The value-added catalogue of ASAS-SN eclipsing binaries – II. Properties of extra-physics systems

Rowan, D. M.; Jayasinghe, T.; Stanek, K. Z.; Kochanek, C. S.; Thompson, Todd A.; Shappee, B. J.; Holoien, T. W. S.; Prieto, J. L.; Giles, W.

doi:10.1093/mnras/stad021

Cited by 5 publications

(2 citation statements)

References 114 publications

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“…Two of them have outer orbits reported by Gaia, but no third body eclipses were reported by Gaia. One of the systems, TIC 185615681, was included in the Rowan et al (2023) list of mutlistellar systems tabulated from ASAS-SN data, and studied for the apsidal motion of its inner binary by Zasche (2012) and Kim et al (2018), as well as for RVs by Duerbeck & Rucinski (2007). (a) Where available, we show for each source, the period, eccentricity, and argument of periastron of the outer orbit, separated by semicolons.…”

Section: Objectmentioning

confidence: 99%

Seven new triply eclipsing triple star systems

Rappaport,

Borkovits,

Mitnyan

et al. 2024

A&A

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We have identified nearly a hundred close triply eclipsing hierarchical triple star systems from data taken with the space telescope TESS. These systems are noteworthy in that we can potentially determine their dynamical and astrophysical parameters with a high precision. In the present paper, we report the comprehensive study of seven new compact triply eclipsing triple star systems taken from this larger sample: TICs 133771812, 176713425, 185615681, 287756035, 321978218, 323486857, and 650024463. Most of the data for this study come from TESS observations, but two of them have Gaia measurements of their outer orbits, and we obtained supplemental radial velocity (RV) measurements for three of the systems. The eclipse timing variation curves extracted from the TESS data, the photometric light curves, the RV points, and the spectral energy distribution (SED) are combined in a complex photodynamical analysis to yield the stellar and orbital parameters of all seven systems. Four of the systems are quite compact with outer periods in the range of 41-56 days. All of the systems are substantially flat, with mutual inclination angles of $ Including the systems reported in this work, we have now studied in considerable detail some 30 triply eclipsing triples with TESS, and are accumulating a meaningful census of these systems.

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Section: Objectmentioning

confidence: 99%

Seven new triply eclipsing triple star systems

Rappaport,

Borkovits,

Mitnyan

et al. 2024

A&A

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“…In total, TESS short cadence or K2 light curves are available for 150 stars, that is 82.9% of the programme stars; missing stars are in areas not covered by TESS or K2, still mostly in Upper Scorpius. None of the programme stars is in the Gaia EB catalogue (Mowlavi et al 2023), in the Gaia DR2 variability catalogue (Gaia Collaboration 2019), and in the ASAS detached eclipsing variable catalogue (Rowan et al 2023) because they are too bright. Light variations for HIP 67464 (ν Cen: listed as EB in SIMBAD) and HIP 76297 (γ Lup) are likely caused by the reflection effects of the light from the B-star on the companion, but there is no real eclipse as shown by the analysis of Jerzykiewicz et al (2021).…”

Section: Eclipsing Binariesmentioning

confidence: 99%

Multiples among B stars in the Scorpius-Centaurus association

Gratton,

Squicciarini,

Nascimbeni

et al. 2023

A&A

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Context. The frequency, semi-major axis, and mass distribution of stellar companions likely depend on the mass of the primaries and on the environment where the stars form. These properties are very different for early- and late-type stars. However, data are largely incomplete, even for the closest environments to the Sun, preventing a cleaner view of the problem. Aims. This paper provides basic information about the properties of companions to B stars in the Scorpius-Centaurus association (age ∼ 15 Myr); this is the closest association containing a large population of 181 B-stars. Methods. We gathered available data combining high contrast imaging samples from BEAST, SHINE, and previous surveys with evidence of companions from Gaia (both through direct detection and astrometry), from eclipsing binaries, and from spectroscopy. We evaluated the completeness of the binary search and estimated the mass and semi-major axis for all detected companions. These data provide a complete sample of stellar secondaries (extending well in the substellar regime) for separation> 3 au, and they are highly informative as to closer companions. Results. We found evidence for 200 companions around 181 stars. We did not find evidence for companions for only 43 (23.8 ± 3.6%) of the targets, with the fraction being as low as 15.2 ± 4.1% for stars with MA > 3.5 M⊙ while it is 31.5 ± 5.9% for lower-mass stars. This confirms earlier findings for a clear trend of a binary fraction with stellar mass. The median semi-major axis of the orbits of the companions is smaller for B than in A stars, confirming a turn-over previously found for OB stars. The mass distribution of the very wide (a > 1000 au) and closer companions is different. Very few companions of massive stars MA > 5.0 M⊙ have a mass below solar and even fewer are M stars with a semi-major axis < 1000 au. However, the scarcity of low-mass companions extends throughout the whole sample. Period and mass ratio distributions are different for early B stars (up to B7 spectral type) and stars of a later spectral type: most early B stars are in compact systems with massive secondaries, while less massive stars are mainly in wider systems with a larger spread in mass ratios. We derived log-normal fits to the distribution of the semi-major axis and mass ratios for low and high-mass B stars; these relations suggest that it is not probable that the planets and brown dwarf (BD) companions to b Cen and μ2 Sco are extreme cases in the distribution of stellar companions. Conclusions. We interpret our results as the formation of secondaries with a semi-major axis < 1000 au (about 80% of the total) by fragmentation of the disk of the primary and selective mass accretion on the secondaries. The formation of secondaries within the disk of primaries in close binaries has been proposed by many others before; it unifies the scenarios for formation of close binaries with that of substellar companions that also form within the primary disk, though on a different timescale. We also find that the observed trends with primary mass may be explained by a more prolonged phase of accretion episodes on the disk and by a more effective inward migration. Finally, in the Appendices we describe the detection of twelve new stellar companions from the BEAST survey and of a new BD companion at 9.599 arcsec from HIP 74752 using Gaia data, and we discuss the cases of possible BD and low-mass stellar companions to HIP 59173, HIP 62058, and HIP 64053.

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The value-added catalogue of ASAS-SN eclipsing binaries – III. Masses and radii of Gaia spectroscopic binaries

Rowan

Jayasinghe

Stanek

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Masses and radii of stars can be derived by combining eclipsing binary light curves with spectroscopic orbits. In our previous work, we modeled the All-Sky Automated Survey for Supernovae (ASAS-SN) light curves of more than 30,000 detached eclipsing binaries using PHOEBE. Here we combine our results with 128 double-lined spectroscopic orbits from Gaia Data Release 3. We also visually inspect ASAS-SN light curves of the Gaia double-lined spectroscopic binaries on the lower main sequence and the giant branch, adding 11 binaries to our sample. We find that only 50% of systems have Gaia periods and eccentricities consistent with the ASAS-SN values. We use emcee and PHOEBE to determine masses and radii for a total of 122 stars with median fractional uncertainties of 7.9% and 6.3%, respectively.

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The value-added catalogue of ASAS-SN eclipsing binaries – II. Properties of extra-physics systems

Cited by 5 publications

References 114 publications

Seven new triply eclipsing triple star systems

Seven new triply eclipsing triple star systems

Multiples among B stars in the Scorpius-Centaurus association

The value-added catalogue of ASAS-SN eclipsing binaries – III. Masses and radii of Gaia spectroscopic binaries

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