Isolated X-ray-infrared sources in the region of interaction of the supernova remnant IC 443 with a molecular cloud

A. M. Bykov, A. M. Krassilchtchikov, Yu A. Uvarov, H. Bloemen, F. Bocchino, G. M. Dubner, E. B. Giacani, G. G. Pavlov

Research output: Contribution to journalArticle

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Abstract

The nature of the extended hard X-ray source XMMU J061804.3+222732 and its surroundings is investigated using XMM-Newton, Chandra, and Spitzer observations. This source is located in an interaction region of the IC 443 supernova remnant with a neighboring molecular cloud. The X-ray emission consists of a number of bright clumps embedded in an extended structured nonthermal X-ray nebula larger than 30″ in size. Some clumps show evidence for line emission at ∼1.9 and ∼3.7 keV at the 99% confidence level. Large-scale diffuse radio emission of IC 443 passes over the source region, with an enhancement near the source. An IR source of about 14″ × 7″ size is prominent in the 24, 70, and 2.2 μm bands, adjacent to a putative Si K-shell X-ray line emission region. The observed IR/X-ray morphology and spectra are consistent with those expected for J/C-type shocks of different velocities driven by fragmented supernova ejecta colliding with the dense medium of a molecular cloud. The IR emission of the source detected by Spitzer can be attributed to both continuum emission from an H II region created by the ejecta fragment and line emission excited by shocks. This source region in IC 443 may be an example of a rather numerous population of hard X-ray/IR sources created by supernova explosions in the dense environment of star-forming regions. Alternative Galactic and extragalactic interpretations of the observed source are also discussed.

Original languageEnglish (US)
Pages (from-to)1050-1063
Number of pages14
JournalAstrophysical Journal
Volume676
Issue number2
DOIs
StatePublished - Apr 1 2008

Fingerprint

supernova remnants
molecular clouds
x rays
interactions
ejecta
clumps
supernovae
shock
explosion
H II regions
XMM-Newton telescope
radio emission
nebulae
newton
shell
radio
explosions
confidence
fragments
continuums

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Bykov, A. M., Krassilchtchikov, A. M., Uvarov, Y. A., Bloemen, H., Bocchino, F., Dubner, G. M., ... Pavlov, G. G. (2008). Isolated X-ray-infrared sources in the region of interaction of the supernova remnant IC 443 with a molecular cloud. Astrophysical Journal, 676(2), 1050-1063. https://doi.org/10.1086/529117
Bykov, A. M. ; Krassilchtchikov, A. M. ; Uvarov, Yu A. ; Bloemen, H. ; Bocchino, F. ; Dubner, G. M. ; Giacani, E. B. ; Pavlov, G. G. / Isolated X-ray-infrared sources in the region of interaction of the supernova remnant IC 443 with a molecular cloud. In: Astrophysical Journal. 2008 ; Vol. 676, No. 2. pp. 1050-1063.
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abstract = "The nature of the extended hard X-ray source XMMU J061804.3+222732 and its surroundings is investigated using XMM-Newton, Chandra, and Spitzer observations. This source is located in an interaction region of the IC 443 supernova remnant with a neighboring molecular cloud. The X-ray emission consists of a number of bright clumps embedded in an extended structured nonthermal X-ray nebula larger than 30″ in size. Some clumps show evidence for line emission at ∼1.9 and ∼3.7 keV at the 99{\%} confidence level. Large-scale diffuse radio emission of IC 443 passes over the source region, with an enhancement near the source. An IR source of about 14″ × 7″ size is prominent in the 24, 70, and 2.2 μm bands, adjacent to a putative Si K-shell X-ray line emission region. The observed IR/X-ray morphology and spectra are consistent with those expected for J/C-type shocks of different velocities driven by fragmented supernova ejecta colliding with the dense medium of a molecular cloud. The IR emission of the source detected by Spitzer can be attributed to both continuum emission from an H II region created by the ejecta fragment and line emission excited by shocks. This source region in IC 443 may be an example of a rather numerous population of hard X-ray/IR sources created by supernova explosions in the dense environment of star-forming regions. Alternative Galactic and extragalactic interpretations of the observed source are also discussed.",
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Bykov, AM, Krassilchtchikov, AM, Uvarov, YA, Bloemen, H, Bocchino, F, Dubner, GM, Giacani, EB & Pavlov, GG 2008, 'Isolated X-ray-infrared sources in the region of interaction of the supernova remnant IC 443 with a molecular cloud', Astrophysical Journal, vol. 676, no. 2, pp. 1050-1063. https://doi.org/10.1086/529117

Isolated X-ray-infrared sources in the region of interaction of the supernova remnant IC 443 with a molecular cloud. / Bykov, A. M.; Krassilchtchikov, A. M.; Uvarov, Yu A.; Bloemen, H.; Bocchino, F.; Dubner, G. M.; Giacani, E. B.; Pavlov, G. G.

In: Astrophysical Journal, Vol. 676, No. 2, 01.04.2008, p. 1050-1063.

Research output: Contribution to journalArticle

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AU - Krassilchtchikov, A. M.

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N2 - The nature of the extended hard X-ray source XMMU J061804.3+222732 and its surroundings is investigated using XMM-Newton, Chandra, and Spitzer observations. This source is located in an interaction region of the IC 443 supernova remnant with a neighboring molecular cloud. The X-ray emission consists of a number of bright clumps embedded in an extended structured nonthermal X-ray nebula larger than 30″ in size. Some clumps show evidence for line emission at ∼1.9 and ∼3.7 keV at the 99% confidence level. Large-scale diffuse radio emission of IC 443 passes over the source region, with an enhancement near the source. An IR source of about 14″ × 7″ size is prominent in the 24, 70, and 2.2 μm bands, adjacent to a putative Si K-shell X-ray line emission region. The observed IR/X-ray morphology and spectra are consistent with those expected for J/C-type shocks of different velocities driven by fragmented supernova ejecta colliding with the dense medium of a molecular cloud. The IR emission of the source detected by Spitzer can be attributed to both continuum emission from an H II region created by the ejecta fragment and line emission excited by shocks. This source region in IC 443 may be an example of a rather numerous population of hard X-ray/IR sources created by supernova explosions in the dense environment of star-forming regions. Alternative Galactic and extragalactic interpretations of the observed source are also discussed.

AB - The nature of the extended hard X-ray source XMMU J061804.3+222732 and its surroundings is investigated using XMM-Newton, Chandra, and Spitzer observations. This source is located in an interaction region of the IC 443 supernova remnant with a neighboring molecular cloud. The X-ray emission consists of a number of bright clumps embedded in an extended structured nonthermal X-ray nebula larger than 30″ in size. Some clumps show evidence for line emission at ∼1.9 and ∼3.7 keV at the 99% confidence level. Large-scale diffuse radio emission of IC 443 passes over the source region, with an enhancement near the source. An IR source of about 14″ × 7″ size is prominent in the 24, 70, and 2.2 μm bands, adjacent to a putative Si K-shell X-ray line emission region. The observed IR/X-ray morphology and spectra are consistent with those expected for J/C-type shocks of different velocities driven by fragmented supernova ejecta colliding with the dense medium of a molecular cloud. The IR emission of the source detected by Spitzer can be attributed to both continuum emission from an H II region created by the ejecta fragment and line emission excited by shocks. This source region in IC 443 may be an example of a rather numerous population of hard X-ray/IR sources created by supernova explosions in the dense environment of star-forming regions. Alternative Galactic and extragalactic interpretations of the observed source are also discussed.

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Bykov AM, Krassilchtchikov AM, Uvarov YA, Bloemen H, Bocchino F, Dubner GM et al. Isolated X-ray-infrared sources in the region of interaction of the supernova remnant IC 443 with a molecular cloud. Astrophysical Journal. 2008 Apr 1;676(2):1050-1063. https://doi.org/10.1086/529117