Molecular Environments of Supernova Remnants

Chen, Yang; Jiang, Bin; Zhou, Ping; Su, Yang; Zhou, Xin; Li, Hui; Zhang, Xiao

doi:10.1017/s1743921313009423

Cited by 18 publications

(17 citation statements)

References 39 publications

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“…The integrated CO line emission with a high high-to-low excitation line ratio in the line wing is suggested as a probe of the SNR-MC interaction (Seta et al 1998;Jiang et al 2010;Chen et al 2014). The 12 CO (J=2-1) / 12 CO (J=1-0) ratio map in the left (blue) wing 85 − 88 km s −1 is shown in Figure 7.…”

Section: Co Line Emissionmentioning

confidence: 98%

A Study of Fermi-LAT GeV γ-Ray Emission toward the Magnetar-harboring Supernova Remnant Kesteven 73 and Its Molecular Environment

Liu

Chen

Zhang

et al. 2017

ApJ

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We report our independent GeV γ-ray study of the young shell-type supernova remnant (SNR) Kes 73 which harbors a central magnetar, and CO-line millimeter observations toward the SNR. Using 7.6 years of Fermi-LAT observation data, we detected an extended γ-ray source ("source A") with centroid on the west of the SNR, with a significance of 21σ in 0.1-300 GeV and an error circle of 5.′ 4 in angular radius. The γ-ray spectrum cannot be reproduced by a pure leptonic emission or a pure emission from the magnetar, and thus a hadronic emission component is needed. The CO-line observations reveal a molecular cloud (MC) at V LSR ∼ 90 km s −1 , which demonstrates morphological correspondence with the western boundary of the SNR brightened in multiwavelength. The 12 CO (J=2-1)/ 12 CO (J=1-0) ratio in the left (blue) wing 85-88 km s −1 is prominently elevated to ∼ 1.1 along the northwestern boundary, providing kinematic evidence of the SNR-MC interaction. This SNR-MC association yields a kinematic distance 9 kpc to Kes 73. The MC is shown to be capable of accounting for the hadronic γ-ray emission component. The γ-ray spectrum can be interpreted with a pure hadronic emission or a magnetar+hadronic hybrid emission. In the case of pure hadronic emission, the spectral index of the protons is 2.4, very similar to that of the radio-emitting electrons, essentially consistent with the diffusive shock

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Section: Co Line Emissionmentioning

confidence: 98%

A Study of Fermi-LAT GeV γ-Ray Emission toward the Magnetar-harboring Supernova Remnant Kesteven 73 and Its Molecular Environment

Liu

Chen

Zhang

et al. 2017

ApJ

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“…Further observations, for example, searching for 1720 MHz OH maser around the remnant (see discussion in Chen et al 2014 andGiacani 2015), are needed to verify the physical association between the large cavity and remnant.…”

Section: Possibility Of the Random Distribution Of A Cavitymentioning

confidence: 99%

Large-field CO (1–0) observations toward the Galactic historical supernova remnants: a large cavity aroundTycho’s supernova remnant

Chen¹,

Xiong²,

Yang³

2017

A&A

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Context. The investigation of the interaction between the supernova remnants (SNRs) and interstellar gas is not only necessary to improve our knowledge of SNRs, but also to understand the nature of the progenitor systems. Aims. As a part of the Milky Way Imaging Scroll Painting CO line survey, the aim is to study the interstellar gas surrounding the Galactic historical SNRs. In this work, we present the CO results of Tycho's SNR. Methods. Using the 3×3 Superconducting Spectroscopic Array Receiver (SSAR) at the PMO 13.7-meter telescope, we performed large-field (3 • × 2 • ) and high-sensitivity CO (1-0) molecular line observations toward Tycho's SNR. Results. The CO observations reveal large molecular clouds, stream-like structures, and an inner rim around the remnant. We derived the basic properties (column density, mass, and kinematics) of these objects based on the CO observations. The large molecular clouds individually show an arc toward the remnant center, outlining a large cavity with radii of ∼ 0.3 • × 0.6 • (or 13 pc × 27 pc at a distance of 2.5 kpc) around the remnant. The CO line broadenings and asymmetries detected in the surrounding clouds, the observed expansion of the cavity, in concert with enhanced 12 CO (2-1)/(1-0) intensity ratio detected in previous studies, suggest the interaction of the large cavity with a wind in the region. After excluding the scenario of a large bubble produced by bright massive stars, we suggest that the large cavity could be explained by accretion wind from the progenitor system of Tycho's supernova. Nevertheless, the possibility of the random distribution of a large cavity around Tycho's SNR cannot be ruled out thus far. Further observations are needed to confirm the physical association of the large cavity with Tycho's SNR.

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“…So far, there are several signposts to show the physical contact/interaction between SNRs and their molecular environments, e.g., the presence of 1720 MHz OH maser emission, molecular line broadenings or asymmetric profiles, high molecular line ratios between different excitation states, detection of H 2 and/or [Fe II] lines in near-infrared, specific infrared colors within an SNR, and often used morphological correspondence in multiwavelength with SNR features (see Jiang et al 2010). It is also important to study the interplay of SNR-MC systems for investigating various physical and astrophysical processes therein (e.g., Chen et al 2014;Dubner & Giacani 2015;Slane et al 2015).…”

Section: Introductionmentioning

confidence: 99%

“…There are currently 294 SNRs known in the Milky Way (Green 2014) and about 70 of them are confirmed or suggested to be associated with MCs (refer to, e.g., Jiang et al 2010;Chen et al 2014). CO, as an indicator of H 2 , is the most widely used tracer of MCs and it is very common and useful when investigating the nature of the molecular ISM in galaxies.…”

Section: Introductionmentioning

confidence: 99%

Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

Zhou

Yang

et al. 2017

ApJ

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We present CO observations toward three large supernova remnants (SNRs) in the third Galactic quadrant using the Purple Mountain Observatory Delingha 13.7 m millimeter-wavelength telescope. The observations are part of the high-resolution CO survey of the Galactic plane between Galactic longitudes l = −10• to 250• and latitudes b = −5• to 5• . CO emission was detected toward the three SNRs: G205.5+0.5 (Monoceros Nebula), G206.9+2.3 (PKS 0646+06), and G213.0−0.6. Both of SNRs G205.5+0.5 and G213.0−0.6 exhibit the morphological agreement (or spatial correspondences) between the remnant and the surrounding molecular clouds (MCs), as well as kinematic signatures of shock perturbation in the molecular gas. We confirm that the two SNRs are physically associated with their ambient MCs and the shock of SNRs is interacting with the dense, clumpy molecular gas. SNR G206.9+2.3, which is close to the northeastern edge of the Monoceros Nebula, displays the spatial coincidence with molecular partial shell structures at V LSR ∼ 15 km s −1 . While no significant line broadening has been detected within or near the remnant, the strong morphological correspondence between the SNR and the molecular cavity implies that SNR G206.9+2.3 is probably associated with the CO gas and is evolving in the low-density environment. The physical features of individual SNRs, together with the relationship between SNRs and their nearby objects, are also discussed.

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Molecular Environments of Supernova Remnants

Cited by 18 publications

References 39 publications

A Study of Fermi-LAT GeV γ-Ray Emission toward the Magnetar-harboring Supernova Remnant Kesteven 73 and Its Molecular Environment

A Study of Fermi-LAT GeV γ-Ray Emission toward the Magnetar-harboring Supernova Remnant Kesteven 73 and Its Molecular Environment

Large-field CO (1–0) observations toward the Galactic historical supernova remnants: a large cavity aroundTycho’s supernova remnant

Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

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