3D Instrumentation by Allington-Smith J.

By Allington-Smith J.

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Puech, F. Hammer et al: A&A 420, L31 (2004) A User–oriented Comparison of the Techniques for 3D Spectroscopy 49 [10] S. Gillessen, R. Davies, M. D. Kurk, A. Cimatti, S. di Serego Alighieri et al: A&A 422, L13 (2004) [12] O. Le F`evre, M. Saisse, D. Mancini et al: Proc. SPIE Vol. 4841, p. P. P. Conf. Ser. Vol. 195, p. 185 (2000) [14] M. Perryman, C. Foden, A. Peacock et al: Nuc. Inst. Meth. A 325, 319 (1993) [15] N. Pirzkal, C. Xu, S. Malhotra et al: ApJS 154, 501 (2004) The Potential of Integral Field Spectroscopy Observing Extrasolar Planet Transits S.

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. deBergh3 and A. Barucci3 M. org Max-Planck-Institut f¨ ur Astronomie, K¨ onigstuhl 17, 69117 Heidelberg, Germany LESIA, Observatoire Paris-Meudon, 92195 Meudon Cedex, France Laboratoire de Plan´etologie et G´eodynamique, 44322 Nantes, France 601 Campbell Hall, Department of Astronomy, University of California, Berkeley, CA 94720, USA Max-Planck-Institut f¨ ur extraterrestrische Physik, Giessenbachstraße, 85741 Garching, Germany Summary.

It provides a 20 field with a pixel scale of 0 . 02 and is equipped with 18 filters. The centers of the imaging and spectroscopic fields are separated by 20 . The camera is useful as a finder for faint objects, and it can perform parallel observations during spectroscopic exposures. The typical integration times of the spectrograph are sufficiently long to get good signalto-noise on “random” stars within the imager field-of-view. The imager can therefore be used for monitoring of the point spread function, and it provides fiducials for the spatial registration of individual spectroscopic data cubes.

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