A Survey for OH(1720 MHz) Maser Emission Toward Supernova Remnants

Frail, D. A.; Goss, W. M.; Reynoso, E. M.; Giacani, E.; Green, Anne; Otrupcek, Robina E.

doi:10.1086/117904

Cited by 256 publications

(406 citation statements)

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“…Orlando et al 2008). The presence of OH maser emission originating from the shock front can discriminate between these scenarios (Frail et al 1996;Yusef-Zadeh et al 2003), and led to the classification of about 20 Galactic arced remnants such as G31.9+0.0 or G189.1+3.0 as running into a dense cloud.…”

Section: Observations From Maser Emission Such As In 3c391mentioning

confidence: 99%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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After the death of a runaway massive star, its supernova shock wave interacts with the bow shocks produced by its defunct progenitor, and may lose energy, momentum, and its spherical symmetry before expanding into the local interstellar medium (ISM). We investigate whether the initial mass and space velocity of these progenitors can be associated with asymmetric supernova remnants. We run hydrodynamical models of supernovae exploding in the pre-shaped medium of moving Galactic core-collapse progenitors. We find that bow shocks that accumulate more than about 1.5 M ⊙ generate asymmetric remnants. The shock wave first collides with these bow shocks 160 − 750 yr after the supernova, and the collision lasts until 830 − 4900 yr. The shock wave is then located 1.35 − 5 pc from the center of the explosion, and it expands freely into the ISM, whereas in the opposite direction it is channelled into the region of undisturbed wind material. This applies to an initially 20 M ⊙ progenitor moving with velocity 20 km s −1 and to our initially 40 M ⊙ progenitor. These remnants generate mixing of ISM gas, stellar wind and supernova ejecta that is particularly important upstream from the center of the explosion. Their lightcurves are dominated by emission from optically-thin cooling and by X-ray emission of the shocked ISM gas. We find that these remnants are likely to be observed in the [OIII] λ 5007 spectral line emission or in the soft energy-band of X-rays. Finally, we discuss our results in the context of observed Galactic supernova remnants such as 3C391 and the Cygnus Loop.

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Section: Observations From Maser Emission Such As In 3c391mentioning

confidence: 99%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…OH maser emission arises from a wide range of astrophysical objects, such as high-mass star forming regions (e.g., Argon et al 2000), evolved stars (e.g., Nguyen-Q- Rieu et al 1979), supernova remnants (SNRs; e.g., Frail et al 1996), comets (Gérard et al 1998), and active galactic nuclei (Baan et al 1982). In the particular case of evolved stars, groundstate OH maser emission at 18 cm is widespread in the circumstellar envelopes of oxygen-rich stars during the asymptotic giant branch (AGB) phase (Engels & Bunzel 2015), which is characterized by strong mass loss (up to 10 4 - M e yr −1 , Vassiliadis & Wood 1993;Blöcker 1995).…”

Section: Introductionmentioning

confidence: 99%

“…Also, some evolved stars show maser emission at 1665 and 1667 MHz (e.g., Hu 1994; Deacon et al 2004), the velocities of which are close to that of the 1612 MHz masers (Deacon et al 2004). The 1720 MHz OH masers are best known to be associated with shocks created by SNRs interacting with surrounding molecular clouds (Frail et al 1996;Green et al 1997). The 1720 MHz maser transition has never been detected in AGB stars and is extremely rare in other evolved sources, i.e., it has only been detected in one post-AGB star (OH009.1−0.4; IRAS 18043−2116; Sevenster & Chapman 2001) and one Planetary Nebula (PN) (K 3−35; Gómez et al 2009).…”

Section: Introductionmentioning

confidence: 99%

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Qiao

Walsh

Gómez

et al. 2016

ApJ

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We report on OH maser emission toward G336.644−0.695 (IRAS 16333−4807), which is a H 2 O maser-emitting Planetary Nebula (PN). We have detected 1612, 1667, and 1720 MHz OH masers at two epochs using the Australia Telescope Compact Array, hereby confirming it as the seventh known case of an OH-maser-emitting PN. This is only the second known PN showing 1720 MHz OH masers after K 3−35 and the only evolved stellar object with 1720 MHz OH masers as the strongest transition. This PN is one of a group of very young PNe. The 1612 MHz and 1667 MHz masers are at a similar velocity to the 22 GHz H 2 O masers, whereas the 1720 MHz masers show a variable spectrum, with several components spread over a higher velocity range (up to 36 km s −1 ). We also detect Zeeman splitting in the 1720 MHz transition at two epochs (with field strengths of ∼2 to ∼10 mG), which suggests the OH emission at 1720 MHz is formed in a magnetized environment. These 1720 MHz OH masers may trace short-lived equatorial ejections during the formation of the PN.

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“…In an early CO-line survey toward 26 outer (l = 70 • -210 • ) Galactic SNRs, about half were found spatially coincident with large MC complexes (Huang & Thaddeus 1986). After a survey of 1720 MHz OH maser emission towards Galactic SNRs, Frail et al (1996) and Green et al (1997) revealed the unique diagnostic relation between such masers and the SNR shocks in MCs and identified nearly a score of SNRs interacting with MCs. Seta et al (1998) listed 26 SNRs detected in CO-and H 2 -line emissions along the line of sight, but no physical evidence of shock-MC interaction was given for them.…”

Section: Census Of Snr-mc Associationsmentioning

confidence: 99%

Molecular Environments of Supernova Remnants

Chen

Jiang²,

Zhou³

et al. 2013

Proc. IAU

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Abstract. There are about 70 Galactic supernova remnants (SNRs) that are now confirmed or suggested to be in physical contact with molecular clouds (MCs) with six kinds of evidence of multiwavelength observations. Recent detailed CO-line spectroscopic mappings of a series of SNRs reveal them to be in cavities of molecular gas, implying the roles the progenitors may have played. We predict a linear correlation between the wind bubble sizes of main-sequence OB stars in a molecular environment and the stellar masses and discuss its implication for supernova progenitors. The molecular environments of SNRs can serve as a good probe for the γ-rays arising from the hadronic interaction of the accelerated protons, and this paper also discusses the γ-ray emission from MCs illuminated by diffusive protons that escape from SNR shocks.

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A Survey for OH(1720 MHz) Maser Emission Toward Supernova Remnants

Cited by 256 publications

References 0 publications

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Molecular Environments of Supernova Remnants

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