A Multiwavelength Investigation of the Relationship between 2CG 135+1 and LSI +61o303

Strickman, M. S.; Tavani, M.; Coe, M. J.; Steele, I. A.; Fabregat, J.; Martı́, Josep; Paredes, J. M.; Ray, Paul S.

doi:10.1086/305446

Cited by 37 publications

(49 citation statements)

References 32 publications

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“…• 303 (Strickman et al 1998). As can be seen from the radio light curve taken with the Green Bank Interferometer 1 (GBI) as part of that campaign ( Fig.…”

Section: Fig 1 Radio Light Curve Of Ls I +61mentioning

confidence: 94%

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One-sided jet at milliarcsecond scales in LS I +61°303

Massi

Ribó

Paredes

et al. 2001

A&A

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104

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Abstract. We present Very Long Baseline Interferometry (VLBI) observations of the high mass X-ray binary LS I +61• 303, carried out with the European VLBI Network (EVN). Over the 11 hour observing run, performed ∼10 days after a radio outburst, the radio source showed a constant flux density, which allowed sensitive imaging of the emission distribution. The structure in the map shows a clear extension to the southeast. Comparing our data with previous VLBI observations we interpret the extension as a collimated radio jet as found in several other X-ray binaries. Assuming that the structure is the result of an expansion that started at the onset of the outburst, we derive an apparent expansion velocity of 0.003 c, which, in the context of Doppler boosting, corresponds to an intrinsic velocity of at least 0.4 c for an ejection close to the line of sight. From the apparent velocity in all available epochs we are able to establish variations in the ejection angle which imply a precessing accretion disk. Finally we point out that LS I +61• 303, like SS 433 and Cygnus X-1, shows evidence for an emission region almost orthogonal to the relativistic jet.

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“…• 303 (Strickman et al 1998). As can be seen from the radio light curve taken with the Green Bank Interferometer 1 (GBI) as part of that campaign ( Fig.…”

Section: Fig 1 Radio Light Curve Of Ls I +61mentioning

confidence: 94%

“…• 303 obtained with the GBI at 8.4 GHz (Strickman et al 1998). The shaded area indicates the time interval during which our VLBI data were taken.…”

Section: Fig 1 Radio Light Curve Of Ls I +61mentioning

confidence: 99%

One-sided jet at milliarcsecond scales in LS I +61°303

Massi

Ribó

Paredes

et al. 2001

A&A

Self Cite

104

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“…This sets an upper limit on the modeled radio flux. In addition, we have also plotted radio data from Strickman et al (1998), which correspond to an orbital phase of 0.8 and a superorbital phase of 0.8.…”

Section: Spectral Energy Distributionmentioning

confidence: 99%

“…Radio data shown in the figure do not correspond to state1. The average flux from OVRO is shown with filled red circles, whereas the radio data from Strickman et al (1998) are shown by brown triangles.…”

Section: Spectral Energy Distributionmentioning

confidence: 99%

THE MULTI-WAVELENGTH CHARACTERISTICS OF THE TeV BINARY LS I+61°303

Saha

Chitnis

Shukla

et al. 2016

ApJ

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We study the characteristics of the TeV binary LS I+61°303 in radio, soft X-ray, hard X-ray, and gamma-ray (GeV and TeV) energies. The long-term variability characteristics are examined as a function of the phase of the binary period of 26.496 days as well as the phase of the superorbital period of 1626 days, dividing the observations into a matrix of 10 × 10 phases of these two periods. We find that the long-term variability can be described by a sine function of the superorbital period, with the phase and amplitude systematically varying with the binary period phase. We also find a definite wavelength-dependent change in this variability description. To understand the radiation mechanism, we define three states in the orbital/superorbital phase matrix and examine the wideband spectral energy distribution. The derived source parameters indicate that the emission geometry is dominated by a jet structure showing a systematic variation with the orbital/superorbital period. We suggest that LS I+61°303 is likely a microquasar with a steady jet.

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“…In their scenario the γ-rays are produced by Inverse Compton upscattering of stellar UV photons by the non-thermal relativistic electron population that later on will produce the detected radio emission. On the other hand, the X-ray binary system LS I +61 303 has been associated with the EGRET source 3EG J0241+6103 (Tavani et al 1996;Kniffen et al 1997;Strickman et al 1998;Harrison et al 2000), and recently Massi et al (2001Massi et al ( , 2004 have revealed its MQ nature. If the MQ nature of AX J1639.0−4642 is confirmed, it could be the third MQ source related to a high-energy gammaray source detected by the EGRET telescope.…”

Section: Microquasars As Possible Counterparts Of Unidentified Egret mentioning

confidence: 99%

The dust-enshrouded microquasar candidate AX J1639.0-4642 = IGR J16393-4643

Combi

Ribó

Mirabel

et al. 2004

A&A

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Abstract. We present a multiwavelength study of the field containing the unidentified X-ray source AX J1639.0−4642, discovered with the ASCA observatory and recently detected with the IBIS telescope, onboard the INTEGRAL satellite, dubbed IGR J16393−4643. The huge hydrogen column density towards the source, the hard spectral index in the 0.7-10 keV band and its flux variability suggest that the source is a High Mass X-ray Binary (HMXB) enshrouded by dust. Our search reveals the presence of a non-thermal radio counterpart within the X-ray error box. After a study of the broadband emission from X-rays to the radio domain, we propose that AX J1639.0−4642 is a dust-enshrouded Microquasar (MQ) candidate. In addition, the X-ray source is well within the 95% location contour of the unidentified γ-ray source 3EG J1639−4702. The main properties of AX J1639.0−4642/3EG J1639−4702 are consistent with those of two other MQs previously proposed to display high-energy γ-ray emission.

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A Multiwavelength Investigation of the Relationship between 2CG 135+1 and LSI +61o303

Cited by 37 publications

References 32 publications

One-sided jet at milliarcsecond scales in LS I +61°303

One-sided jet at milliarcsecond scales in LS I +61°303

THE MULTI-WAVELENGTH CHARACTERISTICS OF THE TeV BINARY LS I+61°303

The dust-enshrouded microquasar candidate AX J1639.0-4642 = IGR J16393-4643

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