VLT spectroscopy of XTE J2123−058 during quiescence: the masses of the two components
Identifieur interne : 000407 ( Main/Exploration ); précédent : 000406; suivant : 000408VLT spectroscopy of XTE J2123−058 during quiescence: the masses of the two components
Auteurs : J. Casares [Espagne] ; G. Dubus [États-Unis] ; T. Shahbaz [Espagne] ; C. Zurita [Espagne] ; P. A. CharlesSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2002-01.
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- KwdEn :
Abstract
We present Very Large Telescope (VLT) low‐resolution spectroscopy of the neutron star X‐ray transient XTE J2123−058 during its quiescent state. Our data reveal the presence of a K7V companion which contributes 77 per cent to the total flux at λ6300 and orbits the neutron star at . Contrary to other soft X‐ray transients (SXTs), the H emission is almost exactly in antiphase with the velocity curve of the optical companion. Using the light‐centre technique we obtain and hence This, combined with a previous determination of the inclination angle yields and . M2 agrees well with the observed spectral type. Doppler tomography of the Hα emission shows a non‐symmetric accretion disc distribution mimicking that seen in SW Sex stars. Although we find a large systemic velocity of − this value is consistent with the galactic rotation velocity at the position of J2123−058, and hence a halo origin. The formation scenario of J2123−058 is still unresolved.
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DOI: 10.1046/j.1365-8711.2002.04964.x
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<front><div type="abstract" xml:lang="en">We present Very Large Telescope (VLT) low‐resolution spectroscopy of the neutron star X‐ray transient XTE J2123−058 during its quiescent state. Our data reveal the presence of a K7V companion which contributes 77 per cent to the total flux at λ6300 and orbits the neutron star at . Contrary to other soft X‐ray transients (SXTs), the H emission is almost exactly in antiphase with the velocity curve of the optical companion. Using the light‐centre technique we obtain and hence This, combined with a previous determination of the inclination angle yields and . M2 agrees well with the observed spectral type. Doppler tomography of the Hα emission shows a non‐symmetric accretion disc distribution mimicking that seen in SW Sex stars. Although we find a large systemic velocity of − this value is consistent with the galactic rotation velocity at the position of J2123−058, and hence a halo origin. The formation scenario of J2123−058 is still unresolved.</div>
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