Radio observations of W50 and the surrounding area

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

doi:10.1016/0083-6656(81)90046-5

Cited by 30 publications

(61 citation statements)

References 2 publications

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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: 79%

“…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: 79%

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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“…Yang et al (2006) investigated the distribution of molecular gas around the SNR direction through the 12 CO (J = 1-0) transition line, and provided evidence for interaction between the SNR and its neighboring dense ISM at a central velocity V LSR = 55 km s −1 . The corresponding kinematic distance of 3-3.4 kpc implied a source diameter of 25 pc and a younger age, at variance with the initial estimates of Downes et al (1980). The association of the HESS source to this SNR is not straightforward due to the fact that the angular size (>40 FWHM) of the VHE source is significantly larger than the 26 size of the shell.…”

Section: Search For Counterpartsmentioning

confidence: 91%

“…Downes et al (1980), using various Σ−D relations derived a linear diameter of 40-65 pc, an age of (2-4) ×10 4 yr, and estimated the distance to the SNR to be in the range 5.5 to 8.5 kpc, corresponding to a location either in the inter-arm region between the Scutum and the Sagittarius arms, or on the inner edge of the latter. Yang et al (2006) investigated the distribution of molecular gas around the SNR direction through the 12 CO (J = 1-0) transition line, and provided evidence for interaction between the SNR and its neighboring dense ISM at a central velocity V LSR = 55 km s −1 .…”

Section: Search For Counterpartsmentioning

confidence: 99%

Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06

Aharonian

Akhperjanian

Anton

et al. 2009

A&A

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Aims. Detection of a γ-ray source above 300 GeV is reported, confirming the unidentified source MGRO J1908+06, discovered by the Milagro collaboration at a median energy of 20 TeV. Methods. The source was observed during 27 h as part of the extension of the HESS Galactic plane survey to longitudes >30• . Results. HESS J1908+063 is detected at a significance level of 10.9σ with an integral flux above 1 TeV of (3.76 ± 0.29 stat ± 0.75 sys ) × 10 −12 ph cm −2 s −1 , and a spectral photon index Γ = 2.10 ± 0.07 stat ± 0.2 sys . The positions and fluxes of HESS J1908+063 and MGRO J1908+06 are in good agreement. Possible counterparts at other wavelengths and the origin of the γ-ray emission are discussed. The nearby unidentified GeV source, GRO J1908+0556 (GeV) which also remains unidentified and the new Fermi pulsar 0FGL J1907.5+0617, may be connected to the TeV source.

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Search for VHE gamma rays from SS433/W50 with the CANGAROO-II telescope

Hayashi

Kajino

Naito

et al. 2009

Astroparticle Physics

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SS433, located at the center of the supernova remnant W50, is a close proximity binary system consisting of a compact star and a normal star. Jets of material are directed outwards from the vicinity of the compact star symmetrically to the east and west. Non-thermal hard X-ray emission is detected from lobes lying on both sides. Shock accelerated electrons are expected to generate sub-TeV gamma rays through the inverse-Compton process in the lobes. Observations of the western X-ray lobe region of SS433/W50 system have been performed to detect sub-TeV gamma-rays using the 10m CANGAROO-II telescope in August and September, 2001, and July and September, 2002. The total observation times are 85.2 hours for ON source, and 80.8 hours for OFF source data. No significant excess of sub-TeV gamma rays has been found at 3 regions of the western X-ray lobe of SS433/W50 system. We have derived 99% confidence level upper limits to the fluxes of gamma rays and have set constraints on the strengths of the magnetic fields assuming the synchrotron/inverse-Compton model for the wide energy range of photon spectrum from radio to TeV. The derived lower limits are 4.3 microgauss for the center of the brightest X-ray emission region and 6.3 microgauss for the far end from SS433 in the western X-ray lobe. In addition, we suggest that the spot-like X-ray emission may provide a major contribution to the hardest X-ray spectrum in the lobe.Comment: 7 pages, 8 figures, to be published in Astroparticle Physic

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Radio observations of W50 and the surrounding area

Cited by 30 publications

References 2 publications

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06

Search for VHE gamma rays from SS433/W50 with the CANGAROO-II telescope

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