Detalles de publicación
PP 020108
Discovery of optical outflows and inflows in the black hole candidate GRS 1716-249
(1) Instituto de Astrofísica de Canarias; (2) Departamento de Astrofísica, Universidad de La Laguna; (3) South African Astronomical Observatory; (4) University of Southampton; (5) European Southern Observatory; (6) Pontificia Universidad Católica de Chile; (7) University of Oxford; (8) Istituto di Astrofisica e Planetologia Spaziali; (9) Jodrell Bank Centre for Astrophysics; (10) INAF-Osservatorio Astronomico di Brera; (11) Max-Planck-Institut für Extraterrestrische Physik
We present optical spectroscopy obtained with the GTC, VLT and SALT telescopes during the decline of the 2016–2017 outburst of the black hole candidate GRS 1716-249 (Nova Oph 1993). Our 18-epoch data set spans 6 months and reveals that the observational properties of the main emission lines are very variable, even on timescales of a few hours. Several epochs are characterised by P-Cyg (as well as flat-top and asymmetric) profiles in the Hα, Hβ and He II (λ4686) emission lines, implying the presence of an accretion disc wind, which is likely hot and dense. The wind’s terminal velocity (∼2000 km/s) is similar to that observed in other black hole X-ray transients. These lines also show transient and sharp red-shifted absorptions, taking the form of inverted P-Cyg profiles. We argue that these profiles can be explained by the presence of infalling material at ∼1300 km/s. We propose a failed wind scenario to explain this inflow and discuss other alternatives, such as obscuration produced by an accretion-related structure (e.g. the gas stream) in a high inclination system.

