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| image = Pa 30 cropped (SII) cleaned up.jpg
| image = Pa 30 cropped (SII) cleaned up.jpg
| image_size = 300px
| image_size = 300px
| caption= Pa 30 is the presumed remnant.
| caption= Pa 30 is the supernova remnant of SN 1181. Here the nebula is seen as long thin filaments radiating out from the central star.
| epoch = J2000
| epoch = J2000
| type =
| type =
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First observed between August 4 and August 6, 1181, Chinese and Japanese astronomers recorded the [[supernova]] now known as '''SN 1181''' in eight separate texts.
First observed between August 4 and August 6, 1181, Chinese and Japanese astronomers recorded the [[supernova]] now known as '''SN 1181''' in eight separate texts.
One of only five supernovae in the [[Milky Way]] confidently identified in pre-telescopic records,<ref>{{cite book |first=F. Richard |last=Stephenson |first2=David |last2=Green |year=2002 |title=Historical Supernovae and their Remnants |isbn=0-19-850766-6 }}</ref> it appeared in the constellation [[Cassiopeia (constellation)|Cassiopeia]] and was visible and non-moving for 185 days. F. R. Stephenson first recognized that the 1181 AD `guest star' must be a supernova, because such a bright transient that lasts for 185 days and does not move in the sky can only be a galactic supernova<ref>{{cite journal
One of only five [[supernova]]e in the [[Milky Way]] confidently identified in pre-[[Telescope|telescopic]] records,<ref>{{cite book |first1=F. Richard |last1=Stephenson |first2=David |last2=Green |year=2002 |title=Historical Supernovae and their Remnants |publisher=Clarendon Press |isbn=0-19-850766-6 }}</ref> it appeared in the constellation [[Cassiopeia (constellation)|Cassiopeia]] and was visible and motionless against the fixed stars for 185 days. [[F. Richard Stephenson|F. R. Stephenson]] first recognized that the 1181 AD "[[Guest star (astronomy)|guest star]]" must be a [[supernova]], because such a bright transient that lasts for 185 days and does not move in the sky can only be a galactic supernova.<ref>{{cite journal
| title=A Suspected Supernova in A. D. 1181
| title=A Suspected Supernova in A. D. 1181
| last1=Stephenson | first1=F. Richard
| last1=Stephenson | first1=F. Richard
Line 29: Line 29:
| year=1971
| year=1971
| pages=10–38
| pages=10–38
| bibcode=1971QJRAS..12...10S }}</ref>.
| bibcode=1971QJRAS..12...10S }}</ref>


==Pa 30==
==Original Candidate Remnant: 3C 58==
[[File:IRAS 00500+6713.jpg|thumb|A comparison between an observed image (left panel; X-ray image (XMM) and IR contours (WISE)) and schematic picture of IRAS 00500+671<ref>{{cite journal |last1=Ko |first1=Takatoshi |last2=Suzuki |first2=Hiromasa |last3=Kashiyama |first3=Kazumi |last4=Uchida |first4=Hiroyuki |last5=Tanaka |first5=Takaaki |last6=Tsuna |first6=Daichi |last7=Fujisawa |first7=Kotaro |last8=Bamba |first8=Aya |last9=Shigeyama |first9=Toshikazu |title=A Dynamical Model for IRAS 00500+6713: The Remnant of a Type Iax Supernova SN 1181 Hosting a Double Degenerate Merger Product WD J005311 |journal=The Astrophysical Journal |date=1 July 2024 |volume=969 |issue=2 |pages=116 |doi=10.3847/1538-4357/ad4d99|doi-access=free |arxiv=2304.14669 |bibcode=2024ApJ...969..116K }}</ref>]]
The only plausible conventional supernova remnant in the historical area is the radio and X-ray [[pulsar]] J0205+6449 (also known as [[3C 58]]), which rotates about 15 times per second. If the supernova and pulsar are associated, the star is still rotating about as quickly as it did when it first formed.<ref>{{cite journal
Pa 30 was discovered in 2013 by [[Americans|American]] amateur astronomer [[Dana Patchick]] while searching for planetary nebula in [[Wide-field Infrared Survey Explorer|WISE]] infrared data.<ref>{{cite conference
|last1=Kronberger |first1=M. |display-authors=etal
|title=New Planetary Nebulae and Candidates from Multicolour Multiwavelength Surveys
| year=2014
| conference=Asymmetrical Planetary Nebulae VI conference
| url=http://www.astroscu.unam.mx/apn6/PROCEEDINGS/B3-Kronberger.pdf }}</ref>
It was the 30th nebula discovered by his searches, and as a result it is designated Pa 30. Pa 30 appeared as a nearly-round [[nebula]] roughly 171x156 arc-seconds in size, with an extremely blue central star. Pa 30 refers to both the nebula (originally catalogued as [[IRAS 00500+6713]]) and the central star (designated as WD J005311). The shell is bright in the [[infrared]], but very faint in the [[Optics|optical]], at first visible only by [[light]] in the [O III] band.

In 2019, [[Spectroscopy|optical spectroscopy]] of the central [[star]] revealed a very hot star with an intense [[stellar wind]] expanding at a very high velocity of 16,000&nbsp;km/s and a composition mainly of [[carbon]], [[oxygen]], and [[neon]] (with no [[hydrogen]] or [[helium]]).<ref name=":1">{{cite journal
| journal=[[Nature (journal)|Nature]]
|last1=Gvaramadze |first1=Vasilii V. |display-authors=etal
|title=A massive white-dwarf merger product before final collapse | volume=569
| year=2019
| issue=7758
| pages=684–687
| doi=10.1038/s41586-019-1216-1
|pmid=31110332 |arxiv=1904.00012 | bibcode=2019Natur.569..684G |s2cid=90260784 }}</ref> Such a speed could only arise from a [[supernova]] or an event of similar magnitude, more specifically from a [[Neutron star merger|merger]] of two [[white dwarf]]s. [[X-ray spectroscopy]] studies of the shell also revealed a very hot [[nebula]] containing carbon-burning ashes which can only be produced in a supernova.<ref>{{cite journal
| journal=[[Astronomy & Astrophysics]]
|last1=Oskinova |first1=Lidia M. |display-authors=etal
|title=X-rays observations of a super-Chandrasekhar object reveal an ONe and a CO white dwarf merger product embedded in a putative SN Iax remnant | volume=644
| year=2020
| pages=L8
| doi=10.1051/0004-6361/202039232
|arxiv=2008.10612 | bibcode=2020A&A...644L...8O |s2cid=221293111 }}</ref>
However, the remnant [[star]] of Pa 30 is a [[white dwarf]], not one of the conventional supernova remnants ([[neutron star]]s or [[black hole]]s). It has been suggested that Pa 30 is the remnant of a rare class of supernovae known as "[[Type Iax supernova|sub-luminous Type Iax Supernova]]" and that a merger of a CO white dwarf and an ONe white dwarf produced the remnant shell along with its supermassive [[white dwarf]] remnant. More recent observations in the [SII] band also revealed fine filamentary structures within the shell that had not previously been seen.<ref>{{Cite journal |last=Hall |first=Shannon |date=2023-01-26 |title=Weird supernova remnant blows scientists' minds |journal=Nature |volume=614 |issue=7947 |page=206 |language=en |doi=10.1038/d41586-023-00202-1 |pmid=36702966 |bibcode=2023Natur.614..206H |doi-access=free }}</ref><ref>{{Cite journal |last1=Fesen |first1=Robert A. |last2=Schaefer |first2=Bradley E. |last3=Patchick |first3=Dana |date=2023-01-11 |title=Discovery of an Exceptional Optical Nebulosity in the Suspected Galactic SN Iax Remnant Pa 30 Linked to the Historical Guest Star of 1181 CE |journal=The Astrophysical Journal Letters |volume=945 |issue=1 |pages=L4 |doi=10.3847/2041-8213/acbb67 | arxiv=2301.04809 |bibcode=2023ApJ...945L...4F |doi-access=free }}</ref>

A 2021 study measured the expansion velocity of ~1,100 km/s for the nebula from optical spectroscopy of the [S II] doublet. Together with the angular size of Pa 30 and the GAIA distance of 2.3 kpc, the age of the nebula could be estimated to be approximately 1,000 years. This made Pa 30 the new prime candidate for the remnant of the SN 1181 event.<ref>{{cite journal
| journal=[[The Astrophysical Journal Letters]]
|last1=Ritter |first1=Andreas |display-authors=etal
|title=The Remnant and Origin of the Historical Supernova 1181 AD | volume=918
| year=2021
|issue=2 | pages=L33
| doi=10.3847/2041-8213/ac2253
|arxiv=2105.12384 | bibcode=2021ApJ...918L..33R |doi-access=free }}</ref> Furthermore, the expansion velocity of the nebula and the inferred absolute brightness of the 1181 event are consistent with a Type Iax Supernova, making Pa 30 the only SN Iax remnant in our Galaxy and the only one which can be studied in detail.

With a temperature near 200,000 K,<ref name=":1" /> WD J005311 is among the hottest stars known.<ref>{{Cite web|url=https://arstechnica.com/science/2021/09/study-hottest-star-in-the-milky-way-is-likely-remnant-of-ancient-supernova/|title=Astronomers solve centuries-old mystery of supernova observed in 1181|date=17 September 2017|access-date=21 August 2024|first=Jennifer|last=Ouellette|website=arstechnica.com}}</ref> The extreme properties of the central star are being powered by the residual radioactive decay of [[Isotopes of nickel|<sup>56</sup>Ni]], where the usual half-life of 6.0 days from electron capture is increased to many centuries due to the nickel being completely ionized.<ref>{{cite journal
| author=Shen, Ken J.
| author2=Schwab, Josiah
| title=Wait for it: Post-supernova Winds Driven by Delayed Radioactive Decays
| journal=[[The Astrophysical Journal]]
| volume=834
| year=2017 | issue=2
| pages=180
| doi=10.3847/1538-4357/834/2/180
| doi-access=free
| arxiv=1610.06573
| bibcode=2017ApJ...834..180S }}</ref>

==3C 58==
{{Main articles|3C 58}}
Before 2013, the only plausible conventional [[supernova remnant]] in the old historical area for the supernova was the supernova remnant 3C 58. This remnant has a [[radio]] and [[X-ray]] [[pulsar]] that rotates about 15 times per second. So historically, SN 1181 had been associated with 3C 58 and its pulsar, although many researchers noted that this association is problematic. For example, if the [[supernova]] and pulsar are associated, then the star is still rotating about as quickly as it did when it first formed.<ref>{{cite journal
| title=The absolute magnitude and the type classification of SN 1181 equals 3 C 58
| title=The absolute magnitude and the type classification of SN 1181 equals 3 C 58
| last1=Panagia | first1=N.
| last1=Panagia | first1=N.
Line 41: Line 92:
| year=1980
| year=1980
| pages=389–391
| pages=389–391
| bibcode=1980A&A....82..389P }}</ref> This is in contrast to the [[Crab pulsar]], known to be the remnant of the [[SN 1054]] [[supernova]] in the year 1054, which has lost two-thirds of its rotational energy in essentially the same time span.<ref>{{cite journal
| bibcode=1980A&A....82..389P }}</ref> This is in contrast to the [[Crab pulsar]], known to be the remnant of the [[SN 1054]] [[supernova]] in the year 1054, which has lost two-thirds of its [[rotational energy]] in essentially the same span of time.<ref>{{cite journal
| author=Galas, C. M. F.
| author=Galas, C. M. F.
| author2=Tuohy, I. R.
| author2=Tuohy, I. R.
Line 52: Line 103:
| bibcode=1980ApJ...236L..13G }}</ref>
| bibcode=1980ApJ...236L..13G }}</ref>


The proper motion of the expanding shell of 3C 58 has been measured three times, always with an age of around 3500 years. Further, a collection of age measures from eight methods returns ages from 2400 to 7000 years.<ref>{{cite journal
The age of the 3C 58 remnant has been estimated by many measures.<ref>{{cite journal
| title=Optical Imaging and Spectroscopy of the Galactic Supernova Remnant 3C 58 (G130.7+3.1)
| title=Optical Imaging and Spectroscopy of the Galactic Supernova Remnant 3C 58 (G130.7+3.1)
| last1=Fesen | first1=Robert |last2=Rudie |first2=Gwen |last3=Hurford |first3=Alan |last4=Soto |first4=Aljeandro
| last1=Fesen | first1=Robert |last2=Rudie |first2=Gwen |last3=Hurford |first3=Alan |last4=Soto |first4=Aljeandro
| year=2008 | journal=[[The Astrophysical Journal Supplement Series]]
| year=2008 | journal=[[The Astrophysical Journal Supplement Series]]
| volume=174
| volume=174
| pages=379-395
| issue=2 | pages=379–395
| doi=10.1086/522781
| doi=10.1086/522781
| bibcode=2008ApJS..174..379F
| bibcode=2008ApJS..174..379F
| s2cid=120672848 | doi-access=free}}</ref>
<ref name="Kothes">{{cite journal
| author=Kothes, A.
| title=Distance and age of the pulsar wind nebula 3C 58
| journal=[[Astronomy and Astrophysics]]
| volume=560
| year=2013
| pages=A18
| doi=10.1051/0004-6361/201219839
| arxiv=1307.8384
| bibcode=2013A&A...560A..18K| s2cid=118595074
}}</ref>
}}</ref>
Most directly, the proper motion of the expanding shell of 3C 58 has been measured three times, resulting in a distance-independent estimated age of around 3500 years. The measures of the decline rate of the radio flux have substantial variability and uncertainty, so they are not useful for estimating the remnant's age. Age estimates involving the remnant's energy and the swept-up mass are both not useful due to large uncertainties with the distance as well as the presumed energetics and densities. The pulsar is offset from the center of 3C 58, implying an age of ~3700 years, although it is possible to be substantially younger if its transverse velocity happens to be high. The pulsar spin-down age is 5380 years. The neutron star cooling age is >5000 years. With these age estimates, 3C 58 is much too old a remnant to be associated with SN 1181.
So 3C 58 is not the remnant of SN 1181.


The possible sky position of the 1181 supernova has been revised to include additional information on the proximity of the "guest star" to adjacent Chinese constellations, resulting in a greatly smaller error region.<ref name=":0">{{Cite journal |last=Schaefer |first=Bradley E. |date=2023-08-01 |title=The path from the Chinese and Japanese observations of supernova 1181 AD, to a Type Iax supernova, to the merger of CO and ONe white dwarfs |journal=Monthly Notices of the Royal Astronomical Society |volume=523 |issue=3 |pages=3885–3904 |doi=10.1093/mnras/stad717 |doi-access=free |issn=0035-8711|arxiv=2301.04807 |bibcode=2023MNRAS.523.3885S }}</ref> This improved region does not contain 3C 58, because the guest star does not have proximity to two constellations as reported. So SN 1181 is not associated with 3C 58. Rather, this new small region contains Pa 30, which is independently known to be a ~800 year old supernova remnant.
==Supernova Remnant Pa 30==

In 2013, American amateur astronomer Dana Patchick discovered the shell and central star of Pa 30.
== Gallery ==
<ref>{{cite conference
<gallery widths="200" heights="200">
|last1=Kronberger |first1=M. |display-authors=etal
File:SN 1181 - Schaefer 2023 Figure 5.png|Constrains from ancient Chinese and Japanese observations of SN 1181 (cyan area) and the position of 3C 58 and Pa 30 according to Schaefer 2023<ref name=":0" />
|title=New Planetary Nebulae and Candidates from Multicolour Multiwavelength Surveys
File:IRAS 00500+6713 WISE.png|Pa 30 as shown with WISE
| year=2014
</gallery>
| conference=Asymmetrical Planetary Nebulae VI conference
| url=http://www.astroscu.unam.mx/apn6/PROCEEDINGS/B3-Kronberger.pdf }}</ref>
Patchick had been systematically searching the infrared all-sky survey of the WISE satellite for shells around stars. Patchick discovered 41 stars with shells, and the traditional designation is the discoverer's initials plus a running index number, so Patchick's new nebula in Cassiopeia is designated Pa 30. Pa 30 appeared as a nearly-round nebula roughly 171x156 arc-seconds in size, with an extremely blue central star. The shell is bright in the infrared, but very faint in the optical, at first only seen by the light of [O III]. Gvaramadze et al. (2019)<ref>{{cite journal
| journal=[[Nature]]
|last1=Gvaramadze |first1=Vasilii V. |display-authors=etal
|title=A massive white-dwarf merger product before final collapse | volume=569
| year=2019
| issue=7758
| pages=684-687
| doi=10.1038/s41586-019-1216-1
|arxiv=1904.00012 | bibcode=2019Natur.569..684G }}</ref>
used optical spectroscopy to see the central star as a very hot star with an intense stellar wind expanding at an incredible rate of 16,000 km/s and a composition mainly of carbon, oxygen, and neon (with no hydrogen or helium). They realized that this could only arise from a supernova, more specifically from a merger of two white dwarfs. Oskinova et al. (2020)<ref>{{cite journal
| journal=[[Astronomy & Astrophysics]]
|last1=Oskinova |first1=Lidia M. |display-authors=etal
|title=X-rays observations of a super-Chandrasekhar object reveal an ONe and a CO white dwarf merger product embedded in a putative SN Iax remnant | volume=644
| year=2020
| pages=L8
| doi=10.1051/0004-6361/202039232
|arxiv=2008.10612 | bibcode=2020A&A...644L...8O }}</ref>
used X-ray spectroscopy to reveal a very hot nebula composed mainly of carbon, oxygen, and neon, all with an age of order 8 centuries. The unique Pa 30 could only have been made by a supernova, but this supernova could not be any of the common classes, for example, with core-collapse and Type Ia supernovae producing neutron stars or black holes but not any white dwarfs with a fierce stellar wind. Oskinova et al. connected Pa 30 with the rare sub-class called `sub-luminous Type Iax Supernova' and pointed to a merger of a CO white dwarf and an ONe white dwarf. Ritter et al. (2021)<ref>{{cite journal
| journal=[[The Astrophysical Journal Letters]]
|last1=Ritter |first1=Andreas |display-authors=etal
|title=The Remnant and Origin of the Historical Supernova 1181 AD | volume=918
| year=2021
| pages=L33
| doi=10.3847/2041-8213/ac2253
|arxiv=2105.12384 | bibcode=2021ApJ...918L..33R }}</ref> made the connection from the supernova remnant Pa 30 back to the Supernova of 1181 AD. In October 2022, Professor Rob Fesen obtained deep narrowband imagery in the light of [SII] that recorded fine filaments not revealed until now.<ref>{{Cite journal |last=Hall |first=Shannon |date=2023-01-26 |title=Weird supernova remnant blows scientists' minds |journal=Nature |volume=614 |issue=7947 |page=206 |language=en |doi=10.1038/d41586-023-00202-1 |pmid=36702966 |bibcode=2023Natur.614..206H |doi-access=free }}</ref><ref>{{Cite journal |last1=Fesen |first1=Robert A. |last2=Schaefer |first2=Bradley E. |last3=Patchick |first3=Dana |date=2023-01-11 |title=Discovery of an Exceptional Optical Nebulosity in the Suspected Galactic SN Iax Remnant Pa 30 Linked to the Historical Guest Star of 1181 CE |journal=The Astrophysical Journal Letters |volume=945 |issue=1 |pages=L4 |doi=10.3847/2041-8213/acbb67 | arxiv=2301.04809 |bibcode=2023ApJ...945L...4F |doi-access=free }}</ref>


==See also==
==See also==
Line 108: Line 144:
{{Cassiopeia (constellation)|state=collapsed}}
{{Cassiopeia (constellation)|state=collapsed}}


{{DEFAULTSORT:Sn 1181}}
[[Category:Supernova remnants]]
[[Category:Supernova remnants]]
[[Category:Cassiopeia (constellation)]]
[[Category:Cassiopeia (constellation)]]

Revision as of 20:46, 3 September 2024

Supernova SN 1181
Pa 30 is the supernova remnant of SN 1181. Here the nebula is seen as long thin filaments radiating out from the central star.
F Edit this on Wikidata
Datebetween August 4 and August 6, 1181
ConstellationCassiopeia
Right ascension00h 53m 11.2s
Declination+67° 30′ 02.4″
EpochJ2000
RemnantPa 30
HostMilky Way
Notable featuresVisible at night for 185 days
Peak apparent magnitude0?
Preceded bySN 1054
Followed bySN 1572
[edit on Wikidata]

First observed between August 4 and August 6, 1181, Chinese and Japanese astronomers recorded the supernova now known as SN 1181 in eight separate texts. One of only five supernovae in the Milky Way confidently identified in pre-telescopic records,[1] it appeared in the constellation Cassiopeia and was visible and motionless against the fixed stars for 185 days. F. R. Stephenson first recognized that the 1181 AD "guest star" must be a supernova, because such a bright transient that lasts for 185 days and does not move in the sky can only be a galactic supernova.[2]

Pa 30

A comparison between an observed image (left panel; X-ray image (XMM) and IR contours (WISE)) and schematic picture of IRAS 00500+671[3]

Pa 30 was discovered in 2013 by American amateur astronomer Dana Patchick while searching for planetary nebula in WISE infrared data.[4] It was the 30th nebula discovered by his searches, and as a result it is designated Pa 30. Pa 30 appeared as a nearly-round nebula roughly 171x156 arc-seconds in size, with an extremely blue central star. Pa 30 refers to both the nebula (originally catalogued as IRAS 00500+6713) and the central star (designated as WD J005311). The shell is bright in the infrared, but very faint in the optical, at first visible only by light in the [O III] band.

In 2019, optical spectroscopy of the central star revealed a very hot star with an intense stellar wind expanding at a very high velocity of 16,000 km/s and a composition mainly of carbon, oxygen, and neon (with no hydrogen or helium).[5] Such a speed could only arise from a supernova or an event of similar magnitude, more specifically from a merger of two white dwarfs. X-ray spectroscopy studies of the shell also revealed a very hot nebula containing carbon-burning ashes which can only be produced in a supernova.[6] However, the remnant star of Pa 30 is a white dwarf, not one of the conventional supernova remnants (neutron stars or black holes). It has been suggested that Pa 30 is the remnant of a rare class of supernovae known as "sub-luminous Type Iax Supernova" and that a merger of a CO white dwarf and an ONe white dwarf produced the remnant shell along with its supermassive white dwarf remnant. More recent observations in the [SII] band also revealed fine filamentary structures within the shell that had not previously been seen.[7][8]

A 2021 study measured the expansion velocity of ~1,100 km/s for the nebula from optical spectroscopy of the [S II] doublet. Together with the angular size of Pa 30 and the GAIA distance of 2.3 kpc, the age of the nebula could be estimated to be approximately 1,000 years. This made Pa 30 the new prime candidate for the remnant of the SN 1181 event.[9] Furthermore, the expansion velocity of the nebula and the inferred absolute brightness of the 1181 event are consistent with a Type Iax Supernova, making Pa 30 the only SN Iax remnant in our Galaxy and the only one which can be studied in detail.

With a temperature near 200,000 K,[5] WD J005311 is among the hottest stars known.[10] The extreme properties of the central star are being powered by the residual radioactive decay of 56Ni, where the usual half-life of 6.0 days from electron capture is increased to many centuries due to the nickel being completely ionized.[11]

3C 58

Main article: 3C 58

Before 2013, the only plausible conventional supernova remnant in the old historical area for the supernova was the supernova remnant 3C 58. This remnant has a radio and X-ray pulsar that rotates about 15 times per second. So historically, SN 1181 had been associated with 3C 58 and its pulsar, although many researchers noted that this association is problematic. For example, if the supernova and pulsar are associated, then the star is still rotating about as quickly as it did when it first formed.[12] This is in contrast to the Crab pulsar, known to be the remnant of the SN 1054 supernova in the year 1054, which has lost two-thirds of its rotational energy in essentially the same span of time.[13]

The age of the 3C 58 remnant has been estimated by many measures.[14] [15] Most directly, the proper motion of the expanding shell of 3C 58 has been measured three times, resulting in a distance-independent estimated age of around 3500 years. The measures of the decline rate of the radio flux have substantial variability and uncertainty, so they are not useful for estimating the remnant's age. Age estimates involving the remnant's energy and the swept-up mass are both not useful due to large uncertainties with the distance as well as the presumed energetics and densities. The pulsar is offset from the center of 3C 58, implying an age of ~3700 years, although it is possible to be substantially younger if its transverse velocity happens to be high. The pulsar spin-down age is 5380 years. The neutron star cooling age is >5000 years. With these age estimates, 3C 58 is much too old a remnant to be associated with SN 1181.

The possible sky position of the 1181 supernova has been revised to include additional information on the proximity of the "guest star" to adjacent Chinese constellations, resulting in a greatly smaller error region.[16] This improved region does not contain 3C 58, because the guest star does not have proximity to two constellations as reported. So SN 1181 is not associated with 3C 58. Rather, this new small region contains Pa 30, which is independently known to be a ~800 year old supernova remnant.

  • Constrains from ancient Chinese and Japanese observations of SN 1181 (cyan area) and the position of 3C 58 and Pa 30 according to Schaefer 2023[16]
    Constrains from ancient Chinese and Japanese observations of SN 1181 (cyan area) and the position of 3C 58 and Pa 30 according to Schaefer 2023[16]
  • Pa 30 as shown with WISE
    Pa 30 as shown with WISE

See also

References

  1. ^ Stephenson, F. Richard; Green, David (2002). Historical Supernovae and their Remnants. Clarendon Press. ISBN 0-19-850766-6.
  2. ^ Stephenson, F. Richard (1971). "A Suspected Supernova in A. D. 1181". Quarterly Journal of the Royal Astronomical Society. 12: 10–38. Bibcode:1971QJRAS..12...10S.
  3. ^ Ko, Takatoshi; Suzuki, Hiromasa; Kashiyama, Kazumi; Uchida, Hiroyuki; Tanaka, Takaaki; Tsuna, Daichi; Fujisawa, Kotaro; Bamba, Aya; Shigeyama, Toshikazu (July 1, 2024). "A Dynamical Model for IRAS 00500+6713: The Remnant of a Type Iax Supernova SN 1181 Hosting a Double Degenerate Merger Product WD J005311". The Astrophysical Journal. 969 (2): 116. arXiv:2304.14669. Bibcode:2024ApJ...969..116K. doi:10.3847/1538-4357/ad4d99.
  4. ^ Kronberger, M.; et al. (2014). New Planetary Nebulae and Candidates from Multicolour Multiwavelength Surveys (PDF). Asymmetrical Planetary Nebulae VI conference.
  5. ^ a b Gvaramadze, Vasilii V.; et al. (2019). "A massive white-dwarf merger product before final collapse". Nature. 569 (7758): 684–687. arXiv:1904.00012. Bibcode:2019Natur.569..684G. doi:10.1038/s41586-019-1216-1. PMID 31110332. S2CID 90260784.
  6. ^ Oskinova, Lidia M.; et al. (2020). "X-rays observations of a super-Chandrasekhar object reveal an ONe and a CO white dwarf merger product embedded in a putative SN Iax remnant". Astronomy & Astrophysics. 644: L8. arXiv:2008.10612. Bibcode:2020A&A...644L...8O. doi:10.1051/0004-6361/202039232. S2CID 221293111.
  7. ^ Hall, Shannon (January 26, 2023). "Weird supernova remnant blows scientists' minds". Nature. 614 (7947): 206. Bibcode:2023Natur.614..206H. doi:10.1038/d41586-023-00202-1. PMID 36702966.
  8. ^ Fesen, Robert A.; Schaefer, Bradley E.; Patchick, Dana (January 11, 2023). "Discovery of an Exceptional Optical Nebulosity in the Suspected Galactic SN Iax Remnant Pa 30 Linked to the Historical Guest Star of 1181 CE". The Astrophysical Journal Letters. 945 (1): L4. arXiv:2301.04809. Bibcode:2023ApJ...945L...4F. doi:10.3847/2041-8213/acbb67.
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  12. ^ Panagia, N.; Weiler, K. W. (1980). "The absolute magnitude and the type classification of SN 1181 equals 3 C 58". Astronomy and Astrophysics. 82 (3): 389–391. Bibcode:1980A&A....82..389P.
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