Towards a dynamical mass of the ultraluminous X-ray source NGC 5408 X-1

Abstract

We obtained multi-epoch Very Large Telescope (VLT) optical spectroscopic data in 2011 and 2012 on the ultraluminous X-ray source (ULX) NGC 5408 X-1. We confirm that the HeII\lambda4686 line has a broad component with an average FWHM of v=780\pm64 km/s with a variation of ~13% during observations spanning over 4 years, and is consistent with the origin in the accretion disc. The deepest optical spectrum does not reveal any absorption line from a donor star. Our aim was to measure the radial velocity curve and estimate the parameters of the binary system. We find an upper limit on the semi-amplitude of the radial velocity of K=132\pm42 km/s. A search for a periodic signal in the data resulted in no statistically significant period. The mass function and constraints on the binary system imply a black hole mass of less than ~510 M_sun. Whilst, a disc irradiation model may imply a black hole mass smaller than ~431-1985 M_sun, depending on inclination. Our data can also be consistent with an unexplored orbital period range from a couple of hours to a few days, thus with a stellar-mass black hole and a subgiant companion.

8 pages, 7 figures, accepted for publication in MNRAS

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• Evidence for High-Frequency QPOs with a 3:2 Frequency Ratio from a 5000 Solar Mass Black Hole
• X-ray time lags and nonlinear variability in the ultraluminous X-ray sources NGC 5408 X-1 and NGC 6946 X-1
• Temporal evolution of long-timescale periodicities in ULX NGC 5408 X-1
• Variability in Ultra-luminous X-ray Sources
• Identification of a Helium Donor Star in NGC 247 ULX-1
• Experimental study of an advanced concept of moderate-resolution holographic spectrographs
• X-ray reverberation models of the disc wind in ultraluminous X-ray source NGC 5408 X-1
• First Search for an X-ray -- Optical Reverberation Signal in an Ultraluminous X-ray Source