Using genotyping-by-sequencing to understand Musa diversity

Poster presented at Plant and Animal Genome, PAG XXII. San Diego (USA), 11-15 Jan 201

Maximum-likelihood models for mapping genetic markers showing segregation distortion : 2. F2 populations

Dans la génération F2, la sélection naturelle des gamètes et des zygotes peut affecter les linkages génétiques. Une équation mathématique qui prend toutes les probabibilités de linkage en compte est développée. L'intégration des marqueurs génétiques dominants et codominants permet d'obtenir une courbe de probabilité asymptotique. La comparaison de l'utilité et de la précision des modèles montre que la prise en compte des marqueurs dominants seuls ne donne pas assez d'information sur le cas de distorsions de ségrégation. L'estimation de la fraction de recombinaisons entre les marqueurs codominants est peu affectée par la sélection, ce qui n'est pas le cas pour les marqueurs dominant

The HARPS search for southern extra-solar planets XXXV. Planetary systems and stellar activity of the M dwarfs GJ 3293, GJ 3341, and GJ 3543

Context. Planetary companions of a fixed mass induce larger amplitude reflex motions around lower-mass stars, which helps make M dwarfs excellent targets for extra-solar planet searches. State of the art velocimeters with $\sim$1m/s stability can detect very low-mass planets out to the habitable zone of these stars. Low-mass, small, planets are abundant around M dwarfs, and most known potentially habitable planets orbit one of these cool stars. Aims. Our M-dwarf radial velocity monitoring with HARPS on the ESO 3.6m telescope at La Silla observatory makes a major contribution to this sample. Methods. We present here dense radial velocity (RV) time series for three M dwarfs observed over $\sim5$ years: GJ 3293 (0.42M$_\odot$), GJ 3341 (0.47M$_\odot$), and GJ 3543 (0.45M$_\odot$). We extract those RVs through minimum $\chi^2$ matching of each spectrum against a high S/N ratio stack of all observed spectra for the same star. We then vet potential orbital signals against several stellar activity indicators, to disentangle the Keplerian variations induced by planets from the spurious signals which result from rotational modulation of stellar surface inhomogeneities and from activity cycles. Results. Two Neptune-mass planets - $msin(i)=1.4\pm0.1$ and $1.3\pm0.1M_{nept}$ - orbit GJ 3293 with periods $P=30.60\pm0.02$ d and $P=123.98\pm0.38$ d, possibly together with a super-Earth - $msin(i)\sim7.9\pm1.4M_\oplus$ - with period $P=48.14\pm0.12\;d$. A super-Earth - $msin(i)\sim6.1M_\oplus$ - orbits GJ 3341 with $P=14.207\pm0.007\;d$. The RV variations of GJ 3543, on the other hand, reflect its stellar activity rather than planetary signals.Comment: Accepted for publication in A&A, 19 pages, 12 figures, 7 table

Characterization of the hot Neptune GJ 436b with Spitzer and ground-based observations

We present Spitzer Space Telescope infrared photometry of a secondary eclipse of the hot Neptune GJ436b. The observations were obtained using the 8-micron band of the InfraRed Array Camera (IRAC). The data spanning the predicted time of secondary eclipse show a clear flux decrement with the expected shape and duration. The observed eclipse depth of 0.58 mmag allows us to estimate a blackbody brightness temperature of T_p = 717 +- 35 K at 8 microns. We compare this infrared flux measurement to a model of the planetary thermal emission, and show that this model reproduces properly the observed flux decrement. The timing of the secondary eclipse confirms the non-zero orbital eccentricity of the planet, while also increasing its precision (e = 0.14 +- 0.01). Additional new spectroscopic and photometric observations allow us to estimate the rotational period of the star and to assess the potential presence of another planet.Comment: Accepted for publication in A&A on 11/09/2007; 7 pages, 6 figure

Maximum-likelihood models for mapping genetic markers showing segregation distortion : 1. Backcross populations

Une approche du maximum de vraisemblance est utilisée pour estimer les fréquences de recombinaison entre des marqueurs présentant des distorsions de ségrégation dans des populations backcross. L'hypothèse faite ici est que les distorsions sont induites par des différences de viabilité entre gamètes ou zygotes dues à la présence d'un ou plusieurs allèles contre-sélectionnés. Nous montrons que l'estimateur de Bailey (1949) reste convergent donc efficace sous des conditions plus générales que celles définies par son auteur. Cet estimateur devrait donc être utilisé à la place de l'estimateur classique du maximum de vraisemblance. La question de la détection d'une liaison peut être affectée par les distorsions de ségrégation. (Résumé d'auteur

The SOPHIE search for northern extrasolar planets VIII. A warm Neptune orbiting HD164595

High-precision radial velocity surveys explore the population of low-mass exoplanets orbiting bright stars. This allows accurately deriving their orbital parameters such as their occurrence rate and the statistical distribution of their properties. Based on this, models of planetary formation and evolution can be constrained. The SOPHIE spectrograph has been continuously improved in past years, and thanks to an appropriate correction of systematic instrumental drift, it is now reaching 2 m/s precision in radial velocity measurements on all timescales. As part of a dedicated radial velocity survey devoted to search for low-mass planets around a sample of 190 bright solar-type stars in the northern hemisphere, we report the detection of a warm Neptune with a minimum mass of 16.1 +- 2.7 Mearth orbiting the solar analog HD164595 in 40 +- 0.24 days . We also revised the parameters of the multiplanetary system around HD190360. We discuss this new detection in the context of the upcoming space mission CHEOPS, which is devoted to a transit search of bright stars harboring known exoplanets.Comment: 11 pages, 9 figure