Fresip: A mission to determine the character and frequency of extra-solar planets around solar-like stars

Borucki, W. J.; Dunham, E. W.; Koch, David; Cochran, William D.; Rose, J. D.; Cullers, D. K.; Granados, Arno F.; Jenkins, Jon M.

doi:10.1007/bf00644220

Cited by 38 publications

(10 citation statements)

References 33 publications

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“…The total census of transiting exoplanets is more than 2960 planets in 2223 planetary systems. Up to this date, the most successful transiting-exoplanet searcher is the Kepler space telescope (Borucki et al 1996(Borucki et al , 2004(Borucki et al , 2011, launched in 2009 and decomissioned in 2018. The Kepler and K2 missions (Howell et al 2014) together discovered 2734 confirmed transiting exoplanets.…”

Section: Introductionmentioning

confidence: 99%

Periodic transit timing variations and refined system parameters of the exoplanet XO-6b

Garai

Pribulla

Komžík

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Only a few exoplanets are known to orbit around fast rotating stars. One of them is XO-6b, which orbits an F5V-type star. Shortly after the discovery, we started multicolor photometric and radial-velocity follow-up observations of XO-6b, using the telescopes of Astronomical Institute of the Slovak Academy of Sciences. Our main scientific goals were to better characterize the planetary system and to search for transit timing variations. We refined several planetary and orbital parameters. Based on our measurements, the planet XO-6b seems to be about 10% larger, which is, however, only about 2σ difference, but its orbit inclination angle, with respect to the plane of the sky, seems to be significantly smaller, than it was determined originally by the discoverers. In this case we found about 9.5σ difference. Moreover, we observed periodic transit timing variations of XO-6b with a semi-amplitude of about 14 min and with a period of about 450 days. There are two plausible explanations of such transit timing variations: (1) a third object in the system XO-6 causing light-time effect, or (2) resonant perturbations between the transiting planet XO-6b and another unknown low-mass planet in this system. From the O-C diagram we derived that the assumed third object in the system should have a stellar mass, therefore significant variations are expected in the radial-velocity measurements of XO-6. Since this is not the case, and since all attempts to fit radial velocities and O-C data simultaneously failed to provide a consistent solution, more realistic is the second explanation.

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Section: Introductionmentioning

confidence: 99%

Periodic transit timing variations and refined system parameters of the exoplanet XO-6b

Garai

Pribulla

Komžík

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…They determined λ = 23 ± 4 deg, and I * = 138 ± 4 deg 1 , which gives the real misalignment of 56 ± 4 deg. This represents the first spin-orbit measurement obtained based on precise Kepler photometry (Borucki et al 1996(Borucki et al , 2004, although later Johnson et al (2014) obtained λ = 58 ± 2 deg via Doppler tomography, which is a significantly different value for the sky projected spin-orbit misalignment angle. Moreover, the stellar rotation of Kepler-13A is in exact 5:3 resonance with the orbital period of the substellar companion, and the long-term transit duration variation with a rate of (1.14 ± 0.30) × 10 −6 d cycle −1 is due to the precession of its orbital plane (Szabó et al 2012).…”

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confidence: 76%

Rapidly rotating stars and their transiting planets: KELT-17b, KELT-19Ab, and KELT-21b in the CHEOPS and TESS era

Garai,

Pribulla,

Kovács

et al. 2022

Preprint

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Rapidly rotating early-type main-sequence stars with transiting planets are interesting in many aspects. Unfortunately, several astrophysical effects in such systems are not well understood yet. Therefore, we performed a photometric mini-survey of three rapidly rotating stars with transiting planets, namely KELT-17b, KELT-19Ab, and KELT-21b, using the Characterising Exoplanets Satellite (CHEOPS ), complemented with Transiting Exoplanet Survey Satellite (TESS ) data, and spectroscopic data. We aimed at investigating the spin-orbit misalignment and its photometrical signs, therefore the high-quality light curves of the selected objects were tested for transit asymmetry, transit duration variations, and orbital precession. In addition, we performed transit time variation analyses, obtained new stellar parameters, and refined the system parameters. For KELT-17b and KELT-19Ab we obtained significantly smaller planet radius as found before. The gravity-darkening effect is very small compared to the precision of CHEOPS data. We can report only on a tentative detection of the stellar inclination of KELT-21, which is about 60 deg. In we were able to exclude long-term transit duration variations causing orbital precession. The shorter transit duration of KELT-19Ab compared to the discovery paper is probably a consequence of a smaller planet radius. KELT-21b is promising from this viewpoint, but further precise observations are needed. We did not find any convincing evidence for additional objects in the systems.

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“…In the case of dedicated missions, such as Kepler (Borucki et al 1996;Jenkins et al 2010), the instrument response functions are well characterised in advance and conceived to reach the required 10 -4 to10 -5 photometric precision. EChO aims at reaching the same level of photometric precision.…”

Section: Decorrelating Instrument Systematicsmentioning

confidence: 99%

The EChO science case

et al. 2015

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The discovery of almost two thousand exoplanets has revealed an unexpectedly diverse planet population. We see gas giants in few-day orbits, whole multi-planet systems within the orbit of Mercury, and new populations of planets with masses between that of the Earth and Neptune-all unknown in the Solar System. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? How do planetary systems work and what causes the exceptional diversity observed as compared to the Solar System? The EChO (Exoplanet Characterisation Observatory) space mission was conceived to take up the challenge to explain this diversity in terms of formation, evolution, internal structure and planet and atmospheric composition. This requires in-depth spectroscopic knowledge of the atmospheres of a large and well-defined planet sample for which precise physical, chemical and dynamical information can be obtained. In order to fulfil this ambitious scientific program, EChO was designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large, diverse and well-defined planet sample within its 4-year mission lifetime. The transit and eclipse spectroscopy method, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allows us to measure atmospheric signals from the planet at levels of at least 10 −4 relative to the star. This can only be achieved in conjunction with a carefully designed stable payload and satellite platform. It is also necessary to provide broad instantaneous wavelength coverage to detect as many molecular species as possible, to probe the thermal structure of the planetary atmospheres and to correct for the contaminating effects of the stellar photosphere. This requires wavelength coverage of at least 0.55 to 11 μm with a goal of covering from 0.4 to 16 μm. Only modest spectral resolving power is needed, with R~300 for wavelengths less than 5 μm and R~30 for wavelengths greater than this. spectroscopy technique means that no spatial resolution is required. A telescope collecting area of about 1 m 2 is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 m 2 telescope, diffraction limited at 3 μm has been adopted. Placing the satellite at L2 provides a cold and stable thermal environment as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. EChO has been conceived to achieve a single goal: exoplanet spectroscopy. The spectral coverage and signal-to-noise to be achieved by EChO, thanks to its high stability and dedicated design, would be a game changer by allowing atmospheric composition to be measured with unparalleled exactness: at least a factor 10 more precise and a factor 10 to 1000 more accurate tha...

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Fresip: A mission to determine the character and frequency of extra-solar planets around solar-like stars

Cited by 38 publications

References 33 publications

Periodic transit timing variations and refined system parameters of the exoplanet XO-6b

Periodic transit timing variations and refined system parameters of the exoplanet XO-6b

Rapidly rotating stars and their transiting planets: KELT-17b, KELT-19Ab, and KELT-21b in the CHEOPS and TESS era

The EChO science case

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