Interacting large-scale magnetic fields and ionized gas in the W50/SS433 system

Farnes, J. S.; Gaensler, B. M.; Purcell, Cormac; Sun, Xiaohui; Haverkorn, M.; Lenc, E.; O’Sullivan, S. P.; Akahori, Takuya

doi:10.1093/mnras/stx338

Cited by 34 publications

(55 citation statements)

References 105 publications

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“…The previous jet episodes (or possible intermittent jet activities, e.g. Goodall et al 2011a,b), the winds from the system (e.g., Begelman et al 1980;Konigl 1983;Fabrika 2004;Begelman et al 2006;Panferov 2017), and the loop magnetic field on the large scale (Farnes et al 2017) may play significant roles in the formation of the SS 433/W50's current configuration.…”

Section: The Fossil Record Of Jet-ism Interactionsmentioning

confidence: 99%

The Large-scale Interstellar Medium of SS 433/W50 Revisited

Zhou

Yang

et al. 2018

ApJ

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With new high-resolution CO and H i data, we revisited the large-scale interstellar medium (ISM) environment toward the SS 433/W50 system. We find that two interesting molecular cloud (MC) concentrations, G39.315−1.155 and G40.331−4.302, are well aligned along the precession cone of SS 433 within a smaller opening angle of ∼ ±7 • . The kinematic features of the two MCs at ∼73-84 km s −1 , as well as those of the corresponding atomic-gas counterparts, are consistent with the kinematic characteristics of SS 433. That is, the receding gas from SS 433 jet is probably responsible for the redshifted feature of G39.315−1.155 near the Galactic plane and the approaching one may power the blueshifted gas of G40.331−4.302 toward the observer. Moreover, the H i emission at V LSR ∼70-90 km s −1 displays the morphological resemblance with the radio nebula W50. We suggest that the V LSR =77±5 km s −1 gas is physically associated with SS 433/W50, leading to a near kinematic distance of 4.9±0.4 kpc for the system. The observed gas features, which are located outside the current radio boundaries of W50, are probably the fossil record of jet-ISM interactions at ∼ 10 5 years ago. The energetic jets of the unique microquasar have profound effects on its ISM environment, which may facilitate the formation of molecular gas on the timescale of < ∼ 0.1 Myr for the ram pressure of ∼ 2 × 10 6 K cm −3 .

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Section: The Fossil Record Of Jet-ism Interactionsmentioning

confidence: 99%

The Large-scale Interstellar Medium of SS 433/W50 Revisited

Zhou

Yang

et al. 2018

ApJ

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“…We here briefly review the observations and the data reduction. See Farnes et al (2017) for further details. The polarization leakage and polarization angle calibration were based upon the techniques developed in Schnitzeler et al (2011) and Anderson et al (2016).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…They also found an irregular distribution of Faraday rotation measure (RM) in W50, albeit only using two frequencies. Recently, Farnes et al (2017) performed full polarization, mosaicked observations of the whole region of W50 by using the Australia Telescope Compact Array (ATCA).…”

Section: Introductionmentioning

confidence: 99%

Magnetic field analysis of the bow and terminal shock of the SS 433 jet

Sakemi

Machida

Akahori

et al. 2018

Publications of the Astronomical Society of Japan

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We report a polarization analysis of the eastern region of W50, observed with the Australia Telescope Compact Array (ATCA) at 1.4 -3.0 GHz. In order to study the physical structures in the region where the SS433 jet and W50 interact, we obtain an intrinsic magnetic field vector map of that region. We find that the orientation of the intrinsic magnetic field vectors are aligned along the total intensity structures, and that there are characteristic, separate structures related to the jet, the bow shock, and the terminal shock. The Faraday rotation measures (RMs), and the results of Faraday Tomography suggest that a high intensity, filamentary structure in the north-south direction of the eastern-edge region can be separated into at least two parts to the north and south. The results of Faraday Tomography also show 1 that there are multiple components along the line of sight and/or within the beam area. In addition, we also analyze the X-ray ring-like structure observed with XMM-Newton. While the possibility still remains that this X-ray ring is "real", it seems that the structure is not ring-like at radio wavelengths. Finally, we suggest that the structure is a part of the helical structure that coils the eastern ear of W50.Key words: magnetic fields1 -polarization2 -ISM : individual (W50)3 -ISM : jets and outflows4stars : individual (SS433)5

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“…A recent paper presents many radio images of the full W 50 field of view and also reveals numerous faint Hα filaments associated with the central region of W 50, suggestive of SNR shock emission (Farnes et al 2017).…”

Section: W 50mentioning

confidence: 99%

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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Interacting large-scale magnetic fields and ionized gas in the W50/SS433 system

Cited by 34 publications

References 105 publications

The Large-scale Interstellar Medium of SS 433/W50 Revisited

The Large-scale Interstellar Medium of SS 433/W50 Revisited

Magnetic field analysis of the bow and terminal shock of the SS 433 jet

W 50 and SS 433

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