PONTI, GABRIELEGABRIELEPONTIBIANCHI, STEFANOSTEFANOBIANCHIMuñoz-Darias, TeoTeoMuñoz-DariasNandra, KirpalKirpalNandra2020-12-302020-12-3020181745-3925http://hdl.handle.net/20.500.12386/29388The determination of fundamental parameters in low-mass X-ray binaries (LMXBs) typically relies on measuring the radial velocity curve of the companion star through optical or near-infrared spectroscopy. It was recently suggested that high resolution X-ray spectroscopy might enable a measurement of the radial velocity curve of the compact object by monitoring the Doppler shifts induced by the orbital motion of the disc wind or the disc atmosphere. We analysed a Chandra-HETG+NuSTAR soft state observation of MXB 1659-298, an eclipsing neutron star LMXB. We measured a radial velocity curve whose phase offset and semi-amplitude are consistent with the primary star. We derived the value for the semi-amplitude of the radial velocity for the compact object K<SUB>1</SUB> = 89 ± 19 km s<SUP>-1</SUP>, constrained the mass of the secondary (0.3 M<SUB>☉</SUB> ≤ M<SUB>2</SUB> ≤ 0.8 M<SUB>☉</SUB>) and the orbital inclination of the binary system (73°≤ i≤77°). These values are consistent with previous estimates from independent methods. Via the same technique, the next generation of X-ray observatories equipped with high spectral resolution instruments (e.g. Athena) will have the potential to measure the radial velocity curve of the primary in high inclination X-ray binaries to an accuracy of a few per cent.STAMPAenArticle10.1093/mnrasl/sly1202-s2.0-85056464112000451569100020https://academic.oup.com/mnrasl/article/481/1/L94/5046462?login=true2018MNRAS.481L..94PFIS/05 - ASTRONOMIA E ASTROFISICA