Prof Suzanne Aigrain: Publications

Stellar_flare_hits_HD_189733_b_(artist's_impression)

This artist's impression shows the hot Jupiter HD 189733b, as it passes in front of its parent star, as the latter is flaring, driving material away from the planet. The escaping atmosphere is seen silhouetted against the starlight. The surface of the star, which is around 80% the mass of the Sun, is based on observations of the Sun from NASA's Solar Dynamics Observatory.

Credit: NASA, ESA, L. Calçada, Solar Dynamics Observatory

Photospheric activity, rotation, and radial velocity variations of the planet-hosting star CoRoT-7

(2010)

Authors:

AF Lanza, AS Bonomo, C Moutou, I Pagano, S Messina, G Leto, G Cutispoto, S Aigrain, R Alonso, P Barge, M Deleuil, M Auvergne, A Baglin, A Collier Cameron

The SARS algorithm: Detrending CoRoT light curves with Sysrem using simultaneous external parameters

Monthly Notices of the Royal Astronomical Society: Letters 404:1 (2010)

Authors:

A Ofir, R Alonso, AS Bonomo, L Carone, S Carpano, B Samuel, J Weingrill, S Aigrain, M Auvergne, A Baglin, P Barge, P Borde, F Bouchy, HJ Deeg, M Deleuil, R Dvorak, A Erikson, SF Mello, M Fridlund, M Gillon, T Guillot, A Hatzes, L Jorda, H Lammer, A Leger, A Llebaria, C Moutou, M Ollivier, M Päetzold, D Queloz, H Rauer, D Rouan, J Schneider, G Wuchterl

Abstract:

Surveys for exoplanetary transits are usually limited not by photon noise but rather by the amount of red noise in their data. In particular, although the CoRoT space-based survey data are being carefully scrutinized, significant new sources of systematic noises are still being discovered. Recently, a magnitude-dependant systematic effect was discovered in the CoRoT data by Mazeh et al. and a phenomenological correction was proposed. Here we tie the observed effect to a particular type of effect, and in the process generalize the popular Sysrem algorithm to include external parameters in a simultaneous solution with the unknown effects. We show that a post-processing scheme based on this algorithm performs well and indeed allows for the detection of new transit-like signals that were not previously detected. © 2010 The Authors. Journal compilation © 2010 RAS.

Ground-based detection of thermal emission from the exoplanet WASP-19b

\mnras 404 (2010) L114-L118-L114-L118

Authors:

NP Gibson, S Aigrain, DL Pollacco, SCC Barros, L Hebb, M Hrudková, EK Simpson, I Skillen, R West

The thermal emission of the exoplanets WASP-1b and WASP-2b

(2010)

Authors:

Peter J Wheatley, Andrew Collier Cameron, Joseph Harrington, Jonathan J Fortney, James M Simpson, David R Anderson, Alexis MS Smith, Suzanne Aigrain, William I Clarkson, Michael Gillon, Carole A Haswell, Leslie Hebb, Guillaume Hébrard, Coel Hellier, Simon T Hodgkin, Keith D Horne, Stephen R Kane, Pierre FL Maxted, Andrew J Norton, Don L Pollacco, Frederic Pont, Ian Skillen, Barry Smalley, Rachel A Street, Stephane Udry, Richard G West, David M Wilson

Transiting exoplanets from the CoRoT space mission: IX. CoRoT-6b: A transiting hot Jupiter planet in an 8.9d orbit around a low-metallicity star

Astronomy and Astrophysics 512:3 (2010)

Authors:

M Fridlund, G Hébrard, R Alonso, M Deleuil, D Gandolfi, M Gillon, H Bruntt, A Alapini, S Csizmadia, T Guillot, H Lammer, S Aigrain, JM Almenara, M Auvergne, A Baglin, P Barge, P Bordé, F Bouchy, J Cabrera, L Carone, S Carpano, HJ Deeg, R De La Reza, R Dvorak, A Erikson, S Ferraz-Mello, E Guenther, P Gondoin, R Den Hartog, A Hatzes, L Jorda, A Léger, A Llebaria, P Magain, T Mazeh, C Moutou, M Ollivier, M Pätzold, D Queloz, H Rauer, D Rouan, B Samuel, J Schneider, A Shporer, B Stecklum, B Tingley, J Weingrill, G Wuchterl

Abstract:

The CoRoT satellite exoplanetary team announces its sixth transiting planet in this paper. We describe and discuss the satellite observations as well as the complementary ground-based observations-photometric and spectroscopic- carried out to assess the planetary nature of the object and determine its specific physical parameters. The discovery reported here is a "hot Jupiter" planet in an 8.9d orbit, 18 stellar radii, or 0.08 AU, away from its primary star, which is a solar-type star (F9V) with an estimated age of 3.0 Gyr. The planet mass is close to 3 times that of Jupiter. The star has a metallicity of 0.2 dex lower than the Sun, and a relatively high 7Li abundance. While the light curve indicates a much higher level of activity than, e.g., the Sun, there is no sign of activity spectroscopically in e.g., the [Ca ii] H&K lines. © ESO, 2010.

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