An Apparently Extended Infrared Counterpart to 1e 1740.7–2942

Martı́, Josep; Luque-Escamilla, Pedro L.; Sánchez‐Sutil, J. R.; Muñoz‐Arjonilla, A. J.; Sánchez-Ayaso, E.; Combi, J. A.; García-Hernández, M.T.

doi:10.1088/2041-8205/721/2/l126

Cited by 10 publications

(13 citation statements)

References 14 publications

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“…1 we provide a general view of the 1E 1740.7−2942 field for illustrative purposes. This figure shows the microquasar location in a complex region rich in extended radio emission (Martí et al 2010). Other large-scale filamentary features, such as G359.10−00.20 also known as the Galactic center Snake (Yusef-Zadeh et al 1984) are present as well.…”

Section: Introductionmentioning

confidence: 80%

“…In particular, the absolute magnitude of the infrared counterpart candidate proposed in Martí et al (2010) should be revised to K s = −3.0. At 5 kpc, this would be consistent with an early-type B star on the main sequence or a middle-KIII giant star.…”

Section: Implications Of the Precession Modelmentioning

confidence: 99%

“…In contemporary times, the infrared counterpart of GRS 1758−258 has been confidently identified as a variable, point-like source whose spectral energy distribution agrees with a microquasar system harboring a low-mass stellar companion (Luque-Escamilla et al 2014). For 1E 1740.7−2942, only a candidate counterpart has been reported in the near-infrared based on astrometric coincidence with the X-ray and radio position of the microquasar central core (Martí et al 2010). Accounting for the high interstellar absorption towards this source, the observed magnitudes agree with a high-mass X-ray binary (HMXB) or a low-mass X-ray binary (LMXB) microquasar, depending on the near-infrared emission being dominated or not by stellar emission and, of course, the assumed distance.…”

Section: Introductionmentioning

confidence: 99%

“…For 1E 1740.7−2942, only a candidate counterpart has been reported in the nearinfrared based on astrometric coincidence with the X-ray and radio position of the microquasar central core (Martí et al 2010). Accounting for the high interstellar absorption towards this source, the observed magnitudes agree with a high-mass X-ray binary (HMXB) or a low-mass X-ray binary (LMXB) microquasar, depending on the near-infrared emission being dominated or not by stellar emission and, of course, the assumed distance.…”

Section: Introductionmentioning

confidence: 99%

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The precessing jets of 1E 1740.7−2942

Luque-Escamilla¹,

Martı́²,

Martı́nez-Aroza³

2015

A&A

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Context. The source 1E 1740.7−2942 is believed to be one of the two prototypical microquasars towards the Galactic center region whose X-ray states strongly resemble those of Cygnus X-1. Yet, the bipolar radio jets of 1E 1740.7−2942 are very reminiscent of a radio galaxy. The true nature of the object has thus remained an open question for nearly a quarter of a century. Aims. Our main goal here is to confirm the Galactic membership of 1E 1740.7−2942 by searching for morphological changes of its extended radio jets in human timescales. This work was triggered as a result of recent positive detection of fast structural changes in the large-scale jets of the very similar source GRS 1758−258. Methods. We carried out an in-depth exploration of the Very Large Array public archives and fully recalibrated all 1E 1740.7−2942 extended data sets in the C configuration of the array. We obtained and analyzed matching beam radio maps for five epochs, covering years 1992, 1993, 1994, 1997 and 2000, with an angular resolution of a few arcseconds. Results. We clearly detected structural changes in the arc-minute jets of 1E 1740.7−2942 on timescales of roughly a year, which set a firm distance upper limit of 12 kpc. Moreover, a simple precessing twin-jet model was simultaneously fitted to the five observing epochs available. The observed changes in the jet flow are strongly suggestive of a precession period of ∼1.3 yr. Conclusions. The fitting of the precession model to the data yields a distance of ∼5 kpc. This value, and the observed changes, rule out any remaining doubts about the 1E 1740.7−2942 Galactic nature. To our knowledge, this microquasar is the second whose jet precession ephemeris become available after SS433. This kind of information is relevant to the physics of compact objects, since the genesis of the precession phenomenon occurs very close to the interplay region between the accretion disk and the compact object in the system.

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Section: Introductionmentioning

confidence: 80%

Section: Implications Of the Precession Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The precessing jets of 1E 1740.7−2942

Luque-Escamilla¹,

Martı́²,

Martı́nez-Aroza³

2015

A&A

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“…There is, until now, no optical or infrared counterpart confirmed for E-mail: paulo.stecchini@inpe.br 1E 1740.7−2942 -which is usually attributed to the high galactic extinction towards the GC at these wavelengths (see, e.g., Gallo & Fender 2002). In one of the most recent attempts, Martí et al (2010) have successfully identified a single near-infrared source towards the system's location. The study suggested two hypotheses to explain the counterpart candidate detected: an Active Galactic Nucleus projected along the line of sight of the system or a black hole highmass X-ray binary.…”

Section: Introductionmentioning

confidence: 99%

Broadband X-ray analysis of 1E 1740.7−2942: constraints on spin, inclination, and a tentative black hole mass

Stecchini

D'Amico

Jablonski

et al. 2020

Monthly Notices of the Royal Astronomical Society

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1E 1740.7−2942 is one of the strongest hard X-ray emitters in the Galactic Centre region, believed to be a black hole in a high-mass X-ray binary system. Although extensively studied in X-rays, many aspects about the underlying nature of the system are still unknown. For example, X-ray data analyses of 1E 1740.7−2942 up to date have not yet unveiled the signature of a reflection component, whose modelling could be used to estimate parameters such as the spin of the black hole and inclination of the disc. We report here on the determination of these parameters from the analysis of the reflection component present in a public NuSTAR observation which hasn't been subject to any previous study. We include XMM-Newton and INTEGRAL data to build a combined spectrum, enabling a joint analysis of both the disc and comptonisation components. Results point to a relatively high inclination disc 50 • (3 σ) and a near-maximum speed rotating black hole. The former is in agreement with a previous radio study and the latter is reported here for the first time. Lastly, we follow the methodology of recent efforts to weight black holes with only X-ray spectra and find results that suggest a black hole mass of about 5 M for 1E 1740.7−2942.

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