| 1. |
- Hebb, L., et al.
(author)
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MML 53 : a new low-mass, pre-main sequence eclipsing binary in the Upper Centaurus-Lupus region discovered by SuperWASP
- 2010
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In: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 522:2, s. A37-
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Journal article (peer-reviewed)abstract
- We announce the discovery of a new low-mass, pre-main sequence eclipsing binary, MML 53. Previous observations of MML 53 found it to be a pre-main sequence spectroscopic multiple associated with the 15-22 Myr Upper Centaurus-Lupus cluster. We identify the object as an eclipsing binary for the first time through the analysis of multiple seasons of time series photometry from the SuperWASP transiting planet survey. Re-analysis of a single archive spectrum shows MML 53 to be a spatially unresolved triple system of young stars which all exhibit significant lithium absorption. Two of the components comprise an eclipsing binary with period, P = 2.097891(6) +/- 0.000005 and mass ratio, q similar to 0.8. Here, we present the analysis of the discovery data.
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| 2. |
- Hebb, L., et al.
(author)
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Precise orbit solution of MML 53, a low-mass, pre-main sequence eclipsing binary in Upper Centaurus Lupus
- 2011
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In: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 531, s. A61-
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Journal article (peer-reviewed)abstract
- Aims. We present a double-lined orbit solution for MML 53, the recently discovered low-mass pre-main sequence eclipsing binary. Methods. Using high-resolution spectra from the SMARTS 1.5 m echelle spectrograph, we measure precise radial velocities and derive the orbital parameters of the system. Results. The 2.1 d orbit of the eclipsing pair is circular, and we find the minimum masses of the eclipsing components to be M(1) sin(3) i = 0.97 M(circle dot) and M(2) sin(3) i = 0.84 M(circle dot), with formal uncertainties of 2.0% and an additional systematic uncertainty of approximate to 2.5% most likely caused by large star spots on the primary star. MML 53 has been previously identified as a member of the Upper Centaurus Lupus (UCL) star forming region (age similar to 15 Myr). The systemic radial velocity from our orbit solution, v(gamma) = + 1.4 +/- 0.3 +/- 0.8 km s(-1) (statistical and systematic), is also consistent with kinematic membership in this association. In addition, we detect a change in v(gamma) between 2006 and 2009 providing further evidence for the presence of a the third body in a wide (several year) orbit.
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