{{Short description|Supernova remnant}} {{Infobox supernova|name=G306.3-0.9|image=G306.3-0.9.jpg|constellation=[[Centaurus]]|epoch=J2000|event_type=[[Supernova remnant]]|type=Ia|ra=13h 21m 51s|dec=-63°34′|gal=G306.3-00.9|distance=20,000 parsecs}}
'''SNR G306.3-00.9''', also called '''G306.3-0.9'''<ref>{{Cite web |title=SNR G306.3-00.9 |url=https://simbad.u-strasbg.fr/simbad/sim-id |access-date=2024-04-24 |website=simbad.u-strasbg.fr}}</ref> is a [[supernova remnant]] located in the constellation [[Centaurus]]. It was discovered by the [[Neil Gehrels Swift Observatory|Swift Space Observatory]] in 2011.<ref>{{Cite journal |last1=Miller |first1=J. M. |last2=Reynolds |first2=M. R. |last3=Maitra |first3=D. |last4=Gultekin |first4=K. |last5=Gehrels |first5=N. |last6=Kennea |first6=J. |last7=Siegel |first7=M. |last8=Gelbord |first8=J. |last9=Kuin |first9=P. |date=2011-06-01 |title=Discovery of a New Supernova Remnant in the Swift Galactic Plane Survey |url=https://ui.adsabs.harvard.edu/abs/2011ATel.3415....1M |journal=The Astronomer's Telegram |volume=3415 |pages=1|bibcode=2011ATel.3415....1M }}</ref>
== Morphology == The first observations carried out with the [[Chandra X-ray Observatory]] revealed that SNR G306.3-00.9 has a distorted morphology, brighter towards the southwest. The strong radio and [[X-ray emission spectroscopy|X-ray emission]] from this area suggests either that there is interaction with an interstellar cloud or that it is the consequence of an asymmetric supernova explosion.<ref name=":0">{{Cite journal |last1=Chawner |first1=H. |last2=Gomez |first2=H. L. |last3=Matsuura |first3=M. |last4=Smith |first4=M. W. L. |last5=Papageorgiou |first5=A. |last6=Rho |first6=J. |last7=Noriega-Crespo |first7=A. |last8=De Looze |first8=I. |last9=Barlow |first9=M. J. |last10=Cigan |first10=P. |last11=Dunne |first11=L. |last12=Marsh |first12=K. |date=2020-04-01 |title=A complete catalogue of dusty supernova remnants in the Galactic plane |journal=Monthly Notices of the Royal Astronomical Society |volume=493 |issue=2 |pages=2706–2744 |doi=10.1093/mnras/staa221 |doi-access=free |arxiv=2001.05504 |bibcode=2020MNRAS.493.2706C |issn=0035-8711}}</ref> Emission from highly [[Atom|ionized atoms]] of [[magnesium]], [[silicon]], [[sulfur]] and [[argon]], and suggests that it is the remnant of a [[Type Ia supernova]].<ref name=":1">{{Cite journal |last1=Reynolds |first1=Mark T. |last2=Loi |first2=Shyeh T. |last3=Murphy |first3=Tara |last4=Miller |first4=Jon M. |last5=Maitra |first5=Dipankar |last6=Gültekin |first6=Kayhan |last7=Gehrels |first7=Neil |last8=Kennea |first8=Jamie A. |last9=Siegel |first9=Michael H. |last10=Gelbord |first10=Jonathan |last11=Kuin |first11=Paul |last12=Moss |first12=Vanessa |last13=Reeves |first13=Sarah |last14=Robbins |first14=William J. |last15=Gaensler |first15=B. M. |date=2013-04-01 |title=G306.3-0.9: A Newly Discovered Young Galactic Supernova Remnant |url=https://ui.adsabs.harvard.edu/abs/2013ApJ...766..112R |journal=The Astrophysical Journal |volume=766 |issue=2 |pages=112 |doi=10.1088/0004-637X/766/2/112 |arxiv=1303.3546 |bibcode=2013ApJ...766..112R |issn=0004-637X}}</ref> Such a spectrum can be described by a non-equilibrium ionization plasma with a temperature below 1 keV.<ref name=":2">{{Cite journal |last1=Sawada |first1=Makoto |last2=Tachibana |first2=Katsuhiro |last3=Uchida |first3=Hiroyuki |last4=Ito |first4=Yuta |last5=Matsumura |first5=Hideaki |last6=Bamba |first6=Aya |last7=Tsuru |first7=Takeshi Go |last8=Tanaka |first8=Takaaki |date=2019-06-01 |title=Ionization age of iron ejecta in the Galactic Type Ia supernova remnant G306.3-0.9 |url=https://ui.adsabs.harvard.edu/abs/2019PASJ...71...61S |journal=Publications of the Astronomical Society of Japan |volume=71 |issue=3 |pages=61 |doi=10.1093/pasj/psz036 |arxiv=1903.02554 |bibcode=2019PASJ...71...61S |issn=0004-6264}}</ref> In infrared images at 24 μm, the morphology of the dust grains impacted by the shock wave is shell-shaped, coinciding with the distribution observed in hard X-rays. At 70 μm the dust emission is concentrated in the south, with very little dust in the northwest.<ref name=":0" />
== Distance == The age of SNR G306.3-00.9 is not well known. It was initially estimated that it could be approximately 2,500 years old—a very young supernova remnant—considering that it was 8,000 parsecs away.<ref name=":1" /> A later study, which compares the X-ray absorption column with the distribution of H I decomposed along the line of sight, gives it a distance of around 20,000 parsecs, so its age may be 6000 years and evolutionarily it would be in the late Sedov phase. According to this, the most probable location of SNR G306.3-00.9 is in the outer extension of the Perseus arm.<ref name=":2" /> However, according to other models, its age could be considerably older, 12,800 (+2500, − 2500) years.<ref>{{Cite journal |last1=Leahy |first1=D. A. |last2=Ranasinghe |first2=S. |last3=Gelowitz |first3=M. |date=2020-05-01 |title=Evolutionary Models for 43 Galactic Supernova Remnants with Distances and X-Ray Spectra |journal=The Astrophysical Journal Supplement Series |volume=248 |issue=1 |pages=16 |doi=10.3847/1538-4365/ab8bd9 |doi-access=free |arxiv=2003.08998 |bibcode=2020ApJS..248...16L |issn=0067-0049}}</ref>
== See also ==
* [[List of supernova remnants]] * [[2011 in science]]
== References == {{reflist}}
[[Category:Supernova remnants]] [[Category:Centaurus]]