![]() Kasper: High angular resolution detection of β Pictoris b at 2.18 mm. Astronomy and Astrophysics 525, id.A11 (2011)īonnefoy, M., A. Dullemond: Dust size distributions in coagulation/fragmentation equilibrium: numerical solutions and analytical fits. ![]() Dupuy: A Keck LGS AO search for brown dwarf and planetary mass companions to Upper Scorpius brown dwarfs. Astronomy and Astrophysics 531, id.A26, (2011)īiller, B., K. Kim: High-mass star formation at high luminosities: W31 at > 10 6 L sun. Astronomy and Astrophysics 533, id.A17 (2011)īeuther, H., H. Astronomy and Astrophysics 528, id.A134 (2011)īeuther, H., J. L‘-band observations of the three outer planets. Henning: VLT/NACO astrometry of the HR 8799 planetary system. Astronomy and Astrophysics 531, id.A84, (2011)īergfors, C., W. Weigelt: A low optical depth region in the inner disk of the Herbig Ae star HR 5999. Astronomy and Astrophysics 532, id.A91, (2011)īenisty, M., S. Codella: Molecular outflows and hot molecular cores in G24.78+0.08 at sub-arcsecond angular resolution. Bailer-Jones: The substellar population of ο Orionis: A deep wide survey. Zhang: Black hole mass estimates based on C IV are consistent with those based on the Balmer lines. Celestial Mechanics and Dynamical Astronomy 110, 401-403 (2011)Īssef, R. Williams: Erratum to: Reports of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2006 & 2009. Targets, proper motions, and first results. Teixeira: Parallaxes of Southern Extremely Cool Objects. Astronomy and Astrophysics 526, id.A63, (2011)Īndrei, A. Formation of planets around stars of different masses. Benz: Extrasolar planet population synthesis. Henning: UV-controlled physical and chemical structure of protoplanetary disks. Astronomy and Astrophysics 535, id.A68 (2011)Īkimkin, V. Traub: Searching for faint companions with VLTI/PIONIER. An accuracy of 3e-4 pixel was obtained for the relative positions of artificial stars and we have determined that measures of pixel positions by the metrology is currently limited by stray light.Absil, O., J. ![]() I am going to present the testbed itself, the data analysis methods and the results. The second aspect of the PhD is relative to the testbed, which mimics the NEAT telescope configuration. Regarding the scientific case, I compiled a catalog of mission target stars and reference stars (needed for the differential astrometric measurements) and I estimated the scientific return of NEAT-like missions in terms of number of detected exoplanets and their parameter distributions. During my PhD, my activities were related to astrophysical aspects as well as instrumental aspects of the mission. A laboratory testbed called NEAT-demo was assembled at IPAG, its main goal is to demonstrate CCD detector calibration to the required accuracy. A mission called NEAT (Nearby Earth Astrometric Telescope) has been proposed to ESA in 2010. A scientific consortium has formed to promote this kind of astrometric space mission. Finding habitable Earths in the Solar neighborhood would be a major step forward for exoplanet detection and these planets would be prime targets for attempting to find life outside of the Solar System, by searching for bio-markers in their atmospheres. From space, it is possible to use differential astrometry around nearby Solar-type stars to detect exoplanets down to one Earth mass in habitable zone, where the sensitivity of the technique is optimal. This technique is used frequently and is very successful to determine the masses and the orbits of binary stars. Astrometry, by measuring the reflex effect of planets on their central host stars, lead us to the mass of planets and to their orbit determination. With the present state of exoplanet detection techniques, none of the rocky planets of the Solar System would be discovered, yet their presence is a very strong constraint on the scenarios of formation of planetary systems.
0 Comments
Leave a Reply. |