IRAS sources associated with shocked gas regions in IC 443

Huang, Y. L.; Dickman, R. L.; Snell, R. L.

doi:10.1086/184638

Cited by 41 publications

(50 citation statements)

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“…Many molecular observations have verified that the temperature (T ¼ 33-100 K) and density [n ¼ ð1 8Þ Â 10 5 cm À3 ] are in accord with OH (1720 MHz) theory (Turner et al 1992;Dickman et al 1992;Ziurys, Snell, & Dickman 1989;van Dishoeck, Jansen, & Phillips 1993;Cesarsky et al 1999;Rho et al 2001). The OH (1720 MHz) masers occur in '' clump G '' of the shocked molecular interaction regions in IC 443 (DeNoyer 1979b;Huang, Dickman, & Snell 1986) and, specifically, subclump G1 as resolved by submillimeter and interferometric observations (van Dishoeck et al 1993;Tauber et al 1994). Nonetheless, an important observational constraint that is still required is the transverse size of the region of OH inversion.…”

Section: Introductionmentioning

confidence: 77%

The Sizes of OH (1720 MHz) Supernova Remnant Masers: MERLIN and Very Long Baseline Array Observations of IC 443

Hoffman

Goss

Brogan

et al. 2003

ApJ

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Section: Introductionmentioning

confidence: 77%

The Sizes of OH (1720 MHz) Supernova Remnant Masers: MERLIN and Very Long Baseline Array Observations of IC 443

Hoffman

Goss

Brogan

et al. 2003

ApJ

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“…Located at a distance of 1.5 kpc in a direction largely free of the confusion present toward the Galactic plane, it was well suited for some of the earliest studies of molecular tracers of shock excitation ( Huang et al 1986). Evidence of IC 443's interaction was first observed as large line width, negative velocity neutral hydrogen by DeNoyer (1978).…”

Section: G1892+30 ( Ic 443)mentioning

confidence: 99%

“…Evidence of IC 443's interaction was first observed as large line width, negative velocity neutral hydrogen by DeNoyer (1978). Huang et al (1986) identified a series of shocked CO clumps (designated A-H ) along the southern ridge, with sizes ranging from 0.5 to 5 pc. Further high-resolution study revealed shocked molecular line emission tracing out a ring of perturbed molecular gas about the center of the remnant (van Dishoeck et al 1993).…”

Section: G1892+30 ( Ic 443)mentioning

confidence: 99%

A Survey of Hydroxyl toward Supernova Remnants: Evidence for Extended 1720 MHz Maser Emission

Hewitt

Yusef‐Zadeh

Wardle

2008

Astrophysical Journal

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We present the results of GBT observations of all four ground-state hydroxyl (OH ) transitions toward 15 supernova remnants (SNRs) which show OH (1720 MHz) maser emission. This species of maser is well established as an excellent tracer of an ongoing interaction between the SNR and dense molecular material. For the majority of these objects we detect significantly higher flux densities with a single dish than have been reported with interferometric observations. We infer that spatially extended, low-level maser emission is a common phenomenon that traces the largescale interaction in maser-emitting SNRs. In addition, we use a collisional pumping model to fit the physical conditions under which OH is excited behind the SNR shock front. We find the observed OH gas associated with the SNR interaction having columns N OH 1:5 ; 10 17 cm À2 , temperatures of 20-125 K, and densities $10 5 cm À3 .

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“…Molecular clouds wrap around the southern rim and the boundary region between shells A and B (Beichman et al 1988;Seta et al 1998;Dickman et al 1992;Dame et al 2001). Molecular lines from shocked gas have been found in several clouds suggesting interaction with the blast wave at multiple sites (e.g., Cornett et al 1977;Denoyer & Frerking 1981;Huang et al 1986;Burton et al 1988;Dickman et al 1992;van Dishoeck et al 1993;Richter et al 1995;Seta et al 1998;Snell et al 2005). A prominent band of H i gas has also been found in the southeastern part of shell A (Denoyer 1978;Giovanelli & Haynes 1979;Lee et al 2008, and references therein.).…”

Section: Discussionmentioning

confidence: 99%

“…The processes include: interaction of SNR shocks with molecular and atomic clouds of various densities which produced a break-out (shell B) from shell A as well as associated small-scale structures; interaction of the half-shells with another SNR G189.6+3.3 (e.g., Asaoka & Aschenbach 1994;Keohane et al 1997); penetration of shock fronts into dense molecular clouds leading to molecular line emission (e.g., Denoyer 1979aDenoyer , 1979bDenoyer & Frerking 1981;Huang et al 1986;Burton et al 1988;van Dishoeck et al 1993;Richter et al 1995;Chevalier 1999;Hewitt et al 2006); and interaction between the PWN and the environment (Olbert et al 2001;Leahy 2004;Gaensler et al 2006;Troja et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Observation of Supernova Remnant IC 443 with the Fermi Large Area Telescope

Abdo¹

2012

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We report observation of the supernova remnant (SNR) IC 443 (G189.1+3.0) with the Fermi Gamma-ray Space Telescope Large Area Telescope (LAT) in the energy band between 200 MeV and 50 GeV. IC 443 is a shell-type SNR with mixed morphology located off the outer Galactic plane where high-energy emission has been detected in the X-ray, GeV and TeV gamma-ray bands. Past observations suggest IC 443 has been interacting with surrounding interstellar matter. Proximity between dense shocked molecular clouds and GeV-TeV gamma-ray emission regions detected by EGRET, MAGIC, and VERITAS suggests an interpretation that cosmic-ray (CR) particles are accelerated by the SNR. With the high gamma-ray statistics and broad energy coverage provided by the LAT, we accurately characterize the gamma-ray emission produced by the CRs accelerated at IC 443. The emission region is extended in the energy band with θ 68 = 0.• 27 ± 0.• 01(stat) ± 0.• 03(sys) for an assumed two-dimensional Gaussian profile and overlaps almost completely with the extended source region of VERITAS. Its centroid is displaced significantly from the known pulsar wind nebula (PWN) which suggests the PWN is not the major contributor in the present energy band. The observed spectrum changes its power-law slope continuously and continues smoothly to the MAGIC and VERITAS data points. The combined gamma-ray spectrum (200 MeV < E < 2 TeV) is reproduced well by decays of neutral pions produced by a broken power-law proton spectrum with a break around 70 GeV.

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IRAS sources associated with shocked gas regions in IC 443

Cited by 41 publications

References 0 publications

The Sizes of OH (1720 MHz) Supernova Remnant Masers: MERLIN and Very Long Baseline Array Observations of IC 443

The Sizes of OH (1720 MHz) Supernova Remnant Masers: MERLIN and Very Long Baseline Array Observations of IC 443

A Survey of Hydroxyl toward Supernova Remnants: Evidence for Extended 1720 MHz Maser Emission

Observation of Supernova Remnant IC 443 with the Fermi Large Area Telescope

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