2002/11/25 by Gloria Koenigsberger, Gabriela Canalizo, Koenigsberger, Gloria +10 · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Adaptive optics and wavefront sensing #Astrophysics (astro-ph) #FOS: Physical sciences #Geophysics and Gravity Measurements #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0211554
33 pages, including 13 eps figures. Uses rmaa.cls (included). To appear in RevMexAA
arxiv created 2002/11/25 · openalex publication_date 2002/11/25 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We present high resolution spectroscopic observations of the massive X-ray binary system LS I+65 010=2S 0114+650 in the optical wavelength region. A correlation between equivalent width and radial velocity of photospheric absorption lines is found. The systemic velocity, inferred from the weaker lines is vhelio = -31 +/- 5 km s-1, which, if attributed solely to the Galactic rotation curve, implies that LS I+65 010 lies within 3 kpc from the Sun. The ISM Na I D lines display 2 resolved high velocity components at vhelio = -70, -48 km s-1, possibly associated with gas surrounding the binary system, in addition to the -24, -8 km s-1 ISM features due to the Orion and the Perseus arm regions. Strong photospheric line profile variability is present on a night to night timescale, with He I 5875 A displaying an additional blue-shifted absorption in some of the spectra, similar to what is observed in the optical counterpart of Vela X-1. A connection between the extended blue wing and X-ray maximum is suggested. Short timescale variations in line profiles are detected on only two nights, but the evidence that these variations occur on the 2.78 hour X-ray flaring period is marginal.