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Elebert, P,Reynolds, MT,Callanan, PJ,Hurley, DJ,Ramsay, G,Lewis, F,Russell, DM,Nord, B,Kane, SR,Depoy, DL,Hakala, P;
Monthly Notices of The Royal Astronomical Society
Optical spectroscopy and photometry of SAX J1808.4-3658 in outburst
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accretion, accretion discs binaries: close stars: individual: V4580 Sagittarii stars: neutron pulsars: individual: SAX J1808.4-3658 X-rays: binaries DIFFUSE INTERSTELLAR BANDS ACTIVE RADIO PULSAR X-RAY BINARIES MILLISECOND PULSAR ACCRETION DISCS NEUTRON-STAR LIGHT-CURVE QUIESCENCE COUNTERPART SUPERHUMPS
We present phase resolved optical spectroscopy and photometry of V4580 Sagittarii, the optical counterpart to the accretion powered millisecond pulsar SAX J1808.4-3658, obtained during the 2008 September/October outburst. Doppler tomography of the NIII lambda 4640.64 Bowen blend emission line reveals a focused spot of emission at a location consistent with the secondary star. The velocity of this emission occurs at 324 +/- 15 km s(-1); applying a 'K-correction', we find the velocity of the secondary star projected on to the line of sight to be 370 +/- 40 km s-1. Based on existing pulse timing measurements, this constrains the mass ratio of the system to be 0.044(-0.004)(+0.005), and the mass function for the pulsar to be 0.44(-0.13)(+0.16)M(circle dot). Combining this mass function with various inclination estimates from other authors, we find no evidence to suggest that the neutron star in SAX J1808.4-3658 is more massive than the canonical value of 1.4M(circle dot). Our optical light curves exhibit a possible superhump modulation, expected for a system with such a low mass ratio. The equivalent width of the CaII H and K interstellar absorption lines suggest that the distance to the source is similar to 2.5 kpc. This is consistent with previous distance estimates based on type-IX-ray bursts which assume cosmic abundances of hydrogen, but lower than more recent estimates which assume helium-rich bursts.
DOI 10.1111/j.1365-2966.2009.14562.x
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