A catalogue of Galactic supernova remnants from the Canadian Galactic plane survey

Kothes, R.; Федотов, К. В.; Foster, Tyler; Uyanıker, B.

doi:10.1051/0004-6361:20065062

Cited by 153 publications

(197 citation statements)

References 47 publications

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“…This part of CTB 80 is highly polarized at λ6 cm, and seen in the polarization map at 1.4 GHz (Kothes et al 2006b). The apparent size of this SNR measured from the λ6 cm map is about 128 from east to west and about 96 in the south-north direction, which implies that it has a physical size of 74 pc × 56 pc at 2 kpc.…”

Section: G690+27 (Ctb 80)mentioning

confidence: 91%

“…Strong polarized emission of CTB 80 was observed, which varies with frequency (Mantovani et al 1985). The overall radio spectral index is α = −0.45 ± 0.03 (Kothes et al 2006b). A possible spectral break at a low frequency below 1 GHz was noted by Mantovani et al (1985) and Castelletti et al (2003).…”

Section: G690+27 (Ctb 80)mentioning

confidence: 99%

“…This value is consistent with those quoted by Landecker et al (1990) and Tian & Leahy (2006b) from the CGPS, which used the Effelsberg λ21 cm survey for missing zero-spacings. Using these flux densities together with the flux densities at 408 MHz Kothes et al 2006b;Tian & Leahy 2006b) and other bands (see references in Table 1), we obtained a radio spectral index of α = −0.45 ± 0.04 (see Fig. 2).…”

Section: G397−20 (W50)mentioning

confidence: 99%

“…(1) Downes et al (1981), (2) Downes et al (1986), (3) Dubner et al (1998), (4) Kovalenko et al (1994), (5) Landecker et al (1990), (6) Kothes et al (2006b), (7) Tian & Leahy (2006b), (8) Castelletti et al (2003), (9) Mantovani et al (1985), (10) Velusamy et al (1976), (11) Wendker et al (1991), (12) Higgs et al (1977), (13) Pineault & Chastenay (1990), (14) Zhang et al (1997), (15) Higgs et al (1991), (16) Reich et al (2003), (17) Hirabayashi & Takahashi (1972), (18) Willis (1973), (19) …”

Section: G397−20 (W50)mentioning

confidence: 99%

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A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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Context.Observations of large supernova remnants (SNRs) at high frequencies are rare, but provide valuable information about their physical properties. Aims. The total intensity and polarization properties of 16 large SNRs in the Galactic plane are investigated based on observations of the Urumqi λ6 cm polarization survey of the Galactic plane with an angular resolution of 9. 5. Methods. We extracted total intensity and linear polarization maps of large SNRs from the Urumqi λ6 cm survey, obtained their integrated flux densities, and derived the radio spectra by using these flux densities together with previously published flux densities at various frequencies. In particular, Effelsberg λ11 cm and λ21 cm survey data were used to calculate integrated flux densities. The λ6 cm polarization data also delineate the magnetic field structures of the SNRs. Results. We present the first total intensity maps at λ6 cm for SNRs G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06) and the first polarization measurements at λ6 cm for SNRs G82.2+5.3 (W63), G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06). Most of the newly derived integrated radio spectra are consistent with previous results. The new flux densities obtained from the Urumqi λ6 cm, Effelsberg λ11 cm and λ21 cm surveys are crucial to determine the spectra of SNR G65.1+0.6, G69.0+2.7 (CTB 80), G93.7−0.2, and G114.3+0.3. We find that G192.8−1.1 (PKS 0607+17) consists of background sources, H ii regions, and extended diffuse emission of thermal nature, and conclude that G192.8−1.1 is not a SNR.

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Section: G690+27 (Ctb 80)mentioning

confidence: 91%

Section: G690+27 (Ctb 80)mentioning

confidence: 99%

Section: G397−20 (W50)mentioning

confidence: 99%

Section: G397−20 (W50)mentioning

confidence: 99%

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A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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“…in gamma-rays (Abdo et al 2010), X-ray (Pannuti et al 2014), the infrared (Reach et al 2006) or in submillimeter (van Dishoeck et al 1993). Catalogues of remnants visible in the radio waveband in the northern and southern hemisphere are available in Kothes et al (2006) and Whiteoak & Green (1996), respectively. An exhaustive catalogue of the known Galactic supernova remnants was compiled by Green (2009).…”

Section: Introductionmentioning

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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γCygni SNR morphology viewed in the electromagnetic spectrum

Sinitsyna,

Balygin

et al. 2024

Astron Nachr

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The investigation of very high energy gamma‐ray sources touches on the problem of the cosmic ray origin and the role of the Galaxy in their generation. The SHALON observations have yielded the results on Cygni SNR Galactic supernova remnant. The observation results are presented with spectral energy distribution and emission map by SHALON in comparison with other experiment data obtained by ROSAT in x‐ray energy range, radio‐data by CGPS, and also observations of GeV–TeV gamma‐rays by Fermi LAT. The overall Cygni SNR characteristics detected in radio, x‐rays, and GeV–TeV gamma‐rays can be a result of the shocks at the interaction of the supernova ejecta and the surrounding medium. The collected experimental data help to make clear the origin of TeV ‐ray emission in the Cygni SNR. The density of target material in the SNR surroundings is enough to produce the observable TeV gamma‐ray flux via the shock acceleration of hadrons in the detected regions. The detection of gamma‐ray emission at 0.8–60 TeV from the North‐West and South‐East shells of Cygni SNR by SHALON would favor the hadronic origin of the gamma‐rays in this supernova remnant.

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A catalogue of Galactic supernova remnants from the Canadian Galactic plane survey

Cited by 153 publications

References 47 publications

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Asymmetric supernova remnants generated by Galactic, massive runaway stars

γCygni SNR morphology viewed in the electromagnetic spectrum

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