SNR 0519−69.0
| Supernova remnant | |
|---|---|
SNR 0519−69.0 in X-ray (blue) and visible light (red) | |
| Observation data: J2000 epoch | |
| Class | Supernova remnant |
| Right ascension | 05h 19m 35.14s[1] |
| Declination | −69h 02m 00.5s[1] |
| Distance | 163,000 ly (49,970[2] pc) |
| Constellation | Dorado[3] |
| Physical characteristics | |
| Radius | ~4[4] pc |
| Notable features | Ring-like morphology |
| Designations | SNR B0519−69.0, LHG 26, MC SNR J0519−6902[1][4] |
SNR 0519−69.0 (abbreviated SNR 0519; also known as LHG 26 or MC SNR J0519−6902) 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.[5][2] The progenitor of this supernova was likely a star system composed of two white dwarfs,[6] with a mass of 1.2 to 4.0 solar masses.[4] While its initial explosion has ended, it may possess some wind bubble activity.[7][4] Since then, the nebula has been heavily researched and photographed by astronomers.
It has a diameter of 8 parsecs and exhibits a ring like morphology in radio waves. There are three bright spot regions located to the north, east and south of the supernova remnant. There is a HI cloud that may be associated with the remnant located in the southeastern part.[4]
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.[8] The SNR nature was verified in 1982, and a supernova type of Ia was additionally proposed.[9] In X-ray observations, SNR 0519 was discovered to be oxygen-poor and iron-rich, cementing it as a type Ia supernova.[10]
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 dwarfs.[6] 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).[6][11] A supersoft X-ray source has been entirely ruled out thanks to the absence of a relic ionization nebula.[12]
References
- ^ a b c "SNR B0519-69.0". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ 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.
- ^ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- ^ a b c d e Alsaberi, Rami Z. E.; Filipovic, Miroslav D.; Sano, Hidetoshi; Dai, Shi; Haberl, Frank; Kavanagh, Patrick J.; Leahy, Denis; Maggi, Pierre; Rowell, Gavin; Sasaki, Manami; Seitenzahl, Ivo R.; Urosevic, Dejan; Payne, Jeffrey; Smeaton, Zachary J.; Lazarevic, Sanja (2025). "A New Radio Continuum Study of the Large Magellanic Cloud Supernova Remnant MC SNR J0519-6902". Publications of the Astronomical Society of Australia. 42 e069. arXiv:2504.11746. Bibcode:2025PASA...42...69A. doi:10.1017/pasa.2025.10025.
- ^ "The Astrophysical Journal". Evidence for a Dense, Inhomogeneous Circumstellar Medium in the Type Ia SNR 0519-69.0. Retrieved 24 May 2025.
- ^ a b c Edwards, Zachary I.; Pagnotta, Ashley; Schaefer, Bradley E. (March 2012). "The Progenitor of the Type Ia Supernova that Created SNR 0519-69.0 in the Large Magellanic Cloud". The Astrophysical Journal Letters. 747 (2): L19. arXiv:1201.6377. Bibcode:2012ApJ...747L..19E. doi:10.1088/2041-8205/747/2/L19.
- ^ "Properties of supernova remnant in nearby galaxy explored in radio continuum study". phys.org. Retrieved 2025-05-29.
- ^ 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".
- ^ 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".