By Allington-Smith J.

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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. 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.

V. Good spectral res. v. Galactic centre, distant galaxies, etc. v. Under development Rapid variables Optical pulsars 2D field not covered Prior imaging Mask preparation Scanning in λ Variable central λ Scanning required High sky background Heavy computations Scanning required Large redshift surveys Nearby galaxies Nebulae Galactic centre Very elongated objects References [1] J. Allington–Smith, G. Murray, R. Content et al: PASP 114, 892 (2002) [2] R. Bacon, Y. Copin, G. L. P. Conf. Ser. Vol. 195, p.

Ferrari5 1 2 3 4 5 Dep. br Integral Field Unit (IFU) spectrographs allow continuous space coverage of a small part of the sky by using a microlens array at the telescope focal plane. Each microlens images the telescope pupil onto an optical fiber, which is in turn taken to a bench spectrograph. A larger number of microlenses allows for higher spatial coverage and/or spatial resolution. A larger number of fibers also implies in larger spectrographs, this means higher costs and higher telescope payloads.

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