English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The distance to the relativistic jet source SS 433 and the related supernova remnant W50 is re‐examined using new observations of H  i  in absorption from the Very Large Array, H  i  in emission from the Green Bank Telescope, and  12 CO emission from the Five College Radio Astronomy Observatory. The new measurements show H  i  in absorption against SS 433 to a velocity of 75 km s −1  but not to the velocity of the tangent point, which bounds the kinematic distance at  5.5 ≤ d  k  &lt; 6.5 kpc . This is entirely consistent with a  5.5 ± 0.2 kpc  distance determined from light traveltime arguments by Blundell &amp; Bowler. The H  i  emission map shows evidence of interaction of the lobes of W50 with the interstellar medium near the adopted systemic velocity of   V  LSR = 75 km s −1  . The western lobe sits in a cavity in the H  i  emission near the Galactic plane, while the eastern lobe terminates at an expanding H  i  shell. The expanding shell has a radius of 40 pc, contains  8 ± 3 × 10 3  M ⊙   of H  i  and has a measured kinetic energy of  3 ± 1.5 × 10 49  erg . There may also be a static H  i  ring or shell around the main part of W50 itself at a local standard of rest (LSR) velocity of 75 km s −1 , with a radius of 70 pc and a mass in H  i  of  3.5−10 × 10 4  M ⊙  . We do not find convincing evidence for the interaction of the system with any molecular cloud or with H  i  at other velocities. The H  i  emission data suggest that SS 433 lies in an interstellar environment substantially denser than average for its distance from the Galactic plane.  This Population I system, now about 200 pc below the Galactic plane, most likely originated as a runaway O‐star binary ejected from a young cluster in the plane. Given a modest ejection velocity of  ≥30 km s −1  , the binary could have reached its present location in ≤10 Myr at which time the more massive member became a supernova (SN). New astrometric data on SS 433 show that the system now has a peculiar velocity of a few tens of km s −1  in the direction of the Galactic plane. From this peculiar velocity and the symmetry of the W50 remnant, we derive a time since the SN of  ≤1 × 10 5  yr .

The distance to SS 433/W50 and its interaction with the interstellar medium