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.

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)

(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, Pino Torinese, Italy

24WASP-3

HAT-P-7The 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.

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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.

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.

We conclude that it is possible to indirectly detect low mass companions using this approach as long as sampling error < δP0

The Atmosphere and Auroral Emission of the Transiting Planet HD 209458b

Jeffrey Linsky and Hao YangJILA/University of ColoradoBoulder 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.

Multiple aperture imaging and its application to Exo-Earth Imager

Poster 62

Spectrometer

(u,v) Plane

Spatial AxisSpectral A

xis

Image Plane

Spatial Axis(u,v) Plane

Spatial AxisSpectral Axis

Image Plane

Spatial Axis

New conceptConventional concept

1. We present a spectral imaging method for double-aperture interferometers.

2. We introduce the application to multi-aperture (>3) interferometers.

3. We present a new concept for Exo-Earth imager. Only two apertures allow us to acquire a spatially resolved image of an Exo-Earth.

New concept for Exo-Earth imager

Spectral imaging method for interferometers

~δνν

B

Spectral Imaging with nulling interferometer

• Image of planetary system can be reconstructed from only two visibility measurements.

Imaginary part of the complex visibility Reconstructed image of the planetary system

Poster 63

Taro Matsuo, W. A. Traub (JPL), M. Hattori (Tohoku), and M. Tamura (NAOJ)

Reconstructed spectra of the planets

• Spectra of the planets are reconstructed from a few complex visibilities, the number corresponding with that of the planets.

Configuration of the coronagraph experiment

A coronagraph experiment in a high thermal stability environment with a binary shaped

pupil mask

Poster #100

K. Haze*, K. Enya, T. Kotani, L. Abe, T. Nakagawa, S. Higuchi, T. Sato, T. Wakayama, T. Yamamuro

3600sec 3600sec

Dark region (the raw contrast image)

Dark region (the PSF subtracted image)

PSF subtraction

BackgroundWe 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 statusA contrast of 1.8×10⁻⁹ was achieved using the method of the PSF subtraction in the thermally stable condition.

contrast~10⁻⁹