3D Instrumentation by Allington-Smith J.

By Allington-Smith J.

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These lines were scanned in steps of 1 nm for 11 nm spanning the central wavelength. Fig. 3 shows the collapsed, continuum, absorption line and difference images that are produced from the data cube. No differential CO2 ice signal is detected at sub-Earth longitudes 284W and 307W (full disk coverage). Fig. 4 demonstrates an Ariel like CO2 ice spot with a size of our PSF that would show up as 6σ detection. A detailed description of this experiment can be found in (7). No CO2 ice has been found at sub-Earth longitudes 284W and 307W, neither on a NACO spectrum taken in K-band on 15 January 2005 at 199W (9).

The present results can be improved with multi-transit observations using the recently developed new integral field spectrographs for 8m. g. GMOS: Allington-Smith et al. 2002, SINFONI/SPIFFI: Eisenhauer et al. 2003, VIMOS: Le Fevre et al. 2003). R. et al. , et al. , 1998, ApJL, 505, 43. , and G´ omez-Alvarez, P. (astro-ph/0509407 ) 62 S. Arribas et al. , and Burrows, A. M. , and Charbonneau, D. W. 2000, PASP, 112, 1421 [9] Charbonneau, D. et al. L. 2002, ApJ, 568, 377 [11] Coustenis,A. et al. in ’Brown Dwarfs and Extrasolar Planets’, Ed.

In the x-axis is the spacing between fibers. In the y-axis the FWHM. The numbers superposed to the plot show the average contamination. The smaller numbers below are the scatter in contamination measured in Monte-Carlo simulations. Fig. 3. Same as previous figure for aperture extractions. Note how contamination is much higher. OSIRIS – a New Integral-Field Spectrograph at Keck Observatory A. Quirrenbach1,2 , J. Larkin3 , M. Barczys3 , T. Gasaway2 , C. Iserlohe4 , A. Krabbe4 , M. McElwain3 , I. Song3 , J.

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