T A Lister

Publications (104)162.86 Total impact

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  Available from: F. Faedi

  Article: WASP-52b, WASP-58b, WASP-59b, and WASP-60b: four new transiting close-in giant planets

  G. Hebrard, A. Collier Cameron, D. J. A. Brown, R. F. Diaz, F. Faedi, B. Smalley, D. R. Anderson, D. Armstrong, S. C. C. Barros, J. Bento, [......], A. Santerne, I. Skillen, J. Southworth, J. Tregloan-Reed, A. H. M. J. Triaud, S. Udry, M. Vanhuysse, C. A. Watson, R. G. West, P. J. Wheatley
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  ABSTRACT: We present the discovery of four new transiting hot jupiters, detected mainly from SuperWASP-North and SOPHIE observations. These new planets, WASP-52b, WASP-58b, WASP-59b, and WASP-60b, have orbital periods ranging from 1.7 to 7.9 days, masses between 0.46 and 0.94 M_Jup, and radii between 0.73 and 1.49 R_Jup. Their G1 to K5 dwarf host stars have V magnitudes in the range 11.7-13.0. The depths of the transits are between 0.6 and 2.7%, depending on the target. With their large radii, WASP-52b and 58b are new cases of low-density, inflated planets, whereas WASP-59b is likely to have a large, dense core. WASP-60 shows shallow transits. In the case of WASP-52 we also detected the Rossiter-McLaughlin anomaly via time-resolved spectroscopy of a transit. We measured the sky-projected obliquity lambda = 24 (+17/-9) degrees, indicating that WASP-52b orbits in the same direction as its host star is rotating and that this prograde orbit is slightly misaligned with the stellar equator. These four new planetary systems increase our statistics on hot jupiters, and provide new targets for follow-up studies.
  11/2012;
• Article: A brown dwarf orbiting an M-dwarf: MOA 2009-BLG-411L

  E Bachelet, P Fouqué, C Han, A Gould, M ~D Albrow, J -P Beaulieu, E Bertin, I ~A Bond, G ~W Christie, D Heyrovský, [......], G Maier, L Mancini, S Rahvar, D Ricci, G Scarpetta, J Skottfelt, J Southworth, J Surdej, F Zimmer, Mindstep Consortium
  Astronomy and Astrophysics 11/2012; 547:A55. · 4.59 Impact Factor
• Article: WASP-42 b and WASP-49 b: two new transiting sub-Jupiters

  M. Lendl, D. R. Anderson, A. Collier-Cameron, A. P. Doyle, M. Gillon, C. Hellier, E. Jehin, T. A. Lister, P. F. L. Maxted, F. Pepe, D. Pollacco, D. Queloz, B. Smalley, D. Segransan, A. M. S. Smith, A. H. M. J. Triaud, S. Udry, R. G. West, P. J. Wheatley
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  ABSTRACT: We report the discovery of two new transiting planets from the WASP survey. WASP-42 b is a 0.500 +/- 0.035 M_jup planet orbiting a K1 star at a separation of 0.0548 +/- 0.0017 AU with a period of 4.9816872 +/- 7.3 x 10^-6 days. The radius of WASP-42 b is 1.080 +/- 0.057 R_jup while its equilibrium temperature is T_eq = 995 +/- 34 K. We detect some evidence for a small but non-zero eccentricity of e=0.060 +/- 0.013. WASP-49 b is a 0.378 +/- 0.027 M_jup planet around an old G6 star. It has a period of 2.7817387 +/- 5.6 x 10^-6 days and a separation of 0.0379 +/- 0.0011 AU. This planet is slightly bloated, having a radius of 1.115 +/- 0.047 R_jup and an equilibrium temperature of T_eq = 1369 +/- 39 K. Both planets have been followed up photometrically, and in total we have obtained 5 full and one partial transit light curves of WASP-42 and 4 full and one partial light curves of WASP-49 using the Euler-Swiss, TRAPPIST and Faulkes South telescopes.
  05/2012;
• Article: WASP-35b, WASP-48b, and HAT-P-30b/WASP-51b: Two New Planets and an Independent Discovery of a Hat Planet

  B. Enoch, D. R. Anderson, S. C. C. Barros, D. J. A. Brown, A. Collier Cameron, F. Faedi, M. Gillon, G. Hébrard, T. A. Lister, D. Queloz, [......], A. J. Norton, N. Parley, F. Pepe, D. Pollacco, D. Segransan, E. Simpson, I. Skillen, A. M. S. Smith, S. Udry, and P. J. Wheatley
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  ABSTRACT: We report the detection of WASP-35b, a planet transiting a metal-poor ([Fe/H] = –0.15) star in the Southern hemisphere, WASP-48b, an inflated planet which may have spun-up its slightly evolved host star of 1.75 R ☉ in the Northern hemisphere, and the independent discovery of HAT-P-30b/WASP-51b, a new planet in the Northern hemisphere. Using WASP, RISE, Faulkes Telescope South, and TRAPPIST photometry, with CORALIE, SOPHIE, and NOT spectroscopy, we determine that WASP-35b has a mass of 0.72 ± 0.06 MJ and radius of 1.32 ± 0.05RJ , and orbits with a period of 3.16 days, WASP-48b has a mass of 0.98 ± 0.09 MJ , radius of 1.67 ± 0.10 RJ , and orbits in 2.14 days, while HAT-P-30b/WASP-51b, with an orbital period of 2.81 days, is found to have a mass of 0.76 ± 0.05 MJ and radius of 1.42 ± 0.03 RJ , agreeing with values of 0.71 ± 0.03 MJ and 1.34 ± 0.07 RJ reported for HAT-P-30b.
  The Astronomical Journal 08/2011; 142(3):86. · 4.03 Impact Factor
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  Available from: S. C. C. Barros

  Article: SuperWASP observations of pulsating Am stars

  B. Smalley, D. W. Kurtz, A. M. S. Smith, L. Fossati, D. R. Anderson, S. C. C. Barros, O. W. Butters, A. Collier Cameron, D. J. Christian, B. Enoch, [......], A. J. Norton, N. Parley, D. Pollacco, E. K. Simpson, I. Skillen, J. Southworth, R. A. Street, R. G. West, P. J. Wheatley, P. L. Wood
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  ABSTRACT: We have studied over 1600 Am stars at a photometric precision of 1 mmag with SuperWASP photometric data. Contrary to previous belief, we find that around 200 Am stars are pulsating delta Sct and gamma Dor stars, with low amplitudes that have been missed in previous, less extensive studies. While the amplitudes are generally low, the presence of pulsation in Am stars places a strong constraint on atmospheric convection, and may require the pulsation to be laminar. While some pulsating Am stars have been previously found to be delta Sct stars, the vast majority of Am stars known to pulsate are presented in this paper. They will form the basis of future statistical studies of pulsation in the presence of atomic diffusion.
  07/2011;
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  Available from: Amaury H. M. J. Triaud

  Article: WASP-35b, WASP-48b and WASP-51b: Two new planets and an independent discovery of HAT-P-30b

  B. Enoch, D. R. Anderson, S. C. C. Barros, D. J. A. Brown, A. Collier Cameron, F. Faedi, M. Gillon, G. Hébrard, T A Lister, D. Queloz, [......], A. J. Norton, N. Parley, F. Pepe, D. Pollacco, D. Segransan, E Simpson, I. Skillen, A. M. S. Smith, S. Udry, P. J. Wheatley
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  ABSTRACT: We report the detection of WASP-35b, a planet transiting a metal-poor ([Fe/H] = -0.15) star in the Southern hemisphere, WASP-48b, an inflated planet which may have spun-up its slightly evolved host star of 1.75 R_sun in the Northern hemisphere, and the independent discovery of HAT-P-30b / WASP-51b, a new planet in the Northern hemisphere. Using WASP, RISE, FTS and TRAPPIST photometry, with CORALIE, SOPHIE and NOT spectroscopy, we determine that WASP-35b has a mass of 0.72 +/- 0.06 M_J and radius of 1.32 +/- 0.03 R_J, and orbits with a period of 3.16 days, WASP-48b has a mass of 0.98 +/- 0.09 M_J, radius of 1.67 +/- 0.08 R_J and orbits in 2.14 days, while WASP-51b, with an orbital period of 2.81 days, is found to have a mass of 0.76 +/- 0.05 M_J and radius of 1.42 +/- 0.04 R_J, agreeing with values of 0.71 +/- 0.03 M_J and 1.34 +/- 0.07 R_J reported for HAT-P-30b.
  04/2011;
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  Available from: Elaine Kathryn Simpson

  Article: Independent Discovery of the Transiting Exoplanet HAT-P-14b

  E. K. Simpson, S. C. C. Barros, D. J. A. Brown, A. Collier Cameron, D. Pollacco, I. Skillen, H. C. Stempels, I. Boisse, F. Faedi, G. Hébrard, [......], C. Moutou, A. J. Norton, N. Parley, A. Santerne, B. Smalley, A. M. S. Smith, I. Todd, C. A. Watson, R. G. West, and P. J. Wheatley
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  ABSTRACT: We present SuperWASP observations of HAT-P-14b, a hot Jupiter discovered by Torres et al. The planet was found independently by the SuperWASP team and named WASP-27b after follow-up observations had secured the discovery, but prior to the publication by Torres et al. Our analysis of HAT-P-14/WASP-27 is in good agreement with the values found by Torres et al. and we provide additional evidence against astronomical false positives. Due to the brightness of the host star, V mag = 10, HAT-P-14b is an attractive candidate for further characterization observations. The planet has a high impact parameter and the primary transit is close to grazing. This could readily reveal small deviations in the orbital parameters indicating the presence of a third body in the system, which may be causing the small but significant orbital eccentricity. Our results suggest that the planet may undergo a grazing secondary eclipse. However, even a non-detection would tightly constrain the system parameters.
  The Astronomical Journal 04/2011; 141(5):161. · 4.03 Impact Factor
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  Available from: Amaury H. M. J. Triaud

  Article: WASP-39b: a highly inflated Saturn-mass planet orbiting a late G-type star

  F. Faedi, S. C. C. Barros, D. R. Anderson, D. J. A. Brown, A. Collier Cameron, D. Pollacco, I. Boisse, G. Hebrard, M. Lendl, T A Lister, [......], A. J. Norton, D. Queloz, A. Santerne, E. K. Simpson, I. Skillen, A. M. S. Smith, S. Udry, C. A. Watson, R. G. West, P. J. Wheatley
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  ABSTRACT: We present the discovery of WASP-39b, a highly inflated transiting Saturn-mass planet orbiting a late G-type dwarf star with a period of $4.055259 \pm 0.000008$\,d, Transit Epoch T$_{0}=2455342.9688\pm0.0002$\,(HJD), of duration $0.1168 \pm 0.0008$\,d. A combined analysis of the WASP photometry, high-precision follow-up transit photometry, and radial velocities yield a planetary mass of $\mpl=0.28\pm0.03\,\mj$ and a radius of $\rpl=1.27\pm0.04\,\rj$, resulting in a mean density of $0.14 \pm 0.02\,\rhoj$. The stellar parameters are mass $\mstar = 0.93 \pm 0.03\,\msun$, radius $\rstar = 0.895\pm 0.23\,\rsun$, and age $9^{+3}_{-4}$\,Gyr. Only WASP-17b and WASP-31b have lower densities than WASP-39b, although they are slightly more massive and highly irradiated planets. From our spectral analysis, the metallicity of WASP-39 is measured to be \feh\,$= -0.12\pm0.1$\,dex, and we find the planet to have an equilibrium temperature of $1116^{+33}_{-32}$\,K\,. Both values strengthen the observed empirical correlation between these parameters and the planetary radius for the known transiting Saturn-mass planets.
  02/2011;
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  Available from: ArXiv

  Article: Stellar rotation in the Hyades and Praesepe: gyrochronology and braking timescale

  P. Delorme, A. Collier Cameron, L. Hebb, J. Rostron, T A Lister, A. J. Norton, D. Pollacco, R. G. West
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  ABSTRACT: We present the results of photometric surveys for stellar rotation in the Hyades and in Praesepe, using data obtained as part of the SuperWASP exoplanetary transit-search programme.We determined accurate rotation periods for more than 120 sources whose cluster membership was confirmed by common proper motion and colour-magnitude fits to the clusters' isochrones. This allowed us to determine the effect of magnetic braking on a wide range of spectral types for expected ages of ~600Myr for the Hyades and Praesepe. Both clusters show a tight and nearly linear relation between J - Ks colour and rotation period in the F,G and K spectral range. This confirms that loss of angular momentum was significant enough that stars with strongly different initial rotation rates have converged to the same rotation period for a given mass, by the age of Hyades and Praesepe. In the case of the Hyades our colour-period sequence extends well into the M dwarf regime and shows a steep increase in the scatter of the colour- period relation, with identification of numerous rapid rotators from 0.5SM down to the lowest masses probed by our survey (0.25SM). This provides crucial constraints on the rotational braking timescales and further clears the way to use gyrochronology as an accurate age measurement tool for main-sequence stars.
  01/2011;
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  Available from: S. C. C. Barros

  Article: Short period eclipsing binary candidates identified using SuperWASP

  A. J. Norton, S. G. Payne, T. Evans, R. G. West, P. J. Wheatley, D. R. Anderson, S. C. C. Barros, O. W. Butters, A. Collier Cameron, D. J. Christian, [......], K. D. Horne, T A Lister, P. F. L. Maxted, N. Parley, D. Pollacco, E. K. Simpson, I. Skillen, B. Smalley, J. Southworth, R. A. Street
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  ABSTRACT: We present light curves and periods of 53 candidates for short period eclipsing binary stars identified by SuperWASP. These include 48 newly identified objects with periods <2x10^4 seconds (~0.23d), as well as the shortest period binary known with main sequence components (GSC2314-0530 = 1SWASP J022050.85+332047.6) and four other previously known W UMa stars (although the previously reported periods for two of these four are shown to be incorrect). The period distribution of main sequence contact binaries shows a sharp cut-off at a lower limit of around 0.22d, but until now, very few systems were known close to this limit. These new candidates will therefore be important for understanding the evolution of low mass stars and to allow investigation of the cause of the period cut-off.
  01/2011;
• Article: WASP-30b: A 61 M Jup Brown Dwarf Transiting a V = 12, F8 Star

  D. R. Anderson, A. Collier Cameron, C. Hellier, M. Lendl, P. F. L. Maxted, D. Pollacco, D. Queloz, B. Smalley, A. M. S. Smith, I. Todd, A. H. M. J. Triaud, R. G. West, S. C. C. Barros, B. Enoch, M. Gillon, T. A. Lister, F. Pepe, D. Ségransan, R. A. Street, and S. Udry
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  ABSTRACT: We report the discovery of a 61-Jupiter-mass brown dwarf (BD), which transits its F8V host star, WASP-30, every 4.16 days. From a range of age indicators we estimate the system age to be 1-2 Gyr. We derive a radius (0.89 ± 0.02 R Jup) for the companion that is consistent with that predicted (0.914 R Jup) by a model of a 1 Gyr old, non-irradiated BD with a dusty atmosphere. The location of WASP-30b in the minimum of the mass-radius relation is consistent with the quantitative prediction of Chabrier & Baraffe, thus confirming the theory.
  The Astrophysical Journal Letters 12/2010; 726(2):L19. · 5.53 Impact Factor
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  Available from: Amaury H. M. J. Triaud

  Article: WASP-41b: A transiting hot Jupiter planet orbiting a magnetically-active G8V star

  P. F. L. Maxted, D. R. Anderson, A. Collier Cameron, C. Hellier, D. Queloz, B. Smalley, R. A. Street, A. H. M. J. Triaud, R. G. West, M. Gillon, T A Lister, F. Pepe, D. Pollacco, D. Segransan, A. M. S. Smith, S. Udry
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  ABSTRACT: We report the discovery of a transiting planet with an orbital period of 3.05d orbiting the star TYC 7247-587-1. The star, WASP-41, is a moderately bright G8V star (V=11.6) with a metallicity close to solar ([Fe/H]=-0.08+-0.09). The star shows evidence of moderate chromospheric activity, both from emission in the cores of the CaII H and K lines and photometric variability with a period of 18.4d and an amplitude of about 1%. We use a new method to show quantitatively that this periodic signal has a low false alarm probability. The rotation period of the star implies a gyrochronological age for WASP-41 of 1.8Gyr with an error of about 15%. We have used a combined analysis of the available photometric and spectroscopic data to derive the mass and radius of the planet (0.92+-0.06M_Jup, 1.20+-0.06R_Jup). Further observations of WASP-41 can be used to explore the connections between the properties of hot Jupiter planets and thelevel of chromospheric activity in their host stars.
  12/2010;
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  Available from: Amaury H. M. J. Triaud

  Article: WASP-34b: a near-grazing transiting sub-Jupiter-mass exoplanet in a hierarchical triple system

  B. Smalley, D. R. Anderson, A. Collier Cameron, C. Hellier, M. Lendl, P. F. L. Maxted, D. Queloz, A. H. M. J. Triaud, R. G. West, S. J. Bentley, [......], T A Lister, F. Pepe, D. Pollacco, D. Segransan, A. M. S. Smith, J. Southworth, S. Udry, P. J. Wheatley, P. L. Wood, J. Bento
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  ABSTRACT: We report the discovery of WASP-34b, a sub-Jupiter-mass exoplanet transiting its 10.4-magnitude solar-type host star (1SWASP J110135.89-235138.4; TYC 6636-540-1) every 4.3177 days in a slightly eccentric orbit (e = 0.038 +/- 0.012). We find a planetary mass of 0.59 +/- 0.01 M_Jup and radius of 1.22 ^{+0.11}_{-0.08} R_Jup. There is a linear trend in the radial velocities of 55+/-4 m/s/y indicating the presence of a long-period third body in the system with a mass > 0.45 M_Jup at a distance of >1.2 AU from the host star. This third-body is either a low-mass star, white dwarf, or another planet. The transit depth ((R_P/R_*)^2 = 0.0126) and high impact parameter (b = 0.90) suggest that this could be the first known transiting exoplanet expected to undergo grazing transits, but with a confidence of only ~80%. Comment: 5 pages, 6 figures, accepted on 9 December 2010 by A&A Main Journal, Section 10. Planets and planetary systems
  12/2010;
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  Available from: Amaury H. M. J. Triaud

  Article: The WASP-South search for transiting exoplanets

  Coel Hellier, D. R. Anderson, A. Collier Cameron, M. Gillon, M. Lendl, T A Lister, P. F. L. Maxted, D. Pollacco, D. Queloz, B. Smalley, A. H. M. J. Triaud, R. G. West
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  ABSTRACT: Since 2006 WASP-South has been scanning the Southern sky for transiting exoplanets. Combined with Geneva Observatory radial velocities we have so far found over 30 transiting exoplanets around relatively bright stars of magnitude 9--13. We present a status report for this ongoing survey. Comment: To appear in the proceedings of the OHP conference "Detection and dynamics of transiting exoplanets", 23-27th August 2010
  12/2010;
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  Available from: F. Faedi

  Article: WASP-37b: A 1.8 M J Exoplanet Transiting a Metal-poor Star

  E. K. Simpson, F. Faedi, S. C. C. Barros, D. J. A. Brown, A. Collier Cameron, L. Hebb, D. Pollacco, B. Smalley, I. Todd, O. W. Butters, [......], N. Parley, F. Pepe, D. Queloz, D. Segransan, A. M. S. Smith, H. C. Stempels, S. Udry, C. A. Watson, R. G. West, and P. J. Wheatley
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  ABSTRACT: We report on the discovery of WASP-37b, a transiting hot Jupiter orbiting an m v = 12.7 G2-type dwarf, with a period of 3.577469 ± 0.000011 d, transit epoch T 0 = 2455338.6188 ± 0.0006 (HJD; dates throughout the paper are given in Coordinated Universal Time (UTC)), and a transit duration 0.1304+0.0018 –0.0017 d. The planetary companion has a mass M p = 1.80 ± 0.17 M J and radius R p = 1.16+0.07 –0.06 R J, yielding a mean density of 1.15+0.12 –0.15 ρJ. From a spectral analysis, we find that the host star has M = 0.925 ± 0.120 M ☉, R = 1.003 ± 0.053 R ☉, T eff = 5800 ± 150 K, and [Fe/H] = –0.40 ± 0.12. WASP-37 is therefore one of the lowest metallicity stars to host a transiting planet.
  The Astronomical Journal 12/2010; 141(1):8. · 4.03 Impact Factor
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  Available from: Amaury H. M. J. Triaud

  Article: WASP-31b: a low-density planet transiting a metal-poor, late-F-type dwarf star

  D. R. Anderson, A. Collier Cameron, C. Hellier, M. Lendl, T. A. Lister, P. F. L. Maxted, D. Queloz, B. Smalley, A. M. S. Smith, A. H. M. J. Triaud, R. G. West, D. J. A. Brown, M. Gillon, F. Pepe, D. Pollacco, D. Segransan, R. A. Street, S. Udry
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  ABSTRACT: We report the discovery of the low-density, transiting giant planet WASP-31b. The planet is 0.48 Jupiter masses and 1.55 Jupiter radii. It is in a 3.4-day orbit around a metal-poor, late-F-type, V = 11.7 dwarf star, which is a member of a common proper motion pair. In terms of its low density, WASP-31b is second only to WASP-17b, which is a more highly irradiated planet of similar mass.
  11/2010;
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  Available from: Amaury H. M. J. Triaud

  Article: WASP-30b: a 61 Mjup brown dwarf transiting a V=12, F8 star

  D. R. Anderson, A. Collier Cameron, C. Hellier, M. Lendl, P. F. L. Maxted, D. Pollacco, D. Queloz, B. Smalley, A. M. S. Smith, I. Todd, A. H. M. J. Triaud, R. G. West, S. C. C. Barros, B. Enoch, M. Gillon, T A Lister, F. Pepe, D. Ségransan, R. A. Street, S. Udry
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  ABSTRACT: We report the discovery of a 61-Jupiter-mass brown dwarf, which transits its F8V, rotationally-synchronised host star, WASP-30, every 4.16 days. From a range of age indicators, we estimate the system age to be 1-2 Gyr. We derive a radius (0.89 \pm 0.02 RJup) for the companion that is consistent with that predicted (0.914 RJup) by a model of a 1-Gyr-old, non-irradiated brown dwarf with a dusty atmosphere. Comment: submitted to ApJL: 6 pages, 3 figures, 2 tables
  10/2010;
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  Available from: Damien Ségransan

  Article: WASP-29b: A Saturn-sized Transiting Exoplanet

  Coel Hellier, D. R. Anderson, A. Collier Cameron, M. Gillon, M. Lendl, P. F. L. Maxted, D. Queloz, B. Smalley, A. H. M. J. Triaud, R. G. West, D. J. A. Brown, B. Enoch, T. A. Lister, F. Pepe, D. Pollacco, D. Ségransan, and S. Udry
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  ABSTRACT: We report the discovery of a Saturn-sized planet transiting a V = 11.3, K4 dwarf star every 3.9 days. WASP-29b has a mass of 0.24 ± 0.02 M Jup and a radius of 0.79 ± 0.05 R Jup, making it the smallest planet so far discovered by the WASP survey, and the exoplanet most similar in mass and radius to Saturn. The host star WASP-29 has an above-solar metallicity and fits a possible correlation for Saturn-mass planets such that planets with higher-metallicity host stars have higher core masses and thus smaller radii.
  The Astrophysical Journal Letters 10/2010; 723(1):L60. · 5.53 Impact Factor
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  Available from: Amaury H. M. J. Triaud

  Article: WASP-32b: A transiting hot Jupiter planet orbiting a lithium-poor, solar-type star

  P. F. L. Maxted, D. R. Anderson, A. Collier Cameron, M. Gillon, C. Hellier, D. Queloz, B. Smalley, A. H. M. J. Triaud, R. G. West, R. Enoch, T A Lister, F. Pepe, D. L. Pollacco, D. Ségransan, I. Skillen, S. Udry
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  ABSTRACT: We report the discovery of a transiting planet orbiting the star TYC 2-1155-1. The star, WASP-32, is a moderately bright (V=11.3) solar-type star (Teff=6100 +- 100K, [Fe/H] = -0.13 +- 0.10). The lightcurve of the star obtained with the WASP-South and WASP-North instruments shows periodic transit-like features with a depth of about 1% and a duration of 0.10d every 2.72d. The presence of a transit-like feature in the lightcurve is confirmed using z-band photometry obtained with Faulkes Telescope North. High resolution spectroscopy obtained with the CORALIE spectrograph confirms the presence of a planetary mass companion. From a combined analysis of the spectroscopic and photometric data, assuming that the star is a typical main-sequence star, we estimate that the planet has a mass M_p = 3.60 +- 0.07 M_Jup and a radius R_p = 1.19 +- 0.06R_Jup. WASP-32 is one of a small group of hot Jupiters with masses M_p > 3M_Jup. We find that some stars with hot Jupiter companions and with masses M_* =~ 1.2M_sun, including WASP-32, are depleted in lithium, but that the majority of these stars have similar lithium abundances to field stars. Comment: Accepted for publication in PASP
  10/2010;
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  Available from: S. C. C. Barros

  Article: WASP-38b: A Transiting Exoplanet in an Eccentric, 6.87d Period Orbit

  S. C. C. Barros, F. Faedi, A. Collier Cameron, T A Lister, J. McCormac, D. Pollacco, E. K. Simpson, B. Smalley, R. A. Street, I. Todd, [......], C. Hellier, F. P. Keenan, G. R. M. Miller, V. Moulds, A. J. Norton, N. Parley, I. Skillen, C. A. Watson, R. G. West, P. J. Wheatley
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  ABSTRACT: We report the discovery of WASP-38b, a long period transiting planet in an eccentric 6.871815 day orbit. The transit epoch is 2455335.92050 +/- 0.00074 (HJD) and the transit duration is 4.663 hours. WASP-38b's discovery was enabled due to an upgrade to the SuperWASP-North cameras. We performed a spectral analysis of the host star HD 146389/BD+10 2980 that yielded Teff = 6150 +/- 80K, logg =4.3 +/- 0.1, vsini=8.6 +/- 0.4 km/s, M*=1.16 +/- 0.04 Msun and R* =1.33 +/- 0.03 Rsun, consistent with a dwarf of spectral type F8. Assuming a main-sequence mass-radius relation for the star, we fitted simultaneously the radial velocity variations and the transit light curves to estimate the orbital and planetary parameters. The planet has a mass of 2.69 +/- 0.06 Mjup and a radius of 1.09 +/-0.03 Rjup giving a density, rho_p = 2.1 +/-0.1 rho_jup. The high precision of the eccentricity e=0.0314 +/- 0.0044 is due to the relative transit timing from the light curves and the RV shape. The planet equilibrium temperature is estimated at 1292 +/- 33K. WASP-38b is the longest period planet found by SuperWASP-North and with a bright host star (V =9.4 mag), is a good candidate for followup atmospheric studies. Comment: 7 pages, 4 figures, A&A in press
  10/2010;