XMM-Newton Observations of the Supernova Remnant IC 443. I. Soft X-Ray Emission from Shocked Interstellar Medium

Fabio Reale, Eleonora Troja, Fabio Reale, Bocchino

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35 Citazioni (Scopus)

Abstract

The shocked interstellar medium around IC 443 produces strong X-ray emission in the soft energy band (E<~1.5 keV). We present an analysis of such emission as observed with the EPIC MOS cameras on board the XMM-Newton observatory, with the purpose to find clear signatures of the interactions with the interstellar medium (ISM) in the X-ray band, which may complement results obtained in other wavelengths. We found that the giant molecular cloud mapped in CO emission is located in the foreground and gives an evident signature in the absorption of X-rays. This cloud may have a torus shape, and the part of torus interacting with the IC 443 shock gives rise to 2MASS Ks emission in the southeast. The measured density of emitting X-ray-shocked plasma increases toward the northeastern limb, where the remnant is interacting with an atomic cloud. We found an excellent correlation between emission in the 0.3-0.5 keV band and bright optical/radio filament on large spatial scales. The partial shell structure seen in this band therefore traces the encounter with the atomic cloud.
Lingua originaleUndefined/Unknown
pagine (da-a)258-267
RivistaTHE ASTROPHYSICAL JOURNAL
Volume649
Stato di pubblicazionePublished - 2006

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cita questo

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title = "XMM-Newton Observations of the Supernova Remnant IC 443. I. Soft X-Ray Emission from Shocked Interstellar Medium",
abstract = "The shocked interstellar medium around IC 443 produces strong X-ray emission in the soft energy band (E<~1.5 keV). We present an analysis of such emission as observed with the EPIC MOS cameras on board the XMM-Newton observatory, with the purpose to find clear signatures of the interactions with the interstellar medium (ISM) in the X-ray band, which may complement results obtained in other wavelengths. We found that the giant molecular cloud mapped in CO emission is located in the foreground and gives an evident signature in the absorption of X-rays. This cloud may have a torus shape, and the part of torus interacting with the IC 443 shock gives rise to 2MASS Ks emission in the southeast. The measured density of emitting X-ray-shocked plasma increases toward the northeastern limb, where the remnant is interacting with an atomic cloud. We found an excellent correlation between emission in the 0.3-0.5 keV band and bright optical/radio filament on large spatial scales. The partial shell structure seen in this band therefore traces the encounter with the atomic cloud.",
author = "Fabio Reale and Eleonora Troja and Fabio Reale and Bocchino",
year = "2006",
language = "Undefined/Unknown",
volume = "649",
pages = "258--267",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",

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TY - JOUR

T1 - XMM-Newton Observations of the Supernova Remnant IC 443. I. Soft X-Ray Emission from Shocked Interstellar Medium

AU - Reale, Fabio

AU - Troja, Eleonora

AU - Reale, Fabio

AU - Bocchino, null

PY - 2006

Y1 - 2006

N2 - The shocked interstellar medium around IC 443 produces strong X-ray emission in the soft energy band (E<~1.5 keV). We present an analysis of such emission as observed with the EPIC MOS cameras on board the XMM-Newton observatory, with the purpose to find clear signatures of the interactions with the interstellar medium (ISM) in the X-ray band, which may complement results obtained in other wavelengths. We found that the giant molecular cloud mapped in CO emission is located in the foreground and gives an evident signature in the absorption of X-rays. This cloud may have a torus shape, and the part of torus interacting with the IC 443 shock gives rise to 2MASS Ks emission in the southeast. The measured density of emitting X-ray-shocked plasma increases toward the northeastern limb, where the remnant is interacting with an atomic cloud. We found an excellent correlation between emission in the 0.3-0.5 keV band and bright optical/radio filament on large spatial scales. The partial shell structure seen in this band therefore traces the encounter with the atomic cloud.

AB - The shocked interstellar medium around IC 443 produces strong X-ray emission in the soft energy band (E<~1.5 keV). We present an analysis of such emission as observed with the EPIC MOS cameras on board the XMM-Newton observatory, with the purpose to find clear signatures of the interactions with the interstellar medium (ISM) in the X-ray band, which may complement results obtained in other wavelengths. We found that the giant molecular cloud mapped in CO emission is located in the foreground and gives an evident signature in the absorption of X-rays. This cloud may have a torus shape, and the part of torus interacting with the IC 443 shock gives rise to 2MASS Ks emission in the southeast. The measured density of emitting X-ray-shocked plasma increases toward the northeastern limb, where the remnant is interacting with an atomic cloud. We found an excellent correlation between emission in the 0.3-0.5 keV band and bright optical/radio filament on large spatial scales. The partial shell structure seen in this band therefore traces the encounter with the atomic cloud.

UR - http://hdl.handle.net/10447/28421

M3 - Article

VL - 649

SP - 258

EP - 267

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

ER -