A decade of high-resolution radio observations of GRS 1915+105

Rushton, A.; Spencer, R. E.; Pooley, G. G.; Трушкин, С. А.

doi:10.1111/j.1365-2966.2009.15838.x

Cited by 17 publications

(19 citation statements)

References 20 publications

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“…Galactic black hole accretion systems might serve as laboratories for active galactic nuclei (AGN) on highly contracted time scales. The black hole candidate, GRS 1915+105, routinely ejects powerful radio‐emitting plasma out to large distances from the central black hole at relativistic speeds and might be the Galactic analogue of radio loud AGN (Fender et al 1999; Rodriguez & Mirabel 1999; Rushton et al 2010a). These major flares are relatively rare compared to the so‐called compact jet state (Rushton et al 2010a).…”

Section: Introductionmentioning

confidence: 99%

“…The black hole candidate, GRS 1915+105, routinely ejects powerful radio‐emitting plasma out to large distances from the central black hole at relativistic speeds and might be the Galactic analogue of radio loud AGN (Fender et al 1999; Rodriguez & Mirabel 1999; Rushton et al 2010a). These major flares are relatively rare compared to the so‐called compact jet state (Rushton et al 2010a). A compact, optically thick, elongated structure is frequently observed with long baseline interferometry (Dwahan, Mirabel & Rodriguez 2000; Fuchs et al 2003; Ribo, Dhawan & Mirabel 2004).…”

Section: Introductionmentioning

confidence: 99%

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Models of the compact jet in GRS 1915+105

Punsly¹

2011

Monthly Notices of the Royal Astronomical Society

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In this article, models are constructed of the compact jet in GRS 1915+105 during an epoch of optimal data capture. On 2003 April 2, the object was observed in the hard X‐ray/soft gamma‐ray band (INTEGRAL), hard X‐ray band (RXTE), near‐IR (ESO/New Technology Telescope) and the Very Long Baseline Array (VLBA) (8.3 and 15 GHz). The source was in a so‐called ‘high plateau state’. The large radio flux provides high signal‐to‐noise ratios in the radio images. Thus, one can image the jet out to large distances (>1015 cm). This combined with the broad‐band coverage make this epoch the best suited for modelling the jet. The parametric method that has been successfully utilized in the realm of extragalactic radio jets is implemented. The basic model is one where external inverse Compton (EIC) scattering of accretion disc photons by jet plasma provides the hard X‐ray power law. Unlike active galactic nucleus (AGN) jets, it is found that the radio jet must be highly stratified in the transverse direction in order to produce the observed surface brightness distribution in the radio images. Various jet models are considered. The jet power is Q ≈ 3–4 × 1038 erg s−1 if the hard X‐ray power‐law luminosity is from EIC in the jet and Q ≈ 2–9 × 1037 erg s−1 if the X‐rays are emitted from the accretion disc corona. These estimates indicate that the jet power can be as high as 60 per cent of the total X‐ray luminosity.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Models of the compact jet in GRS 1915+105

Punsly¹

2011

Monthly Notices of the Royal Astronomical Society

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“…Further, it has been postulated that the GRS 1915+105 jet may be precessing (Rodriguez & Mirabel 1999;Rushton et al 2010), which could result in the energy carried by the jet being smeared around a conical path, with only a fraction of the arc traced out by the precessing jet depositing energy into the molecular cloud. Assuming the precessing jet traces out a cone, with opening angle of ∼ 10 degrees (Rodriguez & Mirabel 1999) and edge length of the distance between the sources (42.5 pc), then the power in the jet would be larger by a factor of 2πR cone arclength ∼ 150 (for R cone = 7 pc and arclength = 0.3 pc), resulting in Q jet,precess ∼ 1 × 10 35 erg s −1 .…”

Section: Constraints On Jet Propertiesmentioning

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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“…Several of these are associated with resolved structure and have emitted jansky-strength radio flares which show pronounced evolution in intensity on intraday time scales. Examples include Circinus X-1 (Haynes et al 1978;Tudose et al 2008), Cygnus X-3 (Tudose et al 2009) and GRS 1915+ 105 (Fender et al 1999;Rushton et al 2010).…”

Section: Introductionmentioning

confidence: 99%

A multiple-beam CLEAN for imaging intra-day variable radio sources

Stewart

Fenech

Muxlow

2011

A&A

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The CLEAN algorithm, widely used in radio interferometry for the deconvolution of radio images, performs well only if the raw radio image (dirty image) is, to good approximation, a simple convolution between the instrumental point-spread function (dirty beam) and the true distribution of emission across the sky. An important case in which this approximation breaks down is during frequency synthesis if the observing bandwidth is wide enough for variations in the spectrum of the sky to become significant. The convolution assumption also breaks down, in any situation but snapshot observations, if sources in the field vary significantly in flux density over the duration of the observation. Such time-variation can even be instrumental in nature, for example due to jitter or rotation of the primary beam pattern on the sky during an observation. An algorithm already exists for dealing with the spectral variation encountered in wide-band frequency synthesis interferometry. This algorithm is an extension of CLEAN in which, at each iteration, a set of N "dirty beams" are fitted and subtracted in parallel, instead of just a single dirty beam as in standard CLEAN. In the wide-band algorithm the beams are obtained by expanding a nominal source spectrum in a Taylor series, each term of the series generating one of the beams. In the present paper this algorithm is extended to images which contain sources which vary over both frequency and time. Different expansion schemes (or bases) on the time and frequency axes are compared, and issues such as Gibbs ringing and non-orthogonality are discussed. It is shown that practical considerations make it often desirable to orthogonalize the set of beams before commencing the cleaning. This is easily accomplished via a Gram-Schmidt technique.

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A decade of high-resolution radio observations of GRS 1915+105

Cited by 17 publications

References 20 publications

Models of the compact jet in GRS 1915+105

Models of the compact jet in GRS 1915+105

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

A multiple-beam CLEAN for imaging intra-day variable radio sources

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