Astrometric mass ratios for three spectroscopic binaries

Fekel, Francis C.

doi:10.1051/0004-6361/201322078

Cited by 12 publications

(12 citation statements)

References 19 publications

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“…They were fitted with five-parameter models using the orbital parameters obtained from the radial velocities, following the method described in detail by Sahlmann et al (2011). This method has proven to be reliable in detecting astrometric orbital signatures (e.g., Sahlmann et al 2011Sahlmann et al , 2013Díaz et al 2012;Wilson et al 2016). Here we detected no orbital motions.…”

Section: Methodsmentioning

confidence: 99%

The SOPHIE search for northern extrasolar planets

Hébrard

Arnold

Forveille

et al. 2016

A&A

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We present new radial velocity measurements of eight stars that were secured with the spectrograph SOPHIE at the 193 cm telescope of the Haute-Provence Observatory. The measurements allow detecting and characterizing new giant extrasolar planets. The host stars are dwarfs of spectral types between F5 and K0 and magnitudes of between 6.7 and 9.6; the planets have minimum masses M p sin i of between 0.4 to 3.8 M Jup and orbital periods of several days to several months. The data allow only single planets to be discovered around the first six stars (HD 143105, HIP 109600, HD 35759, HIP 109384, HD 220842, and HD 12484), but one of them shows the signature of an additional substellar companion in the system. The seventh star, HIP 65407, allows the discovery of two giant planets that orbit just outside the 12:5 resonance in weak mutual interaction. The last star, HD 141399, was already known to host a four-planet system; our additional data and analyses allow new constraints to be set on it. We present Keplerian orbits of all systems, together with dynamical analyses of the two multi-planet systems. HD 143105 is one of the brightest stars known to host a hot Jupiter, which could allow numerous follow-up studies to be conducted even though this is not a transiting system. The giant planets HIP 109600b, HIP 109384b, and HD 141399c are located in the habitable zone of their host star.

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Section: Methodsmentioning

confidence: 99%

The SOPHIE search for northern extrasolar planets

Hébrard

Arnold

Forveille

et al. 2016

A&A

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“…Uncertainties in the solution parameters were derived by Monte Carlo simulations, which also propagate the uncertainties in the RV parameters. This method has proven to be reliable in detecting orbital signatures in the H IAD (Sahlmann et al 2011b,a;Díaz et al 2012;Sahlmann & Fekel 2013). Table 4 lists the target names and the basic parameters of the H observations relevant for the astrometric analysis.…”

Section: Analysis Of the Hipparcos Astrometrymentioning

confidence: 99%

The SOPHIE search for northern extrasolar planets

Wilson

Hébrard

Santos

et al. 2016

A&A

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Radial velocity planet search surveys of nearby solar-type stars have shown a strong scarcity of brown dwarf companions within ∼5 AU. There is presently no comprehensive explanation for this lack of brown dwarf companions; therefore, increasing the sample of such objects is crucial to understand their formation and evolution. Based on precise radial velocities obtained using the SOPHIE spectrograph at Observatoire de Haute-Provence we characterise the orbital parameters of 15 companions to solar-type stars and constrain their true mass using astrometric data from the H space mission. The nine companions not shown to be stellar in nature have minimum masses ranging from ∼13 to 70 M Jup , and are well distributed across the planet/brown dwarf mass regime, making them an important contribution to the known population of massive companions around solar-type stars. We characterise six companions as stellar in nature with masses ranging from a minimum mass of 76 ± 4 M Jup to a mass of 0.35 ± 0.03 M . The orbital parameters of two previously known substellar candidates are improved.

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“…We search for an orbital signature in Hipparcos IAD using the methodology described in Sahlmann et al (2011b), which has been shown to reliably detect such orbital signatures in Hipparcos IAD (Sahlmann et al 2011b,a;Sahlmann & Fekel 2013). We use the spectroscopic orbital parameters given in Tab.…”

Section: Orbit Analysismentioning

confidence: 99%

Revealing Δ Cephei’s Secret Companion and Intriguing Past

Anderson

Sahlmann

Holl

et al. 2015

ApJ

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236

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Classical Cepheid variable stars are crucial calibrators of the cosmic distance scale thanks to a relation between their pulsation periods and luminosities. Their archetype, δ Cephei, is an important calibrator for this relation. In this paper, we show that δ Cephei is a spectroscopic binary based on newly-obtained highprecision radial velocities. We combine these new data with literature data to determine the orbit, which has period 2201 days, semi-amplitude 1.5 km s −1 , and high eccentricity (e = 0.647). We re-analyze Hipparcos intermediate astrometric data to measure δ Cephei's parallax ( = 4.09 ± 0.16 mas) and find tentative evidence for an orbital signature, although we cannot claim detection. We estimate that Gaia will fully determine the astrometric orbit. Using the available information from spectroscopy, velocimetry, astrometry, and Geneva stellar evolution models (M δCep ∼ 5.0 − 5.25 M ), we constrain the companion mass to within 0.2 < M 2 < 1.2 M . We discuss the potential of ongoing and previous interactions between the companion and δ Cephei near pericenter passage, informing reported observations of circumstellar material and bow-shock. The orbit may have undergone significant changes due to a Kozai-Lidov mechanism 4 Swiss National Science Foundation Fellow

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Astrometric mass ratios for three spectroscopic binaries

Cited by 12 publications

References 19 publications

The SOPHIE search for northern extrasolar planets

The SOPHIE search for northern extrasolar planets

The SOPHIE search for northern extrasolar planets

Revealing Δ Cephei’s Secret Companion and Intriguing Past

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