A High-Resolution Radio Study of the W50–SS 433 System and the Surrounding Medium

Dubner, G.; Holdaway, M. A.; Goss, W. M.; Mirabel, I. F.

doi:10.1086/300537

Cited by 225 publications

(341 citation statements)

References 30 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: 89%

“…(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)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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“…Dwek (2004) attributes this law to the presence of relatively short metallic needles in the interstellar medium that could form in the supernova ejecta and in quiescent O-rich stellar outflow. SS 433 may have undergone a supernova explosion to form its compact object, as it is surrounded by the W50 radio nebula (Dubner et al 1998), which is possibly a supernova remnant. Thus the Lutz law is likely to be valid in the case of SS 433, so we used it in this study.…”

Section: Dereddeningmentioning

confidence: 99%

SS 433: a phenomenon imitating a Wolf-Rayet star

Fuchs

Miramond

Ábrahám

2006

A&A

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We present mid-infrared (2-12 µm) spectra of the microquasar SS 433 obtained with the Infrared Space Observatory (spectroscopic mode of ISOPHOT and ISOCAM). We compare them to the spectra of four Wolf-Rayet stars: WR 78, WR 134, WR 136, and WR 147 in the same wavelength range. The mid-infrared spectrum of SS 433 mainly shows H i and He i emission lines and is very similar to the spectrum of WR 147, a WN8(h)+B0.5V binary. The 2-12 µm continuum emission of SS 433 corresponds to optically thin and partially optically thick free-free emission, from which we calculate a mass loss rate of 2−3 × 10 −4 M yr −1 if the wind is homogeneous and a third of these values if it is clumped. This is consistent with a strong stellar wind from a WN star. However, following recent studies concluding that the mass donor star of SS 433 is not a Wolf-Rayet star, we propose that this strong wind out flows from a geometrically thick envelope of material that surrounds the compact object like a stellar atmosphere, imitating the Wolf-Rayet phenomenon. This wind could also wrap the mass donor star, and at larger distances (∼40 AU), it might form a dust envelope from which the thermal emission, detected with ISOPHOT at 25 µm and 60 µm, would originate. This wind also probably feeds the material that is ejected in the orbital plane of the binary system and that forms the equatorial outflow detected in radio at distances > 100 AU.

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“…Non-thermal emission from these regions has indeed been observed from radio to Xray energies (Brinkmann et al 1996, Dubner et al 1998Safi-Harb & Ögelman 1997;Safi-Harb & Petre 1999;Fuchs 2002;Brinkmann et al 2007.…”

Section: Gamma-ray Emission and Absorption Processes In Ss 433/w50mentioning

confidence: 96%

“…SS 433 is extremely bright with a bolometric luminosity of L bol ∼ 10 40 erg s −1 (Cherepashchuk 2002) peaking at ultraviolet wavelengths. The source displays the most powerful jets known in our Galaxy, with L jet 10 39 erg s −1 (Dubner et al 1998;Margon 1984;Marshall et al 2002), ejected at a relativistic velocity of 0.26 c (Margon & Anderson 1989). The jets show a precessional period of ∼162.4 days with a half opening angle of θ pre ≈ 21 • with respect to the normal to the orbital plane, with precessional phase Ψ pre = 0 defined as the phase with the maximum exposure of the accretion disk to the observer (Fabrika 1993).…”

Section: The Ss 433/w50 Systemmentioning

confidence: 98%

Constraints on particle acceleration in SS433/W50 from MAGIC and H.E.S.S. observations

Ahnen¹,

Ansoldi²,

Antonelli³

et al. 2018

A&A

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Context. The large jet kinetic power and non-thermal processes occurring in the microquasar SS 433 make this source a good candidate for a very high-energy (VHE) gamma-ray emitter. Gamma-ray fluxes above the sensitivity limits of current Cherenkov telescopes have been predicted for both the central X-ray binary system and the interaction regions of SS 433 jets with the surrounding W50 nebula. Non-thermal emission at lower energies has been previously reported, indicating that efficient particle acceleration is taking place in the system.Aim. We explore the capability of SS 433 to emit VHE gamma rays during periods in which the expected flux attenuation due to periodic eclipses (Porb~ 13.1 days) and precession of the circumstellar disk (Ppre ~ 162 days) periodically covering the central binary system is expected to be at its minimum. The eastern and western SS 433/W50 interaction regions are also examined using the whole data set available. We aim to constrain some theoretical models previously developed for this system with our observations.Methods. We made use of dedicated observations from the Major Atmospheric Gamma Imaging Cherenkov telescopes (MAGIC) and High Energy Spectroscopic System (H.E.S.S.) of SS 433 taken from 2006 to 2011. These observation were combined for the first time and accounted for a total effective observation time of 16.5 h, which were scheduled considering the expected phases of minimum absorption of the putative VHE emission. Gamma-ray attenuation does not affect the jet/medium interaction regions. In this case, the analysis of a larger data set amounting to ~40–80 h, depending on the region, was employed.Results. No evidence of VHE gamma-ray emission either from the central binary system or from the eastern/western interaction regions was found. Upper limits were computed for the combined data set. Differential fluxes from the central system are found to be ≲ 10−12–10−13 TeV−1 cm−2 s−1 in an energy interval ranging from ~few × 100 GeV to ~few TeV. Integral flux limits down to ~ 10−12–10−13 ph cm−2 s−1 and ~ 10−13–10−14 ph cm−2 s−1 are obtainedat 300 and 800 GeV, respectively. Our results are used to place constraints on the particle acceleration fraction at the inner jetregions and on the physics of the jet/medium interactions.Conclusions. Our findings suggest that the fraction of the jet kinetic power that is transferred to relativistic protons must be relatively small in SS 433, qp ≤ 2.5 × 10−5, to explain the lack of TeV and neutrino emission from the central system. At the SS 433/W50 interface, the presence of magnetic fields ≳10 μG is derived assuming a synchrotron origin for the observed X-ray emission. This also implies the presence of high-energy electrons with Ee− up to 50 TeV, preventing an efficient production of gamma-ray fluxes in these interaction regions.

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A High-Resolution Radio Study of the W50–SS 433 System and the Surrounding Medium

Cited by 225 publications

References 30 publications

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A Sino-Germanλ6 cm polarization survey of the Galactic plane

SS 433: a phenomenon imitating a Wolf-Rayet star

Constraints on particle acceleration in SS433/W50 from MAGIC and H.E.S.S. observations

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