The Large-scale ISM of SS433/W50 Revisited

Abstract

With new high-resolution CO and HI 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 ~7deg. The kinematic features of the two MCs at ~73--84 km/s, 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 HI emission at VLSR~70--90 km/s displays the morphological resemblance with the radio nebula W50. We suggest that the VLSR=77\pm5 km/s gas is physically associated with SS 433/W50, leading to a near kinematic distance of 4.9\pm0.4 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 ~2x10^6 K cm-3.

1 table, 13 figures, to appear in the ApJ. Comments welcome

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Cited by in corpus (18)

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• Molecular gas distribution perpendicular to the Galactic plane
• Gamma-ray heartbeat powered by the microquasar SS 433
• Deciphering the Origin of the GeV--TeV Gamma-ray Emission from SS 433
• Local Molecular Gas toward the Aquila Rift Region
• A Small-Scale Investigation of Molecular Emission toward the Tip of the Western Lobe of W50/SS433
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• Energy estimation of high energy particles associated with the SS433/W50 system through radio observation at 1.4 GHz
• Molecular clouds at the eastern edge of radio nebula W50
• A Cold and Diffuse Giant Molecular Filament in the Region of $l=41^{\circ }$, $b=-1^{\circ }$
• Physical properties of the molecular cloud, N4, in SS433; Evidence for an interaction of molecular cloud with the jet from SS433
• CO Emission Delineating the Interface between the Milky Way Nuclear Wind Cavity and the Gaseous Disk
• Large-field CO (J=1-0) observations toward SNR G150.3+4.5
• Near-Ultraviolet Radiation toward Molecular Cloud N4 in W 50/SS 433: Evidence for Direct Interaction of the Jet with Molecular Cloud
• Investigation of the Microquasar SS 433 with VERITAS
• Discovery of CO Clouds Associated with the X-ray Jets of SS 433: Evidence for Shock-Cloud Interaction Enhancing Nonthermal X-ray Emission