IRAS observations of SS 433 and W50

Abstract

IRAS observations show SS 433 to be a weak but detectable infrared source at 12 |x and 25 |x. The mid-infrared flux is consistent with a continuation of the spectrum at higher frequencies, although the spectrum flattens at low frequency. The resulting spectrum can be explained as the sum of a constant blackbody component and a variable optically thin free-free emission component. No variability is apparent; however, the timing of the observations does not preclude greater intrinsic variability than was observed. The surrounding W50 radio source is not apparent in the infrared, although there is a plateau of infrared emission to the north-northwest that includes the H II region S74. A number of knots with steep spectra can be identified which emit on the order of 10 37 ergs sec 1 if they are at the distance of SS 433. In particular, three infrared knots lie on the jet axis within W50 and two of these three knots bracket the western optical filament. No Ha emission was detected from the western knots. The optical filaments have no obvious infrared emission.

Rossi X‐Ray Timing ExplorerObservations of the Eastern Lobe of W50 Associated with SS 433

“…All the Ðlaments lie well inside the eastern and western boundaries of W50 and within the precession cone of the SS 433 jets. This led to the suggestion that they result from the propagation of shock waves into the preexisting dense Ðlaments of the SNR along the direction of the impinging jets.Infrared observations of W50 (Band 1987 ;Wang et al 1990) reveal the presence of knots aligned with the jets of SS 433. Wang et al (1990) argue that these knots result from dust grains and gas being heated by the fast electrons and ions in the jets.…”

Observations of Molecular Hydrogen in Shocks and PDRs with the Infrared Space Observatory

“…It is equally certain however that even more questions will be raised. C. M. Wright: The detections of the H 2 0-0 8(3) line were made towards the infrared knots 3 and 5 found by Band (1987, PASP, 99, 1269. But more work is needed to confirm that the lines do not arise from somewhere else along the line of sight, e.g.…”

“…Six knots of infrared emission were discovered toward the X-ray binary source SS 433 by Band (1987) using IRAS data. Wang et al (1990) proposed that the knots were due to an interaction between the SS 433 jets and the interstellar medium.…”

“…Spectra taken using the ISO-SWS, shown in Figure 4 Spectra of the H20-0 S(3) and unresolved OH doublet lines toward the infra-red knots 5 and 3 respectively of the X-ray binary SS 433. that molecular material is present in the direction of the knots, but as yet do not clearly identify X-rays as being the heating agent. Band (1987) suggests that there are several unrelated molecular clouds along the line-of-sight, indicated by different velocities. Indeed the heliocentric velocity of the OH absorption line varies between -200 and +100 km s-1 between knots 3 and 5, which are only separated by rv 1.5 arcminutes on the sky, whereas the H 2 0-0 8(3) line remains relatively constant at 0-30 km s-l.…”

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

“…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).…”