Molecular clouds at the eastern edge of radio nebula W50

Abstract

Microquasar SS 433 located at the geometric center of radio nebula W50 is a suitable source for investigating the physical process of how galactic jets affect the surrounding interstellar medium (ISM). Previous studies have searched for evidence of the interaction between the SS 433 jet and ISM, such as neutral hydrogen gas and molecular clouds; however, it is still unclear which ISM interacts with the jet. We looked for new molecular clouds that possibly interact at the terminal of the SS 433 eastern jet using the Nobeyama 45-m telescope and the Atacama Submillimeter Telescope Experiment (ASTE). We identified two molecular clouds, comprising many small clumps, in the velocity range of 30.1--36.5 km s${}^{-1}$ for the first time. These clouds have complex velocity structures, and one of them has a density gradient toward SS 433. Although it is difficult to conclude the relation between the molecular clouds and the SS 433/W50 system, there is a possibility that the eastern structure of W50 constructed by the SS 433 jet swept up tiny molecular clumps drifting in the surroundings and formed the molecular clouds that we identified in this study.

22 pages, 11 figures, accepted for publication in PASJ

References in corpus (12)

• The relation between gas and dust in the Taurus Molecular Cloud
• The Distance to SS433/W50 and its Interaction with the ISM
• High-energy Cosmic Ray production in X-ray Binary Jets
• Mapping Jet-ISM Interactions in X-ray Binaries with ALMA: A GRS 1915$+$105 Case Study
• Blazing trails: Microquasars as head-tail sources and the seeding of magnetized plasma into the ISM
• Jet-ISM Interactions near the Microquasars GRS 1758-258 and 1E 1740.7-2942
• Continuous Jets and Backflow Models for the Formation of W50/SS433 in Magnetohydrodynamics Simulations
• Magneto-hydrodynamic Simulations of a Jet Drilling an HI Cloud: Shock Induced Formation of Molecular Clouds and Jet Breakup
• Energy estimation of high energy particles associated with the SS433/W50 system through radio observation at 1.4 GHz
• 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
• Magnetohydrodynamic Simulations of the Formation of Molecular Clouds toward the Stellar Cluster Westerlund 2: Interaction of a Jet with Clumpy Interstellar Medium

Cited by in corpus (6)

• Microquasar jet-cocoon systems as PeVatrons
• Spectral and photometric variability of SS 433 observed with XRISM and simultaneous optical and near-infrared telescopes
• Arcsecond-Scale X-ray Imaging and Spectroscopy of SS 433 with Chandra HETG
• Detection of molecular clouds in the PeVatron candidate source LHAASO J0341$+$5258 by the Nobeyama 45-m radio telescope
• Near-Ultraviolet Radiation toward Molecular Cloud N4 in W 50/SS 433: Evidence for Direct Interaction of the Jet with Molecular Cloud
• Discovery of CO Clouds Associated with the X-ray Jets of SS 433: Evidence for Shock-Cloud Interaction Enhancing Nonthermal X-ray Emission