Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - IV. A 0.61 + 0.45 M⊙ binary in a multiple system

Abstract

We present the orbital and physical parameters of a newly discovered low‐mass detached eclipsing binary from the All‐Sky Automated Survey (ASAS) data base: ASAS J011328–3821.1 A, which is a member of a visual binary system with the secondary component separated by about 1.4 arcsec. The radial velocities have been calculated from the high‐resolution spectra obtained with the 1.9‐m Radcliffe telescope/Grating Instrument for Radiation Analysis with a Fibre‐Fed Echelle (GIRAFFE) spectrograph, the 3.9‐m Anglo‐Australian Telescope (AAT)/University College London Echelle Spectrograph (UCLES) and the 3.0‐m Shane telescope/Hamilton Spectrograph (HamSpec) on the basis of the todcor technique and the positions of the Hα emission lines. For the analysis, we have used V‐ and I‐band photometry obtained with the 1.0‐m Elizabeth telescope and the 0.41‐m Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT), supplemented with the publicly available ASAS light curve of the system. We have found that ASAS J011328–3821.1 A is composed of two late‐type dwarfs, which have masses of M1 = 0.612 ± 0.030 M⊙ and M2 = 0.445 ± 0.019 M⊙ and radii of R1 = 0.596 ± 0.020 R⊙ and R2 = 0.445 ± 0.024 R⊙. Both show a substantial level of activity, which manifests in strong Hα and Hβ emission and the presence of cool spots. The influence of the third light on the eclipsing pair properties has also been evaluated and the photometric properties of component B have been derived. A comparison with several popular stellar evolution models shows that the system is on its main‐sequence evolution stage and that it is probably more metal‐rich than the Sun. We have also found several clues to suggest that component B itself is a binary composed of two nearly identical ∼0.5‐M⊙ stars.

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

“…This is a rare example of a high-order (n > 3) multiple that contains an eclipsing binary. There are only several such known systems, including YY Gem, (Torres & Ribas 2002), V994 Her (Lee et al 2008), ASAS J011328-3821.1 (Hełminiak et al 2012), HD 86222 (Dimitrov et al 2014), KIC 7177553 (Lehmann et al 2016), 1SWASP J093010.78+533859.5 (Koo et al 2014), EPIC 220204960 (Rappaport et al 2017), V482 Per (Torres et al 2017), KIC 4150611 (Hełminiak et al 2017b), and EPIC 219217635 (Borkovits et al 2018). Such systems are usually found in hierarchical configurations, meaning that their components tend to form short-period pairs, which themselves are in large separations.…”

“…In our spectroscopic survey of southern detached eclipsing binaries (DEBs) we initially focused on searching for lowmass pairs, identifying several new ones Hełminiak et al , 2012Hełminiak et al , 2014 but finding even more 1 http://www.astro.keele.ac.uk/~jkt/debcat/ relatively bright, single-lined systems with F-and G-type primaries and faint secondaries not seen or very difficult to identify in the optical spectra 2 . We therefore started a small, loweffort program of infrared (IR) spectroscopic observations with the Subaru telescope, targetting only a few of the most northern objects in our sample.…”

TESS light curves of low-mass detached eclipsing binaries

“…RVs and orbital solutions of AK For and A-011 remain unchanged with respect to the literature (He lminiak et al 2012(He lminiak et al , 2014. In three other cases we used our own new spectroscopy from CHIRON and CORALIE spectrographs, and calculated the RVs with the TODCOR method Zucker & Mazeh (1994).…”

KIC 4150611: a rare multi-eclipsing quintuple with a hybrid pulsator

“…For calculation of the RVs of the G-type pair we decided to use our own implementation of the TODCOR technique (Zucker & Mazeh 1994), which finds velocities v 1 and v 2 of two stars simultaneously. Individual RV errors were estimated with a bootstrap approach (Hełminiak et al 2012).…”