Optical spectroscopy and photometry of SAX J1808.4-3658 in outburst

TL;DR

This study uses optical spectroscopy and photometry during an outburst to analyze the binary system SAX J1808.4-3658, constraining its mass ratio, neutron star mass, and distance, and observing superhump modulation.

Contribution

First phase-resolved optical spectroscopy and Doppler tomography of SAX J1808.4-3658 during outburst, providing new constraints on system parameters and emission origins.

Findings

Mass ratio constrained to ~0.044

Neutron star mass consistent with 1.4 Msun

Distance estimated at ~2.5 kpc

Abstract

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 N III 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; applying a "K-correction", we find the velocity of the secondary star projected onto the line of sight to be 370 +/- 40 km/s. Based on existing pulse timing measurements, this constrains the mass ratio of the system to be 0.044^{+0.005}_{-0.004}, and the mass function for the pulsar to be 0.44^{+0.16}_{-0.13} Msun. 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 1.4 Msun. Our optical light curves exhibit a possible superhump modulation, expected for a system with such a low mass ratio. The equivalent width of the Ca II H and K interstellar absorption lines suggest that the distance to the source is ~2.5 kpc. This is consistent with previous distance estimates based on type-I X-ray bursts which assume cosmic abundances of hydrogen, but lower than more recent estimates which assume helium-rich bursts.