The supernova remnant W50 at 5 GHz

Downes, A. J. B.; Pauls, T.; Salter, C. J.

doi:10.1093/mnras/218.3.393

Cited by 40 publications

(56 citation statements)

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“…We obtained integrated flux densities of S 6 cm = 37.0 ± 3.8 Jy from the Urumqi survey data, S 11 cm = 51.5 ± 5.2 Jy and S 21 cm = 69.7 ± 7.1 Jy from the Effelsberg λ11 cm and λ21 cm survey data. All of these agree with the values obtained by Downes et al (1981Downes et al ( , 1986 and Dubner et al (1998). Using these flux densities together with Table 1.…”

Section: G397−20 (W50)supporting

confidence: 89%

“…The TT-plot using the Urumqi λ6 cm and Effelsberg λ11 cm survey data gave β = −2.41 ± 0.01 for the central part, β = −2.52 ± 0.02 for the southeast "ear", and β = −2.57 ± 0.14 for the northwest "ear", respectively. The central part appears to have a slightly flatter spectrum than the southeast "ear", confirming the finding of Downes et al (1986).…”

Section: G397−20 (W50)supporting

confidence: 80%

“…Jowett & Spencer (1995) mapped SS 443 at 5 GHz with the MERLIN array and detected ejected radio blobs moving away from SS 443. Downes et al (1981) and Downes et al (1986) observed the total intensity and the polarized emission of W50 at λ18 cm, λ11 cm, and λ6 cm with the 100-m Effelsberg radio telescope. The spectral index and RM distributions of this SNR were studied in detail.…”

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: G397−20 (W50)supporting

confidence: 89%

Section: G397−20 (W50)supporting

confidence: 80%

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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“…It is the only knot from which radio emission has been detected-83 ± 9 mjy at 2.695 GHz (Geldzahler et al 1980) and 70 ± 4 mjy at 4.75 GHz (Downes et al 1986)-and in contrast to large regions of W50, it is unpolarized (Downes et al 1986). The flat radio spectrum and absence of polarization suggest a thermal origin.…”

Section: The Knotsmentioning

confidence: 99%

IRAS observations of SS 433 and W50

Band

1987

PASP

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IRAS observations show SS 433 to be a weak but detectable infrared source at 12 |x and 25 |x. The mid-infrared flux is consistent with a continuation of the spectrum at higher frequencies, although the spectrum flattens at low frequency. The resulting spectrum can be explained as the sum of a constant blackbody component and a variable optically thin free-free emission component. No variability is apparent; however, the timing of the observations does not preclude greater intrinsic variability than was observed. The surrounding W50 radio source is not apparent in the infrared, although there is a plateau of infrared emission to the north-northwest that includes the H II region S74. A number of knots with steep spectra can be identified which emit on the order of 10 37 ergs sec 1 if they are at the distance of SS 433. In particular, three infrared knots lie on the jet axis within W50 and two of these three knots bracket the western optical filament. No Ha emission was detected from the western knots. The optical filaments have no obvious infrared emission.

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X-ray lobes of W 50/SS 433 system

et al. 1999

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The X‐ray lobes lie on both sides (east and west) of SS 433, and are presumably produced by the interaction of the jets of SS 433 with the surrounding SNR W 50. The non‐thermal nature of the east lobe has been reported by Yamauchi et al. (1994) using ASCA data. With the further ASCA observations, we studied the spectra and morphology of both the east and west lobes in detail. Their spectra have no emission lines, and are well described by power‐law models with interstellar absorption. The X‐ray emission becomes softer on both sides with increasing distance from SS 433. The X‐ray surface brightness peaks closer to SS 433 in the high‐energy band than in the low energy band, suggesting that the high energy electrons in the X‐ray lobes lose energies by synchrotron emission as the travel away from SS 433. We estimate the magnetic field and the total energy of the high energy electrons to be ∼2 μG and ∼5 × 1046 erg, respectively.

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The supernova remnant W50 at 5 GHz

Cited by 40 publications

References 0 publications

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A Sino-Germanλ6 cm polarization survey of the Galactic plane

IRAS observations of SS 433 and W50

X-ray lobes of W 50/SS 433 system

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