Bright Southern Variable Stars in the bRing Survey

Mellon, Samuel N.; Mamajek, Eric E.; Stuik, Remko; Zwintz, K.; Kenworthy, Matthew A.; Talens, G. J. J.; Burggraaff, Olivier; Bailey, John I.; Dorval, Patrick; Lomberg, Blaine; Kuhn, Rudolf B.; Ireland, Michael

doi:10.3847/1538-4365/ab3662

Cited by 5 publications

(4 citation statements)

References 76 publications

(112 reference statements)

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“…• HD 156623: based on observations with the bRing robotic observatory network, Mellon et al 91 found frequencies in the range 60-70 d −1 and suggested regularity at three different separations: 3.75, 7.25, and 2.75d −1 . This star was observed by TESS in sector 12 and shows a pattern similar to other stars in our sample, with a spacing of ∆ν = 7.31 d −1 .…”

Section: Additional References and Notesmentioning

confidence: 99%

Very regular high-frequency pulsation modes in young intermediate-mass stars

Bedding

Murphy

Hey

et al. 2020

Nature

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Section: Additional References and Notesmentioning

confidence: 99%

Very regular high-frequency pulsation modes in young intermediate-mass stars

Bedding

Murphy

Hey

et al. 2020

Nature

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“…This allows the combination of data between the two bRing stations and the southern MASCARA station. Further discussion on the systematic errors encountered by the bRing stations can be found in Mellon et al (2019c).…”

Section: Mascara Bring and Discovery Observationsmentioning

confidence: 99%

MASCARA-4 b/bRing-1 b: A retrograde hot Jupiter around a bright A-type star

Dorval

Talens

Otten

et al. 2020

A&A

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Context. The Multi-site All-Sky CAmeRA (MASCARA) and bRing are both photometric ground-based instruments with multiple stations that rely on interline charge-coupled devices with wide-field lenses to monitor bright stars in the local sky for variability. MASCARA has already discovered several planets in the northern sky, which are among the brightest known transiting hot Jupiter systems. Aims. In this paper, we aim to characterize a transiting planetary candidate in the southern skies found in the combined MASCARA and bRing data sets of HD 85628, an A7V star of V = 8.2 mag at a distance 172 pc, to establish its planetary nature. Methods. The candidate was originally detected in data obtained jointly with the MASCARA and bRing instruments using a Box Least-Square search for transit events. Further photometry was taken by the 0.7 m Chilean-Hungarian Automated Telescope (CHAT), and radial velocity measurements with the Fiber Dual Echelle Optical Spectrograph on the European Southern Observatory 1.0 m Telescope. High-resolution spectra during a transit were taken with the CTIO high-resolution spectrometer (CHIRON) on the Small and Moderate Aperture Research Telescope System 1.5 m telescope to target the Doppler shadow of the candidate. Results. We confirm the existence of a hot Jupiter transiting the bright A7V star HD 85628, which we co-designate as MASCARA-4b and bRing-1b. It is in an orbit of 2.824 days, with an estimated planet radius of 1.53−0.04+0.07 RJup and an estimated planet mass of 3.1 ± 0.9 MJup, putting it well within the planetary regime. The CHAT observations show a partial transit, reducing the probability that the transit was around a faint background star. The CHIRON observations show a clear Doppler shadow, implying that the transiting object is in a retrograde orbit with |λ| =244.9−3.6+2.7°. The planet orbits at a distance of 0.047 ± 0.004 AU from the star and has a zero-albedo equilibrium temperature of 2100 ± 100 K. In addition, we find that HD 85628 has a previously unreported stellar companion star in the Gaia DR2 data demonstrating common proper motion and parallax at 4.3′′ separation (projected separation ~740 AU), and with absolute magnitude consistent with being a K/M dwarf. Conclusions. MASCARA-4 b/bRing-1 b is the brightest transiting hot Jupiter known to date in a retrograde orbit. It further confirms that planets in near-polar and retrograde orbits are more common around early-type stars. Due to its high apparent brightness and short orbital period, the system is particularly well suited for further atmospheric characterization.

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“…The MASCARA survey utilises two stations, located in the northern and southern hemisphere, to search for transiting exoplanets. For this purpose, it obtains continuous, high-cadence observations of the brightest stars in the sky (4 < V < 8.4), and such observations are also very well-suited for use in variable star studies (Mellon et al 2019). HD 27130 passes over the east, west and zenith pointing cameras of the northern MASCARA station and we use data obtained between February 2015 and August 2018.…”

Section: Photometric Observations With Mascaramentioning

confidence: 99%

Properties of the Hyades, the eclipsing binary HD 27130, and the oscillating red giant ϵ Tauri

Brogaard

Pakštienė

Grundahl

et al. 2020

A&A

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Context. The derivation of accurate and precise masses and radii is possible for eclipsing binary stars, allowing for insights into their evolution. When residing in star clusters, they provide measurements of even greater precision, along with additional information on their properties. Asteroseismic investigations of solar-like oscillations offers similar possibilities for single stars. Aims. We wish to improve the previously established properties of the Hyades eclipsing binary HD 27130 and re-assess the asteroseismic properties of the giant star ϵ Tau. The physical properties of these members of the Hyades can be used to constrain the helium content and age of the cluster. Methods. New multi-colour light curves were combined with multi-epoch radial velocities to yield masses and radii of HD 27130. Measurements of Teff were derived from spectroscopy and photometry, and verified using the Gaia parallax. We estimated the cluster age from re-evaluated asteroseismic properties of ϵ Tau while using HD 27130 to constrain the helium content. Results. The masses, radii, and Teff of HD 27130 were found to be M = 1.0245 ± 0.0024 M⊙, R = 0.9226 ± 0.015 R⊙, Teff = 5650 ± 50 K for the primary, and M = 0.7426 ± 0.0016 M⊙, R = 0.7388 ± 0.026 R⊙, Teff = 4300 ± 100 K for the secondary component. Our re-evaluation of ϵ Tau suggests that the previous literature estimates are trustworthy and that the HIPPARCOS parallax is more reliable than the Gaia DR2 parallax. Conclusions. The helium content of HD 27130 and, thus, of the Hyades is found to be Y = 0.27 but with a significant model dependency. Correlations with the adopted metallicity result in a robust helium enrichment law, with ΔY/ΔZ close to 1.2 We estimate the age of the Hyades to be 0.9 ± 0.1 (stat) ±0.1 (sys) Gyr, which is in slight tension with recent age estimates based on the cluster white dwarfs. The precision of the age estimate can be much improved via asteroseismic investigations of the other Hyades giants and by future improvements to the Gaia parallax for bright stars.

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Bright Southern Variable Stars in the bRing Survey

Cited by 5 publications

References 76 publications

Very regular high-frequency pulsation modes in young intermediate-mass stars

Very regular high-frequency pulsation modes in young intermediate-mass stars

MASCARA-4 b/bRing-1 b: A retrograde hot Jupiter around a bright A-type star

Properties of the Hyades, the eclipsing binary HD 27130, and the oscillating red giant ϵ Tauri

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