Volume 606, October 2017
|Number of page(s)||18|
|Section||Galactic structure, stellar clusters and populations|
|Published online||26 September 2017|
Binary companions of nearby supernova remnants found with Gaia
1 Institute of Astronomy, University of Cambridge, Madingley Rise, Cambridge, CB3 0HA, UK
2 School of Physics, O’Brien Centre for Science North, University College Dublin, Belfield, Dublin 4, Ireland
3 Astrophysics Group, Cavendish Laboratory, 19 J. J. Thomson Avenue, Cambridge CB3 0HE, UK
Received: 9 May 2017
Accepted: 3 July 2017
Aims. We search for runaway former companions of the progenitors of nearby Galactic core-collapse supernova remnants (SNRs) in the Tycho-Gaia astrometric solution (TGAS).
Methods. We look for candidates among a sample of ten SNRs with distances ≲2kpc, taking astrometry and G magnitude from TGAS and B,V magnitudes from the AAVSO Photometric All-Sky Survey (APASS). A simple method of tracking back stars and finding the closest point to the SNR centre is shown to have several failings when ranking candidates. In particular, it neglects our expectation that massive stars preferentially have massive companions. We evolve a grid of binary stars to exploit these covariances in the distribution of runaway star properties in colour – magnitude – ejection velocity space. We construct an analytic model which predicts the properties of a runaway star, in which the model parameters are the location in the grid of progenitor binaries and the properties of the SNR. Using nested sampling we calculate the Bayesian evidence for each candidate to be the runaway and simultaneously constrain the properties of that runaway and of the SNR itself.
Results. We identify four likely runaway companions of the Cygnus Loop (G074.0−08.5), HB 21 (G089.0+ 04.7), S147 (G180.0+ 01.7) and the Monoceros Loop (G205.5+ 00.5). HD 37424 has previously been suggested as the companion of S147, however the other three stars are new candidates. The favoured companion of HB 21 is the Be star BD+50 3188 whose emission-line features could be explained by pre-supernova mass transfer from the primary. There is a small probability that the 2M⊙ candidate runaway TYC 2688-1556-1 associated with the Cygnus Loop is a hypervelocity star. If the Monoceros Loop is related to the on-going star formation in the Mon OB2 association, the progenitor of the Monoceros Loop is required to be more massive than 40M⊙ which is in tension with the posterior for our candidate runaway star HD 261393.
Key words: supernovae: general / binaries: close / ISM: supernova remnants / methods: statistical / stars: emission-line, Be
© ESO, 2017
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