have occurred, astronomers have been unable to identify a surviving companion of SNR 0519 (Though a candidate was discovered in 2019).[7][8] A supersoft X-ray source has been entirely ruled out thanks to the absence of a relic ionization nebula.[9]
References
- ^ a b c d e "The Astrophysical Journal". Evidence for a Dense, Inhomogeneous Circumstellar Medium in the Type Ia SNR 0519-69.0. Retrieved 24 May 2025.
- ^ a b Pietrzyński, G.; Graczyk, D.; Gieren, W.; et al. (March 2013). "An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent". Nature. 495 (7439): 76–79. arXiv:1303.2063. Bibcode:2013Natur.495...76P. doi:10.1038/nature11878. ISSN 0028-0836. PMID 23467166. S2CID 4417699.
- ^ a b c "arXiv". The Progenitor of the Type Ia Supernova that created SNR 0519-69.0 in the Large Magellanic Cloud. Retrieved 24 May 2025.
- ^ Long, Knox S.; Helfand, David J.; Grabelsky, David A. "A soft X-ray study of the Large Magellanic Cloud".
- ^ Tuohy, I. R.; Dopita, M. A.; Mathewson, D. S.; Long, K. S.; Helfand, D. J. "Optical identification of Balmer-dominated supernova remnants in the Large Magellanic Cloud".
- ^ Hughes, J. P.; Hayashi, I.; Helfand, D.; Hwang, D.; Itoh, U.; Kirshner, R. "ASCA observations of the Large Magellanic Cloud supernova remnant sample: Typing supernovae from their remnants".
- ^ Edwards, Zachary I.; Pagnotta, Ashley; Schaefer, Bradley E. "The Progenitor of the Type Ia Supernova that Created SNR 0519-69.0 in the Large Magellanic Cloud".
- ^ Li, Chuan-Jui; Kerzendorf, Wolfgang E.; Chu, You-Hua; Chen, Ting-Wan; Do, Tuan; Gruendl, Robert A.; Holmes, Abigail; Ishioka, Ryoko; Leibundgut, Bruno; Pan, Kuo-Chuan; Ricker, Paul M.; Weisz, Daniel. "Search for Surviving Companions of Progenitors of Young LMC SN Ia Remnants".
- ^ Kuuttila, J.; Gilfanov, M.; Seitenzahl, I. R.; Woods, T. E.; Vogt, F. P. A. "Excluding supersoft X-ray sources as progenitors for four Type Ia supernovae in the Large Magellanic Cloud".