Shock-excited Maser Emission from Supernova Remnants: G32.8−0.1, G337.8−0.1, G346.6−0.2, and the HB 3/W3 Complex

Koralesky, Barron; Frail, D. A.; Goss, W. M.; Claussen, M. J.; Green, Anne

doi:10.1086/300508

Cited by 123 publications

(141 citation statements)

References 71 publications

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“…Therefore, we do not consider these radio sources to be associated with G352.7−0.1. We note that Green et al (1997) and Koralesky et al (1998) detected OH maser emission at 1720 MHz from G352.7−0.1. Such emission is closely associated with interactions between SNRs and molecular clouds.…”

Section: Introductionmentioning

confidence: 68%

XMM-NEWTONANDCHANDRAOBSERVATIONS OF THE EJECTA-DOMINATED MIXED-MORPHOLOGY GALACTIC SUPERNOVA REMNANT G352.7–0.1

Pannuti

Kargaltsev

Napier

et al. 2014

ApJ

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We present a spatial and spectral X-ray analysis of the Galactic supernova remnant (SNR) G352.7−0.1 using archival data from observations made with the XMM-Newton X-ray Observatory and the Chandra X-ray Observatory. Prior X-ray observations of this SNR had revealed a thermal center-filled morphology that contrasts with a shell-like radio morphology, thus establishing G352.7−0.1 as a member of the class of Galactic SNRs known as mixedmorphology SNRs (MMSNRs). Our study confirms that the X-ray emission comes from the SNR interior and must be ejecta dominated. Spectra obtained with XMM-Newton may be fit satisfactorily with a single thermal component (namely a non-equilibrium ionization component with enhanced abundances of silicon and sulfur). In contrast, spectra extracted by Chandra from certain regions of the SNR cannot always be fit by a single thermal component. For those regions, a second thermal component with solar abundances or two thermal components with different temperatures and thawed silicon and sulfur abundances (respectively) can generate a statistically acceptable fit. We argue that the former scenario is more physically plausible: on the basis of parameters of our spectral fits, we calculate physical parameters including X-ray emitting mass (∼45 M for solar abundances). We find no evidence for overionization in the X-ray emitting plasma associated with the SNR: this phenomenon has been seen in other MMSNRs. We have conducted a search for a neutron star within the SNR by using a hard (2-10 keV) Chandra image but could not identify a firm candidate. We also present (for the first time) the detection of infrared emission from this SNR as detected at 24 μm by the MIPS on board Spitzer. Finally, we discuss the properties of G352.7−0.1 in the context of other ejecta-dominated MMSNRs.

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Section: Introductionmentioning

confidence: 68%

XMM-NEWTONANDCHANDRAOBSERVATIONS OF THE EJECTA-DOMINATED MIXED-MORPHOLOGY GALACTIC SUPERNOVA REMNANT G352.7–0.1

Pannuti

Kargaltsev

Napier

et al. 2014

ApJ

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“…The image is smoothed with a Gaussian of width 20 . The yellow crosses indicate the location of the 1720 MHz OH masers detected with the VLA (Koralesky et al 1998). …”

Section: Resultsmentioning

confidence: 99%

An XMM-Newton Study of the Mixed-morphology Supernova Remnant G346.6-0.2

Auchettl

Wong

et al. 2017

ApJ

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We present an X-ray imaging and spectroscopic study of the molecular cloud interacting mixedmorphology (MM) supernova remnant (SNR) G346.6-0.2 using XMM-Newton. The X-ray spectrum of the remnant is well described by a recombining plasma that most likely arises from adiabatic cooling, and has sub-solar abundances of Mg, Si, and S. Our fits also suggest the presence of either an additional power-law component with a photon index of ∼2, or an additional thermal component with a temperature of ∼2.0 keV. We investigate the possible origin of this component and suggest that it could arise from either the Galactic ridge X-ray emission, an unidentified pulsar wind nebula or Xray synchrotron emission from high-energy particles accelerated at the shock. However, deeper, high resolution observations of this object are needed to shed light on the presence and origin of this feature. Based on its morphology, its Galactic latitude, the density of the surrounding environment and its association with a dense molecular cloud, G346.6-0.2 most likely arises from a massive progenitor that underwent core-collapse.

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“…The necessary OH abundance in the shocked gas (OH=H 2 e10 À6 ) is created by the dissociation of shockproduced water induced by thermal X-rays emitted from the hot gas filling the adjacent supernova remnant (Wardle 1999). Nineteen remnants (about 1 in 10) have 1720 MHz masers and are therefore likely to be interacting with clouds Green et al 1997;Koralesky et al 1998;Yusef-Zadeh et al 1999). The inferred interactions have been confirmed by follow-up searches for millimeter or infrared emission from hot molecular gas or from molecules produced by the rich chemistry occurring within the shock front (e.g., Reach & Rho 1998;Frail & Mitchell 1998;Reynoso & Mangum 2000;Yusef-Zadeh et al 2001;Lazendic et al 2002).…”

Section: Introductionmentioning

confidence: 99%

OH (1720 MHz) Masers and Mixed‐Morphology Supernova Remnants

Yusef‐Zadeh

Wardle

Rho

et al. 2003

ApJ

107

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Radio surveys of supernova remnants (SNRs) in the Galaxy have uncovered 19 SNRs accompanied by OH maser emission at 1720 MHz. This unusual class of maser sources is suggested to be produced behind a shock front from the expansion of a supernova remnant running into a molecular cloud. An important ingredient of this model is that X-ray emission from the remnant enhances the production of OH molecules. The role of X-ray emission from maser-emitting (ME) SNRs is investigated by comparing the X-ray-induced ionization rate with the theory. One aspect of this model is verified: there is a strong association between ME and mixed-morphology or thermal composite SNRs-center-filled thermal X-ray emission surrounded by shell-like radio morphology. We also present ROSAT and ASCA observations of two ME SNRs: G21.8À0.6 (Kes 69) and G357.7À0.1 (Tornado).

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Shock-excited Maser Emission from Supernova Remnants: G32.8−0.1, G337.8−0.1, G346.6−0.2, and the HB 3/W3 Complex

Cited by 123 publications

References 71 publications

XMM-NEWTONANDCHANDRAOBSERVATIONS OF THE EJECTA-DOMINATED MIXED-MORPHOLOGY GALACTIC SUPERNOVA REMNANT G352.7–0.1

XMM-NEWTONANDCHANDRAOBSERVATIONS OF THE EJECTA-DOMINATED MIXED-MORPHOLOGY GALACTIC SUPERNOVA REMNANT G352.7–0.1

An XMM-Newton Study of the Mixed-morphology Supernova Remnant G346.6-0.2

OH (1720 MHz) Masers and Mixed‐Morphology Supernova Remnants

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