Characterization of the planetary system Kepler-101 with HARPS-N

Bonomo, A. S.; Sozzetti, A.; Lovis, C.; Malavolta, L.; Rice, Ken; Buchhave, Lars A.; Sasselov, Dimitar; Cameron, A. Collier; Latham, David W.; Molinari, E.; Pepe, F.; Udry, S.; Affer, L.; Charbonneau, David; Cosentino, R.; Dressing, Courtney D.; Dumusque, X.; Figueira, P.; Fiorenzano, A. F. Martínez; Gettel, Sara; Harutyunyan, A.; Haywood, R. D.; Horne, K.; López-Morales, M.; Mayor, M.; Micela, G.; Motalebi, F.; Nascimbeni, V.; Phillips, David F.; Piotto, G.; Pollacco, D.; Queloz, D.; Ségransan, D.; Szentgyorgyi, Andrew; Watson, C. A.

doi:10.1051/0004-6361/201424617

Cited by 42 publications

(40 citation statements)

References 51 publications

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“…HARPS-N is an ultra-stable fiber-fed high-resolution (R=115,000) spectrograph with an optical wavelength coverage from 383 to 693 nm, designed specifically to provide precise radial velocities. The instrument has significantly improved our understanding of small transiting planets with several precise mass measurements of transiting planets (Pepe et al 2013;Bonomo et al 2014;Dumusque et al 2014;López-Morales et al 2014;Gettel et al 2016). We obtained 61 and 64 observations of Kepler-20 in the 2014 and 2015 observing seasons, respectively (125 observations in total).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

A 1.9 Earth Radius Rocky Planet and the Discovery of a Non-Transiting Planet in the Kepler-20 System*

Buchhave

Dressing

Dumusque

et al. 2016

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Kepler-20 is a solar-type star (V = 12.5) hosting a compact system of five transiting planets, all packed within the orbital distance of Mercury in our own solar system. A transition from rocky to gaseous planets with a planetary transition radius of ∼1.6 Å R has recently been proposed by several articles in the literature. Kepler-20b (R p ∼1.9 Å R ) has a size beyond this transition radius; however, previous mass measurements were not sufficiently precise to allow definite conclusions to be drawn regarding its composition. We present new mass measurements of three of the planets in the Kepler-20 system that are facilitated by 104 radial velocity measurements from the HARPS-N spectrograph and 30 archival Keck/HIRES observations, as well as an updated photometric analysis of the Kepler data and an asteroseismic analysis of the host star

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Section: Observations and Data Reductionmentioning

confidence: 99%

A 1.9 Earth Radius Rocky Planet and the Discovery of a Non-Transiting Planet in the Kepler-20 System*

Buchhave

Dressing

Dumusque

et al. 2016

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“…The semi-amplitudes of these signals, however, cannot be inferred by the frequentist analysis alone, since an offset in RV between the data taken before and after 2012 September may exist due to the failure of the first CCD of HARPS-N (see Bonomo et al 2014). The value of this offset cannot be determined a priori, even when observations of RV standard stars are available, since it may depend primarily on the spectral type of the star (i.e., the two CCDs may have a different efficiency as a function of wavelength).…”

Section: Rv Analysismentioning

confidence: 99%

The Kepler-19 System: A Thick-envelope Super-Earth with Two Neptune-mass Companions Characterized Using Radial Velocities and Transit Timing Variations

Malavolta

Borsato

Granata

et al. 2017

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We report a detailed characterization of the Kepler-19 system. This star was previously known to host a transiting planet with a period of 9.29 days, a radius of 2.2 R ⊕ , and an upper limit on the mass of 20 M ⊕ . The presence of a second, non-transiting planet was inferred from the transit time variations (TTVs) of Kepler-19b over eight quarters of Kepler photometry, although neither the mass nor period could be determined. By combining new TTVs measurements from all the Kepler quarters and 91 high-precision radial velocities obtained with the HARPS-N spectrograph, using dynamical simulations we obtained a mass of 8.4±1.6 M ⊕ for . From the same data, assuming system coplanarity, we determined an orbital period of 28.7 days and a mass of 13.1±2.7 M ⊕ for Kepler-19c and discovered a Neptune-like planet with a mass of 20.3±3.4 M ⊕ on a 63-day orbit. By comparing dynamical simulations with non-interacting Keplerian orbits, we concluded that neglecting interactions between planets may lead to systematic errors that can hamper the precision in the orbital parameters when the data set spans several years. With a density of 4.32±0.87 g cm −3 (0.78±0.16 ρ ⊕ ) Kepler-19b belongs to the group of planets with a rocky core and a significant fraction of volatiles, in opposition to low-density planets characterized only by transit time variations and an increasing number of rocky planets with Earth-like density. Kepler-19 joins the small number of systems that reconcile transit timing variation and radial velocity measurements.

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“…on different CCDs each season. To account for the widening of the ingress and egress durations (Kipping 2010), we modeled the LC light-curves using an oversampling factor of 10 suitable to the Kepler data (Bonomo et al 2014). We fitted the free parameters using a Metropolis-Hasting Markov chain Monte Carlo (MCMC) algorithm (e.g., Tegmark et al 2004) with an adaptive step size (Ford 2006).…”

Section: Photometry Analysismentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Bourrier

Étangs

Hébrard

et al. 2015

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We present the detection and characterization of the transiting warm Jupiter KOI-12b, first identified with Kepler with an orbital period of 17.86 days. We combine the analysis of Kepler photometry with Doppler spectroscopy and line-profile tomography of timeseries spectra obtained with the SOPHIE spectrograph to establish its planetary nature and derive its properties. To derive reliable estimates for the uncertainties on the tomographic model parameters, we devised an empirical method of calculating statistically independent error bars on the time-series spectra. KOI-12b has a radius of 1.43 ± 0.13 R Jup and a 3σ upper mass limit of 10 M Jup . It orbits a fast-rotating star (v sin i = 60.0 ± 0.9 km s −1 ) with mass and radius of 1.45 ± 0.09 M and 1.63 ± 0.15 R , located at 426 ± 40 pc from the Earth. Doppler tomography allowed higher precision on the obliquity to be reached by comparison with analysis of the Rossiter-McLaughlin radial velocity anomaly, and we find that KOI-12b lies on a prograde, slightly misaligned orbit with low sky-projected obliquity λ = 12.6 +3.0 −2.9• . The properties of this planetary system, with a 11.4 mag host star, make of KOI-12b a precious target for future atmospheric characterization.

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Characterization of the planetary system Kepler-101 with HARPS-N

Cited by 42 publications

References 51 publications

A 1.9 Earth Radius Rocky Planet and the Discovery of a Non-Transiting Planet in the Kepler-20 System*

A 1.9 Earth Radius Rocky Planet and the Discovery of a Non-Transiting Planet in the Kepler-20 System*

The Kepler-19 System: A Thick-envelope Super-Earth with Two Neptune-mass Companions Characterized Using Radial Velocities and Transit Timing Variations

SOPHIE velocimetry ofKeplertransit candidates

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