3D Instrumentation by Allington-Smith J.

By Allington-Smith J.

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H. et al: ApJ, 639, L43 (2006) [4] Brown, M. , Calvin, W. , Terrile, R. , Brown, R. H. , Delabre, B. , Bird, M.

J. 2005b, ApJ, 622, 1149 [15] Eisenhauer, F. et al. , and Arribas, S. 2003, ISR-NICMOS-03-01, STScI [18] Le Fevre, O. et al. , Kaufer,A. , Winn, J. , Turner, E. , Leigh, C. , Schneider,J. 2000, A&A, 355, 573 [22] Sparks, W. , 2002, ApJ, 578, 543. [23] Vidal-Madjar, A. et al. 2003, Nature 422, 143 [24] Vidal-Madjar, A. et al. 2004, ApJ, 604, L69 Solar System Objects with the NACO Fabry-Perot and SINFONI M. Hartung1 , C. Dumas1 , T. M. Herbst2 , A. Coustenis3 , M. Hirtzig3,4 , ´ amkovics5 , F. Eisenhauer6 , C.

Arribas et al. g. Arribas, Mediavilla, Fuensalida, 1998; Sparks and Ford, 2002). 2 Proposed Method: The potential of IFS in observations of planet transits Here we want to highlight three main advantages of IFS when performing high S/N time series spectrophotometric observations: i) Ability to gather photons during the transit: S/N enhancement. Gilliland, Goudfrooij, and Kimble (1999) proposed to increase the photometric accuracy of very high S/N observations by using the spectroscopic mode of STIS.

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