SNR 0519-69.0
{{Short description|Supernova remnant}}
{{Infobox supernova|name=SNR 0519-69.0|image=NASA-SNR0519690-ChandraXRayObservatory-20150122.jpg|caption=SNR 0519-69.0 in X-ray (blue) and visible light (red)|event_type=Supernova|type=Ia{{cite web
| title = The Astrophysical Journal
| work = Evidence for a Dense, Inhomogeneous Circumstellar Medium in the Type Ia SNR 0519-69.0
| url = https://iopscience.iop.org/article/10.3847/1538-4357/ac81ca
| access-date = 24 May 2025 }}|discovery={{circa}} 1355 (± 70 yrs){{cite web
| title = The Astrophysical Journal
| work = Evidence for a Dense, Inhomogeneous Circumstellar Medium in the Type Ia SNR 0519-69.0
| url = https://iopscience.iop.org/article/10.3847/1538-4357/ac81ca
| access-date = 24 May 2025 }}|ra={{RA|05|19|34.29}}{{cite web
| title = The Astrophysical Journal
| work = Evidence for a Dense, Inhomogeneous Circumstellar Medium in the Type Ia SNR 0519-69.0
| url = https://iopscience.iop.org/article/10.3847/1538-4357/ac81ca
| access-date = 24 May 2025 }}|dec={{DEC|−69|02|5.86}}{{cite web
| title = The Astrophysical Journal
| work = Evidence for a Dense, Inhomogeneous Circumstellar Medium in the Type Ia SNR 0519-69.0
| url = https://iopscience.iop.org/article/10.3847/1538-4357/ac81ca
| access-date = 24 May 2025 }}|epoch=J2000|distance={{convert|49.97|kpc|ly|-3|lk=on|order=flip}}{{Cite journal |last1=Pietrzyński |first1=G. |last2=Graczyk |first2=D. |last3=Gieren |first3=W. |display-authors=etal |date=March 2013 |title=An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent |journal=Nature |language=en |volume=495 |issue=7439 |pages=76–79 |arxiv=1303.2063 |bibcode=2013Natur.495...76P |doi=10.1038/nature11878 |issn=0028-0836 |pmid=23467166 |s2cid=4417699}}|constellation=Dorado|host=Large Magellanic Cloud|progenitor=Double degenerate progenitor (?){{cite web
| title = arXiv
| work = The Progenitor of the Type Ia Supernova that created SNR 0519-69.0 in the Large Magellanic Cloud
| url = https://arxiv.org/abs/1201.6377
| access-date = 24 May 2025 }}|progenitor_type=Type Ia Supernova|peak=?}}
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.{{cite web
| title = The Astrophysical Journal
| work = Evidence for a Dense, Inhomogeneous Circumstellar Medium in the Type Ia SNR 0519-69.0
| url = https://iopscience.iop.org/article/10.3847/1538-4357/ac81ca
| access-date = 24 May 2025 }}{{Cite journal |last1=Pietrzyński |first1=G. |last2=Graczyk |first2=D. |last3=Gieren |first3=W. |display-authors=etal |date=March 2013 |title=An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent |journal=Nature |language=en |volume=495 |issue=7439 |pages=76–79 |arxiv=1303.2063 |bibcode=2013Natur.495...76P |doi=10.1038/nature11878 |issn=0028-0836 |pmid=23467166 |s2cid=4417699}} The progenitor of this supernova was likely a star system composed of two white dwarfs.{{cite web
| title = arXiv
| work = The Progenitor of the Type Ia Supernova that created SNR 0519-69.0 in the Large Magellanic Cloud
| url = https://arxiv.org/abs/1201.6377
| access-date = 24 May 2025 }} 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.{{Cite web |last=Long |first=Knox S. |last2=Helfand |first2=David J. |last3=Grabelsky |first3=David A. |date= |title=A soft X-ray study of the Large Magellanic Cloud. |url=https://ui.adsabs.harvard.edu/abs/1981ApJ...248..925L/abstract}} The SNR nature was verified in 1982, and a Supernova origin type of Ia was additionally proposed.{{Cite web |last=Tuohy |first=I. R. |last2=Dopita |first2=M. A. |last3=Mathewson |first3=D. S. |last4=Long |first4=K. S. |last5=Helfand |first5=D. J. |title=Optical identification of Balmer-dominated supernova remnants in the Large Magellanic Cloud. |url=https://ui.adsabs.harvard.edu/abs/1982ApJ...261..473T/abstract}} In X-ray observations, SNR 0519 was discovered to be oxygen-poor and iron-rich, cementing it as a type Ia supernova.{{Cite web |last=Hughes |first=J. P. |last2=Hayashi |first2=I. |last3=Helfand |first3=D. |last4=Hwang |first4=D. |last5=Itoh |first5=U. |last6=Kirshner |first6=R. |title=ASCA observations of the Large Magellanic Cloud supernova remnant sample: Typing supernovae from their remnants |url=https://adsabs.harvard.edu/full/1995ApJ...444L..81H/L000084.000.html}}
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. 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).{{Cite web |last=Edwards |first=Zachary I. |last2=Pagnotta |first2=Ashley |last3=Schaefer |first3=Bradley E. |title=The Progenitor of the Type Ia Supernova that Created SNR 0519-69.0 in the Large Magellanic Cloud |url=https://ui.adsabs.harvard.edu/abs/2012ApJ...747L..19E/abstract}}{{Cite web |last=Li |first=Chuan-Jui |last2=Kerzendorf |first2=Wolfgang E. |last3=Chu |first3=You-Hua |last4=Chen |first4=Ting-Wan |last5=Do |first5=Tuan |last6=Gruendl |first6=Robert A. |last7=Holmes |first7=Abigail |last8=Ishioka |first8=Ryoko |last9=Leibundgut |first9=Bruno |last10=Pan |first10=Kuo-Chuan |last11=Ricker |first11=Paul M. |last12=Weisz |first12=Daniel |title=Search for Surviving Companions of Progenitors of Young LMC SN Ia Remnants |url=https://ui.adsabs.harvard.edu/abs/2019ApJ...886...99L/abstract}} A supersoft X-ray source has been entirely ruled out thanks to the absence of a relic ionization nebula.{{Cite web |last=Kuuttila |first=J. |last2=Gilfanov |first2=M. |last3=Seitenzahl |first3=I. R. |last4=Woods |first4=T. E. |last5=Vogt |first5=F. P. A. |title=Excluding supersoft X-ray sources as progenitors for four Type Ia supernovae in the Large Magellanic Cloud |url=https://ui.adsabs.harvard.edu/abs/2019MNRAS.484.1317K/abstract}}
References
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