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| volume = 284 | volume = 284
| pages = 573 | pages = 573
| date = 1994 }}</ref><br /> | date = 1994 | last2 = Aschenbach
}}</ref><br />
Notably, IC 443 X-ray morphology is centrally peaked and a very soft X-ray shell is barely visible.<ref name="xmm">{{ Notably, IC 443 X-ray morphology is centrally peaked and a very soft X-ray shell is barely visible.<ref name="xmm">{{
cite journal cite journal
| bibcode = 2006ApJ...649..258T | bibcode = 2006ApJ...649..258T
| author = Troja, E., ''et al.'' | authors = Troja, E.
| title = XMM-Newton Observations of the SNR IC 443. I. Soft X-Ray Emission from Shocked Interstellar Medium | title = XMM-Newton Observations of the SNR IC 443. I. Soft X-Ray Emission from Shocked Interstellar Medium
| journal = Astrophysical Journal | journal = Astrophysical Journal
Line 46: Line 47:
| pages = 258 | pages = 258
| date = 2006 | date = 2006
| doi = 10.1086/506378|arxiv = astro-ph/0606313 }}</ref> | doi = 10.1086/506378|arxiv = astro-ph/0606313 | author = Troja, E.
| author2 = and others
| displayauthors = 1
| last3 = Reale
| first3 = F.
}}</ref>
Unlike plerion remnants, e.g. the ], the inner X-ray emission is not dominated by the central ]. Unlike plerion remnants, e.g. the ], the inner X-ray emission is not dominated by the central ].
It has indeed a thermal origin.<ref name="einstein">{{ It has indeed a thermal origin.<ref name="einstein">{{
cite journal cite journal
| bibcode = 1988ApJ...335..215P | bibcode = 1988ApJ...335..215P
| author = Petre, R., ''et al.'' | authors = Petre, R.
| title = A comprehensive study of the X-ray structure and spectrum of IC 443 | title = A comprehensive study of the X-ray structure and spectrum of IC 443
| journal = Astrophysical Journal | journal = Astrophysical Journal
Line 57: Line 63:
| pages = 215 | pages = 215
| date = 1988 | date = 1988
| doi = 10.1086/166922}}</ref> IC 443 shows very similar features to the class of '''mixed morphology'''<ref>{{ | doi = 10.1086/166922| author = Petre, R.
| author2 = and others
| displayauthors = 1
| last3 = Seward
| first3 = F. D.
| last4 = Willingale
| first4 = R.
}}</ref> IC 443 shows very similar features to the class of '''mixed morphology'''<ref>{{
cite journal cite journal
| bibcode = 1998ApJ...503L.167R | bibcode = 1998ApJ...503L.167R
Line 67: Line 80:
| pages = L167 | pages = L167
| date = 1998 | date = 1998
| doi = 10.1086/311538}}</ref> SNRs. Both optical and X-ray emission are heavily absorbed by a giant molecular cloud in the foreground, crossing the whole remnant body from northwest to southeast. | doi = 10.1086/311538| last2 = Petre
}}</ref> SNRs. Both optical and X-ray emission are heavily absorbed by a giant molecular cloud in the foreground, crossing the whole remnant body from northwest to southeast.


The remnant's age is still uncertain. There is some agreement that the progenitor supernova happened between 3,000<ref name="einstein"/> and 30,000<ref name="chevalier">{{ The remnant's age is still uncertain. There is some agreement that the progenitor supernova happened between 3,000<ref name="einstein"/> and 30,000<ref name="chevalier">{{
Line 82: Line 96:
cite journal cite journal
| bibcode = 2001ApJ...554L.205O | bibcode = 2001ApJ...554L.205O
| author = Olbert, C. M., ''et al.'' | author = Olbert, C. M.
| title = A Bow Shock Nebula around a Compact X-Ray Source in the Supernova Remnant IC 443 | title = A Bow Shock Nebula around a Compact X-Ray Source in the Supernova Remnant IC 443
| journal = Astrophysical Journal Letters | journal = Astrophysical Journal Letters
Line 89: Line 103:
| pages = L205 | pages = L205
| date = 2001 | date = 2001
| doi = 10.1086/321708|arxiv = astro-ph/0103268 }}</ref> and ]<ref>{{ | doi = 10.1086/321708|arxiv = astro-ph/0103268 | author2 = and others
| displayauthors = 1
| last3 = Williams
| last4 = Keohane
| last5 = Frail
}}</ref> and ]<ref>{{
cite journal cite journal
| bibcode = 2001A&A...376..248B | bibcode = 2001A&A...376..248B
Line 99: Line 118:
| pages = 248 | pages = 248
| date = 2001 | date = 2001
| doi = 10.1051/0004-6361:20010882|arxiv = astro-ph/0106417 }}</ref> observations | doi = 10.1051/0004-6361:20010882|arxiv = astro-ph/0106417 | last2 = Bykov
}}</ref> observations
identified a ], close to the remnant southern rim. The point source near the apex of the nebula is a ], relic of a SN explosion. The location in a star forming region and the presence of a ] favor a ], the ultimate fate of a massive star, as the progenitor explosion. identified a ], close to the remnant southern rim. The point source near the apex of the nebula is a ], relic of a SN explosion. The location in a star forming region and the presence of a ] favor a ], the ultimate fate of a massive star, as the progenitor explosion.


Line 124: Line 144:
cite journal cite journal
| bibcode = 1977A&A....54..889C | bibcode = 1977A&A....54..889C
| author = Cornett, R. H. ''et al.'' | author = Cornett, R. H.
| title = Observations of CO emission from a dense cloud associated with the supernova remnant IC 443 | title = Observations of CO emission from a dense cloud associated with the supernova remnant IC 443
| journal = Astronomy & Astrophysics | journal = Astronomy & Astrophysics
| volume = 54 | volume = 54
| pages = 889 | pages = 889
| date = 1977}}</ref> | date = 1977| author2 = and others
| displayauthors = 1
| last3 = Knapp
}}</ref>
and it is likely due to a giant molecular cloud, located between the remnant and the observer. and it is likely due to a giant molecular cloud, located between the remnant and the observer.
This is the main source of extinction of the low energy SNR emission. This is the main source of extinction of the low energy SNR emission.
Line 136: Line 159:
cite journal cite journal
| bibcode = 2001ApJ...547..885R | bibcode = 2001ApJ...547..885R
| author = Rho, J., ''et al.'' | authors = Rho, J.
| title = Near-Infrared Imaging and OI Spectroscopy of IC 443 using Two Micron All Sky Survey and Infrared Space Observatory | title = Near-Infrared Imaging and OI Spectroscopy of IC 443 using Two Micron All Sky Survey and Infrared Space Observatory
| journal = Astrophysical Journal | journal = Astrophysical Journal
Line 143: Line 166:
| pages = 885 | pages = 885
| date = 2001 | date = 2001
| doi = 10.1086/318398}}</ref> | doi = 10.1086/318398| author = Rho, J.
| author2 = and others
| displayauthors = 1
| last3 = Cutri
| first3 = R. M.
| last4 = Reach
| first4 = W. T.
}}</ref>
OH (1720&nbsp;MHz) ] emission, which is a robust tracer of interaction between SNRs and dense molecular clouds, has been detected in this region.<ref>{{ OH (1720&nbsp;MHz) ] emission, which is a robust tracer of interaction between SNRs and dense molecular clouds, has been detected in this region.<ref>{{
cite journal cite journal
| bibcode = 2006ApJ...652.1288H | bibcode = 2006ApJ...652.1288H
| author = Hewitt, J. W., ''et al.'' | author = Hewitt, J. W.
| title = Green Bank Telescope Observations of IC 443: The Nature of OH (1720 MHz) Masers and OH Absorption | title = Green Bank Telescope Observations of IC 443: The Nature of OH (1720 MHz) Masers and OH Absorption
| journal = Astrophysical Journal | journal = Astrophysical Journal
Line 154: Line 184:
| pages = 1288 | pages = 1288
| date = 2006 | date = 2006
| doi = 10.1086/508331|arxiv = astro-ph/0602210 }}</ref> | doi = 10.1086/508331|arxiv = astro-ph/0602210 | author2 = and others
| displayauthors = 1
| last3 = Wardle
| last4 = Roberts
| last5 = Kassim
}}</ref>
Interestingly, a source of gamma-ray radiation<ref>{{ Interestingly, a source of gamma-ray radiation<ref>{{
cite journal cite journal
| bibcode = 2007ApJ...664L..87A | bibcode = 2007ApJ...664L..87A
| author = Albert, J., ''et al.'' | authors = Albert, J.
| title = Discovery of Very High Energy Gamma Radiation from IC 443 with the MAGIC Telescope | title = Discovery of Very High Energy Gamma Radiation from IC 443 with the MAGIC Telescope
| journal = Astrophysical Journal Letters | journal = Astrophysical Journal Letters
Line 165: Line 200:
| pages = L87 | pages = L87
| date = 2007 | date = 2007
| doi = 10.1086/520957|arxiv = 0705.3119 }}</ref> is spatially coincident with IC 443 and the ] emission region, though is not well understood whether it is physically associated with the remnant or not. | doi = 10.1086/520957|arxiv = 0705.3119 | author = Albert, J.
| author2 = and others
| displayauthors = 1
| last3 = Anderhub
| first3 = H.
| last4 = Antoranz
| first4 = P.
| last5 = Armada
| first5 = A.
| last6 = Baixeras
| first6 = C.
| last7 = Barrio
| first7 = J. A.
| last8 = Bartko
| first8 = H.
| last9 = Bastieri
| first9 = D.
| last10 = Becker
| first10 = J. K.
| last11 = Bednarek
| first11 = W.
| last12 = Berger
| first12 = K.
| last13 = Bigongiari
| first13 = C.
| last14 = Biland
| first14 = A.
| last15 = Bock
| first15 = R. K.
| last16 = Bordas
| first16 = P.
| last17 = Bosch-Ramon
| first17 = V.
| last18 = Bretz
| first18 = T.
| last19 = Britvitch
| first19 = I.
| last20 = Camara
| first20 = M.
| last21 = Carmona
| first21 = E.
| last22 = Chilingarian
| first22 = A.
| last23 = Coarasa
| first23 = J. A.
| last24 = Commichau
| first24 = S.
| last25 = Contreras
| first25 = J. L.
| last26 = Cortina
| first26 = J.
| last27 = Costado
| first27 = M. T.
| last28 = Curtef
| first28 = V.
| last29 = Danielyan
| first29 = V.
| last30 = Dazzi
| first30 = F.
}}</ref> is spatially coincident with IC 443 and the ] emission region, though is not well understood whether it is physically associated with the remnant or not.


In the northeast, where the brightest optical filaments are located, the SNR is interacting with In the northeast, where the brightest optical filaments are located, the SNR is interacting with

Revision as of 20:56, 13 January 2015

Supernova Remnant IC 443
Part of the northeastern shell of IC 443, aka the Jellyfish Nebula
Event typeSupernova remnant Edit this on Wikidata
SN II (?)
ConstellationGemini
Right ascension06 17 13
Declination+22° 31′ 05′′
EpochJ2000
Galactic coordinatesG189.1+3.0
Distance5000 light-years, or 1.5 kpc
RemnantMixed Morphology
HostMilky Way
Notable featuresInteraction with molecular clouds
Other designationsIC 443, PGC 2817561, SNR G189.0+03.0, SNR G189.1+03.0, SNR G189.1-03.0, 1ES 0613+22.7, 1ES 0614+22.7, 2C 537, 3C 157, 4C 22.15, LBN 844, LBN 189.13+02.97, SH 2-248, LEDA 2817561, 3FHL J0617.2+2234e, 2EG J0618+2234, 2U 0601+21, 3A 0614+224, 3CR 157, 3EG J0617+2238, 3U 0620+23, 4U 0617+23, ASB 26, CTB 20, INTREF 295, PKS 0615+226, VRO 22.06.01, WKB 0614+22.7, [DGW65] 34, 2FGL J0617.2+2234e, 3FGL J0617.2+2234e, 2FHL J0617.2+2234e
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[edit on Wikidata]

IC 443 (also known as the Jellyfish Nebula and Sharpless 248 (Sh2-248)) is a Galactic supernova remnant (SNR) in the constellation Gemini. On the plan of the sky, it is located near the star Eta Geminorum. Its distance is roughly 5,000 light years from Earth.

IC 443 may be the remains of a supernova that occurred 3,000 - 30,000 years ago. The same supernova event likely created the neutron star CXOU J061705.3+222127, the collapsed remnant of the stellar core. IC 443 is one of the best-studied cases of supernova remnants interacting with surrounding molecular clouds.

Global Properties

IC 443 is an extended source, having an angular diameter of 50 arcmin (by comparison, the full moon is 30 arcmin across). At the estimated distance of 5,000 ly (1,500 parsec) from Earth, it corresponds to a physical size of roughly 70 light years (20 parsec).

The SNR optical and radio morphology is shell-like (e.g. a prototypical shell-like SNR is SN 1006), consisting of two connected sub-shells with different centers and radii. A third larger sub-shell, initially attributed to IC 443, is now recognized as a different and older (100,000 years) SNR, called G189.6+3.3.
Notably, IC 443 X-ray morphology is centrally peaked and a very soft X-ray shell is barely visible. Unlike plerion remnants, e.g. the Crab Nebula, the inner X-ray emission is not dominated by the central pulsar wind nebula. It has indeed a thermal origin. IC 443 shows very similar features to the class of mixed morphology SNRs. Both optical and X-ray emission are heavily absorbed by a giant molecular cloud in the foreground, crossing the whole remnant body from northwest to southeast.

The remnant's age is still uncertain. There is some agreement that the progenitor supernova happened between 3,000 and 30,000 years ago. Recent Chandra and XMM-Newton observations identified a plerion nebula, close to the remnant southern rim. The point source near the apex of the nebula is a neutron star, relic of a SN explosion. The location in a star forming region and the presence of a neutron star favor a Type II supernova, the ultimate fate of a massive star, as the progenitor explosion.

The SNR environment

IC 443 wide field image. The stars η (right) and μ (left) Geminorum, the diffuse emission from S249 (north), and the G189.6+3.3 partial shell (center) are visible.

The SNR IC 443 is located in the Galactic anticenter direction (l=189.1°), close to the Galactic plane (b=+3.0°). Many objects lie in the same region of sky: the HII region S249, several young stars (members of the GEM OB1 association), and an older SNR (G189.6+3.3).

The remnant is evolving in a rich and complex environment, which strongly affects its morphology. Multi-wavelength observations show the presence of sharp density gradients and different cloud geometries in the surroundings of IC 443. Massive stars are known to be short lived (roughly 30 million years), ending their life when they are still embedded within the progenitor cloud. The more massive stars (O-type) probably clear the circum-stellar environment by powerful stellar winds or photoionizing radiation. Early B-type stars, with a typical mass between 8 and 12 solar masses, are not capable of this, and they likely interact with the primordial molecular cloud when they explode. Thus, it is not surprising that the SNR IC 443, which is thought to be the aftermath of a stellar explosion, evolved in such a complex environment. For instance, an appreciable fraction of supernova remnants lies close to dense molecular clouds (~50 out of 265 in the Green catalogue), and most of them (~60%) show clear signs of interaction with the adjacent cloud.

X-ray and the optical images are characterized by a dark lane, crossing IC 443 from northwest to southeast. Emission from quiescent molecular gas has been observed toward the same direction, and it is likely due to a giant molecular cloud, located between the remnant and the observer. This is the main source of extinction of the low energy SNR emission.

In the southeast the blast wave is interacting with a very dense (~10,000 cm) and clumpy molecular cloud, such that the emitting shocked gas has a ring-like shape. The blast wave has been strongly decelerated by the cloud and is moving with an estimated velocity of roughly 30–40 km s. OH (1720 MHz) maser emission, which is a robust tracer of interaction between SNRs and dense molecular clouds, has been detected in this region. Interestingly, a source of gamma-ray radiation is spatially coincident with IC 443 and the maser emission region, though is not well understood whether it is physically associated with the remnant or not.

In the northeast, where the brightest optical filaments are located, the SNR is interacting with a very different environment. The forward shock has encountered a wall of neutral hydrogen (HI), and is propagating into a less dense medium (~10-1,000 cm) with a much higher velocity (80–100 km s) than in the southern ridge.

In the western region, the shock wave breaks out into a more homogeneous and rarefied medium.

References

  1. Asaoka, I. & Aschenbach, B.; Aschenbach (1994). "An X-ray study of IC 443 and the discovery of a new supernova remnant by ROSAT". Astronomy & Astrophysics. 284: 573. Bibcode:1994A&A...284..573A.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  2. ^ Troja, E.; Reale, F.; et al. (2006). "XMM-Newton Observations of the SNR IC 443. I. Soft X-Ray Emission from Shocked Interstellar Medium". Astrophysical Journal. 649 (1): 258. arXiv:astro-ph/0606313. Bibcode:2006ApJ...649..258T. doi:10.1086/506378. {{cite journal}}: Explicit use of et al. in: |author2= (help); Unknown parameter |authors= ignored (help); Unknown parameter |displayauthors= ignored (|display-authors= suggested) (help)
  3. ^ Petre, R.; Seward, F. D.; Willingale, R.; et al. (1988). "A comprehensive study of the X-ray structure and spectrum of IC 443". Astrophysical Journal. 335: 215. Bibcode:1988ApJ...335..215P. doi:10.1086/166922. {{cite journal}}: Explicit use of et al. in: |author2= (help); Unknown parameter |authors= ignored (help); Unknown parameter |displayauthors= ignored (|display-authors= suggested) (help)
  4. Rho, J. & Petre, R.; Petre (1998). "Mixed-Morphology Supernova Remnants". Astrophysical Journal Letters. 503 (2): L167. Bibcode:1998ApJ...503L.167R. doi:10.1086/311538.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  5. Chevalier, R. (1999). "Supernova Remnants in Molecular Clouds". Astrophysical Journal. 511 (2): 798. arXiv:astro-ph/9805315. Bibcode:1999ApJ...511..798C. doi:10.1086/306710.
  6. Olbert, C. M.; Williams; Keohane; Frail; et al. (2001). "A Bow Shock Nebula around a Compact X-Ray Source in the Supernova Remnant IC 443". Astrophysical Journal Letters. 554 (2): L205. arXiv:astro-ph/0103268. Bibcode:2001ApJ...554L.205O. doi:10.1086/321708. {{cite journal}}: Explicit use of et al. in: |author2= (help); Unknown parameter |displayauthors= ignored (|display-authors= suggested) (help)
  7. Bocchino, F. & Bykov, A. M.; Bykov (2001). "The plerion nebula in IC 443: The XMM-Newton view". Astronomy & Astrophysics. 376 (1): 248. arXiv:astro-ph/0106417. Bibcode:2001A&A...376..248B. doi:10.1051/0004-6361:20010882.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  8. Green, D. A (2006), "A Catalogue of Galactic Supernova Remnants (2006 April version)", Astrophysics Group, Cavendish Laboratory, Cambridge, United Kingdom
  9. Cornett, R. H.; Knapp; et al. (1977). "Observations of CO emission from a dense cloud associated with the supernova remnant IC 443". Astronomy & Astrophysics. 54: 889. Bibcode:1977A&A....54..889C. {{cite journal}}: Explicit use of et al. in: |author2= (help); Unknown parameter |displayauthors= ignored (|display-authors= suggested) (help)
  10. ^ Rho, J.; Cutri, R. M.; Reach, W. T.; et al. (2001). "Near-Infrared Imaging and OI Spectroscopy of IC 443 using Two Micron All Sky Survey and Infrared Space Observatory". Astrophysical Journal. 547 (2): 885. Bibcode:2001ApJ...547..885R. doi:10.1086/318398. {{cite journal}}: Explicit use of et al. in: |author2= (help); Unknown parameter |authors= ignored (help); Unknown parameter |displayauthors= ignored (|display-authors= suggested) (help)
  11. Hewitt, J. W.; Wardle; Roberts; Kassim; et al. (2006). "Green Bank Telescope Observations of IC 443: The Nature of OH (1720 MHz) Masers and OH Absorption". Astrophysical Journal. 652 (2): 1288. arXiv:astro-ph/0602210. Bibcode:2006ApJ...652.1288H. doi:10.1086/508331. {{cite journal}}: Explicit use of et al. in: |author2= (help); Unknown parameter |displayauthors= ignored (|display-authors= suggested) (help)
  12. Albert, J.; Anderhub, H.; Antoranz, P.; Armada, A.; Baixeras, C.; Barrio, J. A.; Bartko, H.; Bastieri, D.; Becker, J. K.; Bednarek, W.; Berger, K.; Bigongiari, C.; Biland, A.; Bock, R. K.; Bordas, P.; Bosch-Ramon, V.; Bretz, T.; Britvitch, I.; Camara, M.; Carmona, E.; Chilingarian, A.; Coarasa, J. A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Costado, M. T.; Curtef, V.; Danielyan, V.; Dazzi, F.; et al. (2007). "Discovery of Very High Energy Gamma Radiation from IC 443 with the MAGIC Telescope". Astrophysical Journal Letters. 664 (2): L87. arXiv:0705.3119. Bibcode:2007ApJ...664L..87A. doi:10.1086/520957. {{cite journal}}: Explicit use of et al. in: |author2= (help); Unknown parameter |authors= ignored (help); Unknown parameter |displayauthors= ignored (|display-authors= suggested) (help)

External links

Sharpless catalog
Categories: