2700 MHz Polarization Observations of 17 Supernova Remnants

Milne, D. K.; Dickel, J.R.

doi:10.1071/ph740549

Cited by 18 publications

(25 citation statements)

References 3 publications

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“…G192.8−1.1 is not a SNR G192.8−1.1 (PKS 0607+17) has been proposed as a SNR with an angular extent of about 80 (Milne & Hill 1969;Caswell 1970). The non-thermal spectral index derived was α ∼ −0.5 (Milne & Dickel 1974;Dickel & Denoyer 1975). Berkhuijsen (1974) suggested that G192.8−1.1 is a small part of an even larger SNR, which she called the "Origem Loop" with a diameter of about 5 • , but later Caswell (1985) performed high angular resolution (∼1 ) observations at λ21 cm using the DRAO synthesis telescopes and argued again that G192.8−1.1 is a discrete SNR with a radio spectral index of α ∼ −0.55.…”

Section: Resultsmentioning

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: Resultsmentioning

confidence: 99%

“…Therefore, it was difficult to determine the boundary of the SNR, and reliable integrated flux densities could not be obtained. Early λ11 cm polarization observations were made by Milne & Dickel (1974), but no significant polarized emission was detected.…”

Section: G2055+05 (Monoceros Nebula)mentioning

confidence: 99%

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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“…Observations at frequencies near 2700 MHz were made by Day et al (1972); Milne & Dickel (1974); Velusamy & Kundu (1974); Graham et al (1982). Graham et al (1982) found an average spectral index α = −0.47 ± 0.06 from 111−2700 MHz radio data.…”

Section: Introductionmentioning

confidence: 99%

“…Combining this observation with Effelsberg 21 cm and 11 cm data, they obtained a spectral index of α = −0.43 ± 0.12 for the western shell. Early 11 cm polarization observations were made by Milne & Dickel (1974), but no significant polarized emission was detected. The 6 cm polarization map showed that the magnetic field is closely aligned with the filamentary shell.…”

Section: Introductionmentioning

confidence: 99%

Radio perspectives on the Monoceros SNR G205.5+0.5

Xiao

Zhu

2012

A&A

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Context. The Monoceros supernova remnant (SNR G205.5+0.5) is a large shell-type SNR located in the Rosette molecular complex and thought to be interacting with the Rosette Nebula. Aims. We aim to re-examine the radio spectral index and its spatial variation over the Monoceros SNR as well as study its properties of evolution within the complex interstellar medium. Methods. We extracted radio continuum data for the Monoceros complex region from the Effelsberg 21 cm and 11 cm surveys and the Urumqi 6 cm polarization survey. We used the new Arecibo GALFA-HI survey data with much higher resolution and sensitivity than that previously available to identify the HI shell related with the SNR. Multi-wavelengths data are included to investigate the properties of the SNR. Results. The spectral index α (S ν ∝ ν α ) averaged over the SNR is −0.41 ± 0.16. The TT-plots and the distribution of α over the SNR show spatial variations that steepen toward the inner western filamentary shell. Polarized emission is prominent on the western filamentary shell region. The RM there is estimated to be about 30 ± 77n rad m −2 , where the n = 1 solution is preferred, and the magnetic field has a strength of about 9.5 μG. From the HI channel maps, further evidence is provided for an interaction between the Monoceros SNR and the Rosette Nebula. We identify partial neutral hydrogen shell structures in the northwestern region at velocities of +15 km s −1 circumscribing the continuum emission. The HI shell has swept up a mass of about 4000 M for a distance of 1.6 kpc. The western HI shell, well associated with the dust emission, is found to lie outside of the radio shell. We suggest that the Monoceros SNR is evolving within a cavity blown out by the progenitor and has triggered part of the star formation in the Rosette Nebula. Conclusions. The Monoceros SNR is interacting with the ambient interstellar medium with ultra-high energy emission detected. Its interaction with the Rosette Nebula is further supported by new evidence from HI data, which will help the investigation of the emission mechanism of the high-energy emission.

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“…It has been considered to be a supernova remnant (SNR) by several researchers (e.g., Caswell 1970;Day et al 1972;Milne & Dickel 1974;Dickel & Denoyer 1975) due to its non-thermal radio spectral index. Berkhuijsen (1974) has also proposed that it is a part of the Origem Loop, a large, 5 ¥ -sized continuum shell, rather than an individual SNR.…”

Section: Introductionmentioning

confidence: 99%