The spectroscopic orbits of three double-lined eclipsing binaries: I. BG Ind, IM Mon, RS Sgr

Bakış, V.; Bakıș, H.; Bilir, S.; Soydugan, F.; Soydugan, E.; Demirçan, Osman; Eker, Z.; Yaz, E.; Tüysüz, M.; Šenyüz, T.

doi:10.1016/j.newast.2009.05.005

Cited by 8 publications

(20 citation statements)

References 20 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…1). 3 The same conclusion follows from the velocities measured by Bakış et al (2010), which also nicely phase with ephemeris (1), showing, however, a much larger scatter (the rms residual from our fit to their data is 4.6 km s −1 , only slightly larger than 4.4 km s −1 found in the original paper).…”

Section: Discussionsupporting

confidence: 76%

“…The value found by VHM (39.8 ± 4 km s −1 ) was based on two measurements only, and its error was likely underestimated. 59.4 ± 5 km s −1 of Bakış et al (2010) is rather large for an F-type star in the Sun's vicinity. The origin of such a large discrepancy with all remaining estimates is difficult to explain -we may only note that they did not observe any radial velocity standards, and it is conceivable that they reversed the sign of the heliocentric correction while reducing the data.…”

Section: Discussion a N D C O N C L U S I O N Smentioning

confidence: 85%

“…BG Ind was monitored by Hipparcos satellite (Perryman et al 1997) and robotic telescopes ASAS (Pojmanski 2001) and Pi of the Sky (Małek et al 2010); it is also included in 'The Geneva-Copenhagen survey of the solar neighbourhood' (Holmberg, Nordström & Andersen 2009). Recently, a spectroscopic solution of BG Ind based on data collected in 2006 has been published by Bakış et al (2010), who for P = 1.464 069 d and i = 74. • 14 found by VHM obtained m 1 = 1.47 ± 0.01 M , m 2 = 1.31 ± 0.01 M , and a semimajor axis a = 7.64 ± 0.04 R .…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Absolute properties of BG Ind - a bright F3 system just leaving the main sequence★

Rozyczka

Kałużny

Pych

et al. 2011

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present photometric and spectroscopic analysis of the bright detached eclipsing binary BG Ind. The masses of the components are found to be 1.428 ± 0.008 and 1.293 ± 0.008 M⊙ and the radii to be 2.290 ± 0.017 and 1.680 ± 0.038 R⊙ for primary and secondary stars, respectively. Spectra and isochrone fittings coupled with colour indices calibration yield [Fe/H]=−0.2 ± 0.1. At an age of 2.65 ± 0.20 Gyr, BG Ind is well advanced in the main‐sequence evolutionary phase – in fact, its primary is at TAMS or just beyond it. Together with three similar systems (BK Peg, BW Aqr and GX Gem), it offers an interesting opportunity to test the theoretical description of overshooting in the critical mass range 1.2–1.5 M⊙.

show abstract

Section: Discussionsupporting

confidence: 76%

Section: Discussion a N D C O N C L U S I O N Smentioning

confidence: 85%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Absolute properties of BG Ind - a bright F3 system just leaving the main sequence★

Rozyczka

Kałużny

Pych

et al. 2011

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Out of the 7 class-II systems published in the SB9 catalogue, 5 were identified or suspected to have a shortperiod binary secondary (HIP 20935, 61880, 76031, 81023, 93995, see Johnson & Mayor 1986;Latham et al 2002;Jancart et al 2005;Griffin 2013), confirming our approach. One system is reported to have an equal-mass short-period binary as its primary star (HIP 108478, see Bakış et al 2010). We have found no reports of statistically significant evidence for higher multiplicity for the remaining system (HIP 62124, Griffin 2001).…”

Section: Comparison With the Sb9 Cataloguementioning

confidence: 57%

Triage of astrometric binaries – how to find triple systems and dormant black hole secondaries in the Gaia orbits

Shahaf

Mazeh

Faigler

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Preparing for the expected wealth of Gaia detections, we consider here a simple algorithm for classifying unresolved astrometric binaries with main-sequence (MS) primary into three classes: binaries with a probable MS secondary, with two possible values for the mass ratio; probable hierarchical triple MS systems with an astrometric secondary as a close binary, with a limited range of mass-ratio values; and binaries with a compact-object secondary, with a minimal value of the mass ratio. This is done by defining a unit-less observational parameter 'Astrometric Mass-Ratio Function' (AMRF), A, of a binary, based on primary-mass estimation, in addition to the astrometric parameters-the angular semi-major axis, the period and the parallax. We derive the A value that differentiates the three classes by forward modeling representative binaries of each class, assuming some mass-luminosity relation. To demonstrate the potential of the algorithm, we consider the orbits of 98 Hipparcos astrometric binaries with main-sequence primaries, using the Hipparcos parallaxes and the primarymass estimates. For systems with known spectroscopic orbital solution, our results are consistent with the spectroscopic elements, validating the suggested approach. The algorithm will be able to identify hierarchical triple systems and dormant neutron-star and black-hole companions in the Gaia astrometric binaries.

show abstract

“…First, they found that the more massive and larger star has the lower temperature 1 , thereby indicating clearly that this component has already evolved away from the main sequence and is moving toward the subgiant regime. Second, they made attempts to resolve some problems with both the photometric phasing (already first noted in van Hamme & Manfroid 1988) and discrepancies in the systemic γ velocities obtained in the solutions of the RV curves measured during three highly different epochs by Andersen et al (1984); Bakış et al (2010); Rozyczka et al (2011). However, they were not able arrive at any definitive conclusions regarding these inconsistencies.…”

mentioning

confidence: 98%

BG Ind: the nearest doubly eclipsing, compact hierarchical quadruple system

Borkovits

Rappaport

Maxted

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

BG Ind is a well studied, bright, nearby binary consisting of a pair of F stars in a 1.46-day orbit. We have discovered in the TESS lightcurve for TIC 229804573 (aka BG Ind) a second eclipsing binary in the system with a 0.53-day. Our subsequent analyses of the recent TESS and archival ground-based photometric and radial velocity data, reveal that the two binaries are gravitationally bound in a 721-day period, moderately eccentric orbit. We present the results of a joint spectro-photodynamical analysis of the eclipse timing variation curves of both binaries based on TESS and ground-based archival data, the TESS lightcurve, archival radial velocity data and the spectral energy distribution, coupled with the use of PARSEC stellar isochrones. We confirm prior studies of BG Ind which found that the brighter binary A consists of slightly evolved F-type stars with refined masses of 1.32 and 1.43 M⊙, and radii of 1.59 and 2.34 R⊙. The previously unknown binary B has two less massive stars of 0.69 and 0.64 M⊙ and radii of 0.64 and 0.61 R⊙. Based on a number of different arguments which we discuss, we conclude that the three orbital planes are likely aligned to within 17○.

show abstract

The spectroscopic orbits of three double-lined eclipsing binaries: I. BG Ind, IM Mon, RS Sgr

Cited by 8 publications

References 20 publications

Absolute properties of BG Ind - a bright F3 system just leaving the main sequence★

Absolute properties of BG Ind - a bright F3 system just leaving the main sequence★

Triage of astrometric binaries – how to find triple systems and dormant black hole secondaries in the Gaia orbits

BG Ind: the nearest doubly eclipsing, compact hierarchical quadruple system

Contact Info

Product

Resources

About