The precessing jets of 1E 1740.7-2942

TL;DR

This study confirms 1E 1740.7-2942 as a Galactic microquasar by detecting jet precession and morphological changes over years, providing insights into its distance and jet dynamics.

Contribution

First to measure jet precession in 1E 1740.7-2942, confirming its Galactic nature and estimating its distance using multi-epoch radio observations.

Findings

Detected structural changes in jets over ~1 year

Estimated distance of ~5 kpc

Identified jet precession period of ~1.3 years

Abstract

Context. 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 its 'twin' GRS 1758-258. Methods. We carried out an in-depth exploration of the VLA 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 arcminute 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 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 years. 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.