A multi-wavelength study of the western lobe of W50 powered by the galactic microquasar SS 433

Moldowan, A.; Safi‐Harb, Samar; Fuchs, Y.; Dubner, G.

doi:10.1016/j.asr.2005.01.086

Cited by 19 publications

(20 citation statements)

References 8 publications

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“…Most of the MCs, which are near the H ii region Sh 2-74 and close to the Galactic plane, also have corresponding bright IR emission. We argue that these MCs with prominent 13 CO emission are probably associated with H ii region Sh 2-74 and/or belong to the nearby MC complex with active star formation (see Section 3.3.3), which agrees with suggestions from previous studies (e.g., Band & Gordon 1989;Moldowan et al 2005).…”

Section: 3supporting

confidence: 91%

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: 3supporting

confidence: 91%

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

Zhou

Yang

et al. 2018

ApJ

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“…This is to be expected for a distance of 5 kpc along the Galactic plane and for a Galactic latitude of only . This possibility is further supported by the ISOCAM (Infrared Space Observatory Camera) infrared emission map of the vicinity of the western filaments obtained by Moldowan et al (2005). One patch of infrared emission coincides closely with the visible western filaments (Figs 3a and b and 5) but a larger region of infrared emission has no optical counterpart in our images.…”

Section: Discussionsupporting

confidence: 81%

Deep optical observations of the interaction of the SS 433 microquasar jet with the W50 radio continuum shell

Boumis¹,

Meaburn²,

Alikakos³

et al. 2007

Monthly Notices of the Royal Astronomical Society

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Four mosaics of deep, continuum‐subtracted, CCD images have been obtained over the extensive Galactic radio continuum shell, W50, which surrounds the remarkable stellar system SS 433. Two of these mosaics in the and [O iii] 5007 Å emission lines, respectively, cover a field of which contains all of W50 but at a low angular resolution of 5 arcsec. The third and fourth mosaics cover the eastern (in [O iii] 5007 Å) and western (in 6548, 6584 Å) filamentary nebulosity, respectively, but at an angular resolution of 1 arcsec. These observations are supplemented by new low‐dispersion spectra and long‐slit, spatially resolved echelle spectra. The [O iii] 5007 Å images show for the first time the distribution of this emission in both the eastern and western filaments while new emission features are also found in both of these regions. Approaching flows of faintly emitting material from the bright eastern filaments of up 100 km s−1 in radial velocity are detected. The present observations also suggest that the heliocentric systemic radial velocity of the whole system is 56 ± 2 km s−1. Furthermore, very deep imagery and high‐resolution spectroscopy of a small part of the northern radio ridge of W50 has revealed for the first time the very faint optical nebulosity associated with this edge. It is suggested that patchy foreground dust along the ≈5 kpc sightline is inhibiting the detection of all of the optical nebulosity associated with W50. The interaction of the microquasar jets of SS 433 with the W50 shell is discussed.

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“…Applying equation (4), the minimum energy (in the comoving frame) required to account for the observed radio emission, under the assumptions made above is 8.1 × 10 46 erg. This value is of the same order of magnitude as the one inferred for the W50 nebula around SS433 (Dubner et al 1998;Moldowan et al 2005). This raises the possibility that Cir X-1 might not be a jet-powered radio nebula only, but maybe a distorted SNR as suggested for W50 (e.g.…”

Section: Application To Cir X-1supporting

confidence: 68%

The large-scale jet-powered radio nebula of Circinus X-1

Tudose

Fender

Kaiser

et al. 2006

Monthly Notices of the Royal Astronomical Society

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We present multi-epoch observations of the radio nebula around the neutron star X-ray binary Circinus X-1 made at 1.4 and 2.5 GHz with the Australia Telescope Compact Array between October 2000 and September 2004. The nebula can be seen as a result of the interaction between the jet from the system and the interstellar medium and it is likely that we are actually looking toward the central X-ray binary system through the jet-powered radio lobe. The study of the nebula thus offers a unique opportunity to estimate for the first time using calorimetry the energetics of a jet from an object clearly identified as a neutron star. An extensive discussion on the energetics of the complex is presented: a first approach is based on the minimum energy estimation, while a second one employs a self-similar model of the interaction between the jets and the surrounding medium. The results suggest an age for the nebula of \leq 10^5 years and a corresponding time-averaged jet power \geq 10^{35} erg s^{-1}. During periodic flaring episodes, the instantaneous jet power may reach values of similar magnitude to the X-ray luminosity.Comment: Accepted to MNRA

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A multi-wavelength study of the western lobe of W50 powered by the galactic microquasar SS 433

Cited by 19 publications

References 8 publications

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

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

Deep optical observations of the interaction of the SS 433 microquasar jet with the W50 radio continuum shell

The large-scale jet-powered radio nebula of Circinus X-1

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