LOFAR 150-MHz observations of SS 433 and W 50

Broderick, J. W.; Fender, R. P.; Miller-Jones, J. C. A.; Трушкин, С. А.; Stewart, A.; Anderson, G.; Staley, T. D.; Blundell, Katherine M.; Pietka, M.; Markoff, Sera; Rowlinson, A.; Swinbank, J.; Horst, A. J. van der; Bell, M. E.; Breton, R. P.; Carbone, D.; Corbel, S.; Eislöffel, J.; Falcke, H.; Grießmeier, J.-M.; Hessels, J. W. T.; Kondratiev, V. I.; Law, Casey J.; Molenaar, Gijs; Serylak, M.; Stappers, B. W.; Leeuwen, J. van; Wijers, R. A. M. J.; Wijnands, Rudy; Wise, Michael; Zarka, Philippe

doi:10.1093/mnras/sty081

Cited by 26 publications

(26 citation statements)

References 118 publications

(145 reference statements)

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“…2. LOFAR images at approximately 150 MHz have recently been published (Broderick et al 2018) and in Fig. 1 of that paper W50 is displayed on a smaller scale, revealing its Galactic context.…”

Section: W 50mentioning

confidence: 95%

W 50 and SS 433

Bowler

Keppens

2018

A&A

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Context. The Galactic microquasar SS 433 launches oppositely-directed jets at speeds approximately a quarter of the speed of light. These appear to have punched through and beyond the supposed supernova remnant shell W 50. The problems with this interpretation are: (i) The precessing jets have somehow been collimated before reaching the shell; (ii) Without deceleration, only recently launched jets would have reached no further; and (iii) Certain features in the lobes are moving slowly or are stationary.Aims. Hydrodynamic computations have demonstrated that for at least one set of parameters describing the ambient medium, jets that diverge and precess are both decelerated and collimated; the conformation of W 50 could then have been sculpted by the jets of SS 433. However, the parameters adopted for density and pressure in these computations are not consistent with observations of jets at a few years old; nor do they represent conditions within a supernova remnant. Our aim is to investigate whether the computations already performed can be scaled to a realistic W 50. Methods. We find simple and physically based scaling relations. The distance to collimation varies inversely with the square root of the pressure of the ambient medium and the speed with which the head of a collimated jet propagates scales with the square root of the temperature. We extrapolate the results of the hydrodynamic computations to lower densities and pressures.Results. The jets of SS 433, launched into an ambient medium of pressure ∼ 10 −9 erg cm −3 and temperature ∼ 10 8 K, within a supernova remnant, could be responsible for the characteristics of W 50. The precessing jets are collimated within ∼ 10 pc and the head of the resulting cylindrical jet propagates slowly.Conclusions. The problems of relating W 50 to SS 433 may now be solved.

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Section: W 50mentioning

confidence: 95%

W 50 and SS 433

Bowler

Keppens

2018

A&A

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“…The termination region (e3) is prominent in radio images and well-correlated with X-ray intensity maps. However, the knots, e1, e2, and w1, are not resolved in the 2.7 GHz map by the Effelsberg telescope (Geldzahler et al 1980) nor in the recent 150 MHz map by LOFAR (Broderick et al 2018). This suggests that the contribution from X-ray knots to the observed radio intensity may be sub-dominant, and the radio fluxes should be treated as upper limits.…”

Section: Multi-wavelength Observations Toward X-ray Knotsmentioning

confidence: 98%

Multiwavelength Emission from Galactic Jets: The Case of the Microquasar SS433

Sudoh

Inoue

Khangulyan

2020

ApJ

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SS433 is a Galactic microquasar with powerful jets, where very-high-energy particles are produced. We study particle acceleration in the jets of SS433 in the light of the recent multi-wavelength data from radio to TeV gamma ray. We first present a general framework for the particle acceleration, cooling, and transport in relativistic jets. We then apply this to two X-ray knots in the jets of SS433, focusing on leptonic emission. Our detailed treatment of particle transport and evolution produces substantially different predictions from previous papers. For both regions, our model can account for the multi-wavelength data except for the GeV data. This suggests that GeV emission is mostly from different regions and/or mechanisms. We find that the acceleration process should be efficient, which could be realized by diffusive shock acceleration close to the Bohm limit. Provided that protons are accelerated at the same efficiency as electrons, our results imply that SS433 is a PeVatron, i.e., can accelerate protons beyond a PeV. Future hard X-ray and MeV gamma-ray observations can critically test our models by detecting the spectral turnover or cutoff.

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“…(b) This clump is anti-correlated with the radio continuum, appearing embedded in a void of radio emission (Figure 2 and 3), which is more clearly shown in the upper left panel of Figure 4. The clump is also anticorrelated to the radio continuum at 327.5 MHz (Dubner et al 1998) and at 150 MHz (Broderick et al 2018). It will be shown in § 4.1 that the clump is not likely located in the fore-ground and causing the low radio brightness in region N3 by extinction.…”

Section: Spatial Distribution Of the Cloudsmentioning

confidence: 88%

A Small-scale Investigation of Molecular Emission toward the Tip of the Western Lobe of W50/SS 433

Liu

Chen

Zhou

et al. 2020

ApJ

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We perform a molecular (CO and CN) line observation using the IRAM 30m telescope toward two small regions near the western edge of supernova remnant (SNR) W50/SS 433. CO observation reveals spatial correspondence of two molecular clumps at the local-standard-of-rest (LSR) velocity around +53 km s −1 , with multiwavelength local features of the W50/SS 433 system. One of the two clumps appears to be embedded in a void of diffuse radio and X-ray emission. Toward the two clumps, asymmetric broad-line profiles of the 12 CO lines are obtained, which provide kinematic evidence of the association between the clumps and the jet-related gas. The 12 CO J= 2-1/J= 1-0 line ratios ( 0.9) and the kinetic temperatures (∼ 30 K) of the clumps are distinctively higher than all those of the clumps at other LSR velocities along the same line of sight, which may be physical signatures of the association. We show that the clump coincident with the void can survive the thermal heating if it is surrounded by hot gas, with an evaporation timescale much larger than the age of SNR W50. We also show that the thermal equilibrium in the high-temperature clumps can be maintained by the heating of the penetrating environmental cosmic rays. CN (J = 3/1-1/2) line emission is detected in the two clumps, and the CN abundances derived are much higher than that in the interstellar molecular clouds (MCs) and that in the SNR-interacting MCs.

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LOFAR 150-MHz observations of SS 433 and W 50

Cited by 26 publications

References 118 publications

W 50 and SS 433

W 50 and SS 433

Multiwavelength Emission from Galactic Jets: The Case of the Microquasar SS433

A Small-scale Investigation of Molecular Emission toward the Tip of the Western Lobe of W50/SS 433

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