Cosmic Shear from STIS Pure Parallels: Analysis

The measurement of cosmic shear requires deep imaging with high image quality on many lines of sight to sample the statistics of large-scale structure. The expected distortion of galaxy images by cosmic shear on the STIS angular scale is a few percent, therefore the PSF anisotropy has to be understood and controlled to an accuracy better than 1%. In this poster we present the analysis of the PSF of STIS and a preliminary cosmic shear measurement using archival data from the STIS pure parallel program to show that the STIS camera on-board HST is well suited for our project. The data reduction and catalog production are described in an accompanying paper (astro-ph/0102330).Comment: 4 pages, 5 figures, to appear in the proceedings of the STScI 2001 spring symposium "The Dark Universe: Matter, Energy and Gravity" Baltimore April 2-5 2001, acknowledgements adde

Glanmor (J. Cuillandre). — Mouez an Aochou (La voix des Grèves). — Poésies bretonnes accompagnées de leur traduction française et de plusieurs mélodies populaires

Loth J. Glanmor (J. Cuillandre). — Mouez an Aochou (La voix des Grèves). — Poésies bretonnes accompagnées de leur traduction française et de plusieurs mélodies populaires. In: Annales de Bretagne. Tome 19, numéro 4, 1903. pp. 637-639

Glanmor (J. Cuillandre). —Mouez an Aochou(La voix des Grèves). — Poésies bretonnes accompagnées de leur traduction française et de plusieurs mélodies populaires

Loth J. Glanmor (J. Cuillandre). —Mouez an Aochou(La voix des Grèves). — Poésies bretonnes accompagnées de leur traduction française et de plusieurs mélodies populaires. In: Annales de Bretagne. Tome 19, numéro 4, 1903. pp. 637-639

Retour sur l'arrêt Meissonnier : le « bail fiscal » existe-t-il ?

International audienceBIC. BA. BNC. Frais et charges. Loyer d'un immeuble versé par l'entreprise individuelle à l'exploitant. (Rép. n° 40698 à M. Cuillandre, JOAN 3 avr. 2000, p. 2188, BF Lefebvre 5-2000, n° 505 ; Rép. n° 53346 à M. Jacquat, JOANQ 5 mars 2001, p. 1394, Dr. fisc. 2001, n° 24, p. 893 ; CE, 9e et 10e s.-sect., 6 avr. 2001, Prince, RJF 7-2001, n° 939, Chron. J. Maïa, p. 703

Retour sur l'arrêt Meissonnier : le « bail fiscal » existe-t-il ?

International audienceBIC. BA. BNC. Frais et charges. Loyer d'un immeuble versé par l'entreprise individuelle à l'exploitant. (Rép. n° 40698 à M. Cuillandre, JOAN 3 avr. 2000, p. 2188, BF Lefebvre 5-2000, n° 505 ; Rép. n° 53346 à M. Jacquat, JOANQ 5 mars 2001, p. 1394, Dr. fisc. 2001, n° 24, p. 893 ; CE, 9e et 10e s.-sect., 6 avr. 2001, Prince, RJF 7-2001, n° 939, Chron. J. Maïa, p. 703

Brown Dwarfs and Mass Function of Young Open Clusters

International audienceThe initial mass function is an important key to understand star formation processes. It is still very badly known in the substellar field and its determination is one of the principal motivations to search for brown dwarfs. I will present the results of photometric large field surveys of various clusters of similar age (Pleiades, NGC 2516 and Blanco1). The surveys of Pleiades and Blanco 1 have been carried out with the CFH-12K camera and allow to identify more than 50 candidates brown dwarfs from 0.07Msun to 0.03Msun for each cluster. NGC 2516, the twin of Pleiades in the southern hemisphere, has been observed with the ESO WFI camera and more than 100 candidate brown dwarfs have been identified in 2 square degrees. On the basis of these observations, I will present the initial mass function obtained for each cluster and I will discuss to what extent the dynamic evolution of the clusters could affect these estimates

Brown Dwarfs and Mass Function of Young Open Clusters

International audienceThe initial mass function is an important key to understand star formation processes. It is still very badly known in the substellar field and its determination is one of the principal motivations to search for brown dwarfs. I will present the results of photometric large field surveys of various clusters of similar age (Pleiades, NGC 2516 and Blanco1). The surveys of Pleiades and Blanco 1 have been carried out with the CFH-12K camera and allow to identify more than 50 candidates brown dwarfs from 0.07Msun to 0.03Msun for each cluster. NGC 2516, the twin of Pleiades in the southern hemisphere, has been observed with the ESO WFI camera and more than 100 candidate brown dwarfs have been identified in 2 square degrees. On the basis of these observations, I will present the initial mass function obtained for each cluster and I will discuss to what extent the dynamic evolution of the clusters could affect these estimates