Jet interaction of SS 433 with the ambient medium

Durouchoux, Ph.; Sood, R. K.; Oka, Tomoharu; Segers, Marijke C.; Safi‐Harb, Samar; Vilhu, O.; Huovelin, J.; Thresher, D.; Corbel, S.

doi:10.1016/s0273-1177(99)00826-1

Cited by 9 publications

(13 citation statements)

References 8 publications

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“…For example, we previously detected a correlation between the ROSAT X-ray hot spots and the CO millimeter measurements in observations of SS 433 (Durouchoux et al 2000). The higher ionization environments in shocked molecular gas and near X-ray sources can also enhance the emission from molecules such as HCOà nd HCN (Krolik & Kallman 1983 ;Phillips & Lazio 1995 ;Lepp & Dalgarno 1996 ;Yan & Dalgarno 1997).…”

Section: Millimeter Observationsmentioning

confidence: 91%

Simultaneous Observations of GRS 1758−258 in 1997 by VLA, IRAM, SEST,RXTE, and OSSE: Spectroscopy and Timing

Lin

Smith

Liang

et al. 2000

ApJ

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We report the results of our multiwavelength observations of GRS 1758[258 made in 1997 August. The energy bands include radio, millimeter, X-ray, and gamma-ray. The observations enable us to obtain a complete spectrum of the source over an energy range of 2È500 keV. The spectrum shows that GRS 1758[258 was in its hard state. It is well Ðt by the Sunyaev-Titarchuk (ST) Compton scattering model with a plasma temperature of 45 keV and a Thomson depth of 3.3. Taking relativistic e †ects into account, we get a little higher plasma temperature (52 keV) by using the improved version of the ST model (HT model) plus a soft blackbody component. The spectrum is also Ðt by a power law with an exponential cuto † (PLE) plus a soft blackbody component. The temperature of the soft components in both models is about 1.2 keV, and the energy Ñux is less than 1.5% of the total X-ray and gamma-ray Ñux. The deduced hydrogen column density is in the range of (0.93È2.0) ] 1022 cm~2. No signiÐcant iron lines are detected. The radio emission has a Ñat energy spectrum. The daily radio, X-ray, and gamma-ray light curves show that GRS 1758[258 was stable during the observation period but was highly variable on smaller timescales in X-rays and gamma rays. The power density spectra are typical for the low state, but we Ðnd the photon Ñux for the 5È10 keV band to be more variable than that in the other two energy bands (2È5 keV and 10È40 keV). Harmonically spaced quasi-periodic oscillations are observed in the power spectra. The phase lags between the hard photons and the soft photons have a Ñat distribution over a wide range of frequencies. A high coherence of about 1.0 (0.01È1 Hz) between the hard photons and the soft photons is also obtained in our observations. We compare these results with two variation models. Our millimeter observations did not reveal any conclusive signatures of an interaction between the jet from GRS 1758[258 and the molecular cloud that lies in the direction of GRS 1758[258.

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Section: Millimeter Observationsmentioning

confidence: 91%

Simultaneous Observations of GRS 1758−258 in 1997 by VLA, IRAM, SEST,RXTE, and OSSE: Spectroscopy and Timing

Lin

Smith

Liang

et al. 2000

ApJ

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“…Based on the above analysis, we argue that the MCs in the velocity range of 20-70 km s −1 are accidental superpositions along the LOS and are not associated with the SS 433/W50 system. Both of the very long GMF (see discussions in Huang et al 1983) at V LSR ∼ 29-34 km s −1 and the gas features at V LSR ∼ 40-60 km s −1 (Dubner et al 1998;Durouchoux et al 2000;Yamamoto et al 2008) appear to be just the foreground gas of SS 433/W50 in the FOV. We will not discuss these MCs any further because the above gas is not related to SS 433/W50 at a distance of 4.9 kpc (see Section 4).…”

Section: Other Interesting Mcsmentioning

confidence: 97%

“…On the other hand, MCs at 50-55 km s −1 were suggested to be related to the W50 lobe toward the Galactic plane due to the spatial coincidence between them (Durouchoux et al 2000;Chaty et al 2001;Yamamoto et al 2008). 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.…”

Section: 3mentioning

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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“…The eastern ear shows a helical pattern within the radio continuum morphology, thought to mirror the large scale precession of the jets. The western ear (which is believed to be located in a higher density medium) is smaller in scale, brighter at radio frequencies, and displays multiple hot-spots (Fuchs 2002) that coincide with X-ray (Safi-Harb & Ogelman 1997), infrared (Band 1987;O'Neill et al 2000), and sub-mm molecular emission (CO, HCO + ; Huang et al 1983;Durouchoux et al 2000;Chaty et al 2001). These hot-spots are thought to mark sites where the precessing jet collides with the ambient medium, and the dust and gas are being heated by a shock driven jet-ISM interaction (Fuchs 2002).…”

Section: Comparison To Other Known Jet-ism Interaction Zonesmentioning

confidence: 99%

Mapping jet–ISM interactions in X-ray binaries with ALMA: a GRS 1915+105 case study

Tetarenko

Freeman

Rosolowsky

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present Atacama Large Millimetre/Sub-Millimetre Array (ALMA) observations of IRAS 19132+1035, a candidate jet-ISM interaction zone near the black hole X-ray binary (BHXB) GRS 1915+105. With these ALMA observations (combining data from the 12 m array and the Atacama Compact Array), we map the molecular line emission across the IRAS 19132+1035 region. We detect emission from the 12 CO [Given the morphological, spectral, and kinematic properties of this molecular emission, we present several lines of evidence that support the presence of a jet-ISM interaction at this site, including a jet-blown cavity in the molecular gas. This compelling new evidence identifies this site as a jet-ISM interaction zone, making GRS 1915+105 the third Galactic BHXB with at least one conclusive jet-ISM interaction zone. However, we find that this interaction occurs on much smaller scales than was postulated by previous work, where the BHXB jet does not appear to be dominantly powering the entire IRAS 19132+1035 region. Using estimates of the ISM conditions in the region, we utilize the detected cavity as a calorimeter to estimate the time-averaged power carried in the GRS 1915+105 jets of (8.4 +7.7 −8.1 ) × 10 32 erg s −1 . Overall, our analysis demonstrates that molecular lines are excellent diagnostic tools to identify and probe jet-ISM interaction zones near Galactic BHXBs.

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Jet interaction of SS 433 with the ambient medium

Cited by 9 publications

References 8 publications

Simultaneous Observations of GRS 1758−258 in 1997 by VLA, IRAM, SEST,RXTE, and OSSE: Spectroscopy and Timing

Simultaneous Observations of GRS 1758−258 in 1997 by VLA, IRAM, SEST,RXTE, and OSSE: Spectroscopy and Timing

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

Mapping jet–ISM interactions in X-ray binaries with ALMA: a GRS 1915+105 case study

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