R144 revealed as a double-lined spectroscopic binary

TL;DR

This study confirms R144 as the most massive known binary star system, revealing its double-lined spectroscopic binary nature through multi-epoch spectroscopy, with implications for star formation and stellar dynamics.

Contribution

First detection of R144 as a double-lined spectroscopic binary using multi-epoch spectroscopy, estimating component masses and orbital parameters.

Findings

R144 is a double-lined spectroscopic binary.

Estimated total mass of 200-300 Msun, possibly up to 400 Msun at birth.

Orbital period likely between 2 to 6 months.

Abstract

R144 is a WN6h star in the 30 Doradus region. It is suspected to be a binary because of its high luminosity and its strong X-ray flux, but no periodicity could be established so far. Here, we present new Xshooter multi-epoch spectroscopy of R144 obtained at the ESO Very Large Telescope (VLT). We detect variability in position and/or shape of all the spectral lines. We measure radial velocity variations with an amplitude larger than 250 km/s in NIV and NV lines. Furthermore, the NIII and NV line Doppler shifts are anti-correlated and the NIV lines show a double-peaked profile on six of our seven epochs. We thus conclude that R144 is a double-lined spectroscopic binary. Possible orbital periods range from 2 to 6 months, although a period up to one year is allowed if the orbit is highly eccentric. We estimate the spectral types of the components to be WN5-6h and WN6-7h, respectively. The high luminosity of the system (log Lbol/Lsun ~ 6.8) suggests a present-day total mass content in the range of about 200 to 300 Msun, depending on the evolutionary stage of the components. This makes R144 the most massive binary identified so far, with a total mass content at birth possibly as large as 400 Msun. We briefly discuss the presence of such a massive object 60 pc away from the R136 cluster core in the context of star formation and stellar dynamics.