Chemical abundances for the transiting planet host stars OGLE-TR-10, 56, 111, 113, 132, and TrES-1

Santos, N. C.; Ecuvillon, A.; Israelian, G.; Mayor, M.; Melo, C.; Queloz, D.; Udry, S.; Ribeiro, José Pancrácio; Jorge, Sílvia

doi:10.1051/0004-6361:20065683

Cited by 31 publications

(25 citation statements)

References 43 publications

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“…Our derived distances are listed in Table 4, available electronically from the CDS, and are generally within 2σ of the previously reported values. Notably different distances are those for WASP-66 and WASP-67, for which we find 520±30 pc and 184 ± 6 pc respectively, compared to 380 ± 100 and 255 ± 45 given by Hellier et al (2012); WASP-90, which we find to be at 211 ± 10 compared to 340 ± 60 by West et al (2016); and OGLE-TR-113, which we place at 358±19 pc, much closer than the previously reported distances of 600 pc by Konacki et al (2004) and 553 pc by Santos et al (2006).…”

Section: Host Star Distancessupporting

confidence: 57%

High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)

Evans

Southworth

Maxted

et al. 2016

A&A

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Context. Wide binaries are a potential pathway for the formation of hot Jupiters. The binary fraction among host stars is an important discriminator between competing formation theories, but has not been well characterised. Additionally, contaminating light from unresolved stars can significantly affect the accuracy of photometric and spectroscopic measurements in studies of transiting exoplanets. Aims. We observed 101 transiting exoplanet host systems in the Southern hemisphere in order to create a homogeneous catalogue of both bound companion stars and contaminating background stars, in an area of the sky where transiting exoplanetary systems have not been systematically searched for stellar companions. We investigate the binary fraction among the host stars in order to test theories for the formation of hot Jupiters. Methods. Lucky imaging observations from the Two Colour Instrument on the Danish 1.54 m telescope at La Silla were used to search for previously unresolved stars at small angular separations. The separations and relative magnitudes of all detected stars were measured. For 12 candidate companions to 10 host stars, previous astrometric measurements were used to evaluate how likely the companions are to be physically associated. Results. We provide measurements of 499 candidate companions within 20 arcsec of our sample of 101 planet host stars. 51 candidates are located within 5 arcsec of a host star, and we provide the first published measurements for 27 of these. Calibrations for the plate scale and colour performance of the Two Colour Instrument are presented. Conclusions. We find that the overall multiplicity rate of the host stars is 38 +17 −13 %, consistent with the rate among solar-type stars in our sensitivity range, suggesting that planet formation does not preferentially occur in long period binaries compared to a random sample of field stars. Long period stellar companions (P > 10 yr) appear to occur independently of short period companions, and so the population of close-in stellar companions is unconstrained by our study.

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Section: Host Star Distancessupporting

confidence: 57%

High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)

Evans

Southworth

Maxted

et al. 2016

A&A

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“…1 we show the comparison of the observed H α line profile in an archival Keck/HIRES spectrum against four synthetic profiles for solar-metallicity dwarfs ([Fe/H] = 0.0, log g = 4.5) from the Kurucz database. As is well-known, the H α line is very sensitive to changes in T eff , while relatively insensitive to changes in log g and [Fe/H] (see, e.g., Santos et al 2006;Sozzetti et al 2007, and references therein), thus this exercise helps to test the accuracy of the spectroscopic T eff derived above. The results shown in Fig.…”

Section: Spectroscopic Analysismentioning

confidence: 92%

Characterization of the HD 17156 planetary system

Barbieri¹,

Alonso²,

Desidera

et al. 2009

A&A

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Aims. We present data to improve the known parameters of the HD 17156 system (peculiar due to the eccentricity and long orbital period of its transiting planet) and constrain the presence of stellar companions. Methods. Photometric data were acquired for 4 transits, and high precision radial velocity measurements were simultaneously acquired with the SARG spectrograph at TNG for one transit. The template spectra of HD 17156 was used to derive effective temperature, gravity, and metallicity. A fit of the photometric and spectroscopic data was performed to measure the stellar and planetary radii, and the spin-orbit alignment. Planet orbital elements and ephemeris were derived from the fit. Near infrared adaptive optic images were acquired with the AdOpt module of TNG. Results. We found that the star has a radius of R S = 1.44 ± 0.03 R and the planet R P = 1.02 ± 0.08 R J . The transit ephemeris is T c = 2 454 756.73134 ± 0.00020 + N · 21.21663 ± 0.00045 BJD. Analysis of the Rossiter-Mclaughlin effect shows that the system is spin orbit aligned with an angle β = 4.8 • ± 5.3 • . The analysis of high resolution images did not reveal any stellar companion with a projected separation between of 150 and 1 000 AU from HD 17156.

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“…Abundances for silicon (alpha-element) and nickel (ironpeak element) were derived using the methodology and atomic line lists described in Gilli et al (2006) and Santos et al (2006), and are listed in Table 2. Analysis of these two elements was performed because they have several well defined lines in the spectra of solar type stars, and because they do not present any strong dependence of derived abundance with effective temperature (Bodaghee et al 2003;Gilli et al 2006).…”

Section: Stellar Parameters and Chemical Abundancesmentioning

confidence: 99%

Chemical abundances in six nearby star-forming regions

Santos¹,

Melo

James

et al. 2008

A&A

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In this paper we present a study of chemical abundances in six star-forming regions. Stellar parameters and metallicities are derived using high-resolution, high S/N spectra of weak-line T-Tauri stars in each region. The results show that nearby star-forming regions have a very small abundance dispersion (only 0.033 dex in [Fe/H]). The average metallicity found is slightly below that of the Sun, although compatible with solar once the errors are taken into account. The derived abundances for Si and Ni show that the observed stars have the abundances typical of Galactic thin disk stars of the same metallicity. The impact of these observations is briefly discussed in the context of the Galactic chemical evolution, local inter-stellar medium abundances, and in the origin of metal-rich stars in the solar neighbourhood (namely, stars more likely to harbour planets). The implication for future planet-search programmes around very young, nearby stars is also discussed.

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Chemical abundances for the transiting planet host stars OGLE-TR-10, 56, 111, 113, 132, and TrES-1

Cited by 31 publications

References 43 publications

High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)

High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)

Characterization of the HD 17156 planetary system

Chemical abundances in six nearby star-forming regions

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