CO Observations toward Supernova Remnants with Associated OH 1720 MHz Masers

Reynoso, E. M.; Mangum, J. G.

doi:10.1086/317854

Cited by 64 publications

(118 citation statements)

References 44 publications

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“…The radio shell appears to brighten along the southern edge, where Green et al (1997) detected a single maser at +20 km s À1 . CO clouds at a velocity of +25 km s À1 are present at the location of the maser, as well as in the interior and northwestern edge, confirming the interaction ( Reynoso & Mangum 2000).…”

Section: G167+01supporting

confidence: 57%

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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Section: G167+01supporting

confidence: 57%

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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“…In a few cases, the end-stage interaction of an SNR with molecular gas in the ambient ISM is apparent and these special cases have been studied with great interest; particular examples include IC443 and W44 (Denoyer 1979(Denoyer , 1983, W28 (Wootten 1981;Denoyer 1983;Arikawa et al 1999;Aharonian 2008), Vela (Moriguchi et al 2001) and others noted by Arikawa et al (1999), Reynoso & Mangum (2000) and Moriguchi et al (2005).…”

Section: Introductionmentioning

confidence: 99%

CO $\mathsf{J}=\mathsf{1}{-}0$ observations of gas near the galactic supernova remnants G5.4-1.2, G5.55+0.32 and G5.71-0.08

Liszt

2009

A&A

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Results. Although broad CO lines characteristic of shocked gas were not seen in this kinematically complex region, a bright (14 K), new, marginally-resolved ±9 km s −1 outflow source G5.638+0.233 and a comparably bright rim of CO emission were found at/around the periphery of SNR G5.55+0.12. Most of the periphery of SNR G5.71-0.08 is surrounded by a bright rim of CO emission. CO emission at the 7 km s −1 velocity of a 1720 OH maser spot near SNR G5.70-0.12 is very bright, 19 K, but gas at −21 km s −1 is widespread over the region and CO emission is rather weak toward the OH maser spots at this velocity north of G5.4-1.2. Other very bright CO lines in the region are associated with H II regions, i.e. 27 K toward W28A2 = G5.89-0.39 and 15 K toward an MSX-IR source at l = 5.9 o , b = −0.13 o which is probably the exciting agent of a separate, classical HII region just north of W28A2.

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“…A C-type shock caused by expanding supernova remnant will create such conditions (Elitzur 1976;Lockett et al 1999). This has been confirmed by many molecular line observations (Koralesky et al 1998;Reach & Rho 1998;Frail & Mitchell 1998;Reynoso et al 2000). We took CO(1-0) observations towards the SNRs G21.8-0.6 and G32.8-0.1, both of which are associated with 1720 MHz OH masers.…”

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confidence: 72%

Possible CO clouds interacting with the SNRs G21.8-0.6 and G32.8-0.1

et al. 2007

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Abstract. We have obtained the first CO(1-0) maps towards the SNRs G21.8-0.6 and G32.8-0.1, which are associated with OH 1720 MHz masers. Based on the morphological correspondence between the radio remnant and the CO cloud, and the velocity and position agreement between the OH maser and CO clouds, we tentatively suggest the clouds may be interacting with G21.8-0.6 and G32.8-0.1. However, the shock-excited line broadening was not obvious for these two SNRs. We discuss the possible reasons for this.

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CO Observations toward Supernova Remnants with Associated OH 1720 MHz Masers

Cited by 64 publications

References 44 publications

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

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

CO $\mathsf{J}=\mathsf{1}{-}0$ observations of gas near the galactic supernova remnants G5.4-1.2, G5.55+0.32 and G5.71-0.08

Possible CO clouds interacting with the SNRs G21.8-0.6 and G32.8-0.1

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