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Poster 67

Poster 67. A PHOTOMETRIC TRANSIT SEARCH FOR PLANETS AROUND COOL STARS FROM THE ITALIAN ALPS: RESULTS FROM A FEASIBILITY STUDY. A. Bernagozzi (1), E. Bertolini (1), P. Calcidese (1), M. Damasso (1), P. Giacobbe (2), M. Lattanzi (3), R. Smart (3), A. Sozzetti (3)

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Poster 67

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  1. Poster 67

  2. A PHOTOMETRIC TRANSIT SEARCH FOR PLANETS AROUND COOL STARS FROM THE ITALIAN ALPS: RESULTS FROM A FEASIBILITY STUDY A. Bernagozzi(1), E. Bertolini(1), P. Calcidese(1),M. Damasso(1), P. Giacobbe(2),M. Lattanzi(3), R. Smart (3), A. Sozzetti(3) (1) Astronomical Observatory of the Autonomous Region of the Aosta Valley, Italy (2) Dept. of Physics - University of Turin, Italy (3) INAF - Astronomical Observatory of Turin, PinoTorinese, Italy WASP-3 NEXT TO COME 24 The study demonstrates that the Astronomical Observatory of the Aosta Valley is a suitable site to conduct a photometric survey for transiting low-mass, small-size planets around a well-defined sample of M dwarfs in the Solar neighborhood. HAT-P-7 WASP-3

  3. Signatures of resonant terrestrial planets in long-period systems Gareth F. Kennedy Rosemary A. Mardling Aim: Here we examine the possibility of indirectly detecting low-mass planets by measuring the change in period of an observable Jupiter-mass planet. For the observable planet orbit parameters from HD 216770 have been used; m* = 0.9 Solar masses, mp = 0.65 Jupiter masses and eo = 0.37. The hypothetical companion planet has eccentricity of ei = 0.5 and is at a distance of δσ = -0.05 from exact 2:1 resonance. Piecewise estimates (filled circles) of the orbital period for a simulated HD 216770-type system (left) with and (right) without a 10 Earth mass companion in the interior 2:1 resonance. We conclude that it is possible to indirectly detect low mass companions using this approach as long as sampling error < δP0

  4. The Atmosphere and Auroral Emission of the Transiting Planet HD 209458b Jeffrey Linsky and Hao Yang JILA/University of Colorado Boulder Colorado Poster 15 HST/COS observing program to begin September 14, 2009. Simulations using the G130M and G160M modes. Transit, secondary eclipse, and both quadratures. Searching for wind absorption, fluorescent emission, and electron-impact auroral emission.

  5. Poster 62 Multiple aperture imaging and its application to Exo-Earth Imager • We present a spectral imaging method for double-aperture interferometers. • We introduce the application to multi-aperture (>3) interferometers. • We present a new concept for Exo-Earth imager. Only two apertures allow us to acquire a spatially resolved image of an Exo-Earth. Spectral imaging method for interferometers New concept Conventional concept New concept for Exo-Earth imager Spatial Axis Spatial Axis (u,v) Plane (u,v) Plane Spectrometer Spectral Axis Image Plane Image Plane Spatial Axis Spatial Axis Spectral Axis

  6. Poster 63 Spectral Imaging with nulling interferometer Taro Matsuo, W. A. Traub (JPL), M. Hattori (Tohoku), and M. Tamura (NAOJ) • Image of planetary system can be reconstructed from only two visibility measurements. Imaginary part of the complex visibility Reconstructed image of the planetary system • Spectra of the planets are reconstructed from a few complex visibilities, the number corresponding with that of the planets. Reconstructed spectra of the planets

  7. Poster #100 K. Haze*, K. Enya, T. Kotani, L. Abe, T. Nakagawa, S. Higuchi, T. Sato, T. Wakayama, T. Yamamuro Dark region (the raw contrast image) Dark region (the PSF subtracted image) • Background • We pursued the checkerboard pupil mask coronagraph for SPICA mission. • (Demonstration experiment using He-Ne laser in air →Enya et al, talk on Thursday） • Experiment • To improve contrast more, we installed the insulated vacuum chamber and the temperature control system. • Current status • A contrast of 1.8×10⁻⁹ was achieved using the method of the PSF subtraction in the thermally stable condition. • PSF subtraction A coronagraph experiment in a high thermal stability environment witha binary shaped pupil mask 3600sec 3600sec contrast~10⁻⁹ • Configuration of the coronagraph experiment

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