Optical and near-infrared observations of the microquasar V4641 Sagittarii during the 1999 September outburst

Details Optical and near-infrared observations of the microquasar V4641 Sagittarii during the 1999 September outburst Optical and near-infrared observations of the microquasar V4641 Sagittarii during the 1999 September outburst

2003-03-24

arxiv.org/abs/astro-ph/0303536v1

Mon.Not.Roy.Astron.Soc. 343 (2003) 169

Astronomy and Astrophysics

Astrophysics

7 pages, 6 figures, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2003.06651.x

We present photometric and spectroscopic optical and near-infrared (NIR) observations (Based on observations collected at the European Southern Observatory, Chile (ESO ID 63.H-0493 and 64.H-0382)) taken during the outburst of the microquasar V4641 Sgr = SAX J1819.3-2525 (in'tzand et al., 2000) in September 1999. We observed an increase in the J-Ks colour between 5 and 8 days after the outburst, which we interpret as likely evidence for the presence of dust around the source. We also observed an extraordinarily strong, broad and variable H_alpha line, with a velocity width of 4560 km/s suggesting the presence of a high-velocity outflow component. We constrain the distance of the system between 3 and 8 kpc, locating it further away than previously derived from radio observations (Hjellming et al., 2000), but consistent with Orosz et al. (2001). We then discuss the nature of this system, showing that the companion star is either a B3-A2 main sequence star, or a B3-A2 sub-giant crossing the Hertzsprung gap. The system is therefore an Intermediate or High Mass X-ray Binary System (IMXB or HMXB). The distance derived by these optical/NIR observations implies that the jets observed by Hjellming et al. (2000) would then exhibit apparent velocities of ~ 10 c. We finally discuss the possibility of an interaction between the jets and surroundings of the source, and also of this source being a ``microblazar''.

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