3D Instrumentation by Allington-Smith J.

By Allington-Smith J.

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After fourth contact). The value corresponding to the HST observations by Charbonneau et al. (2002) is shown with an open square (see text). 5-σ. 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.

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. As the fibers are brought closer together at the spectrograph slit, the smaller the spectrograph becomes, and bigger becomes the contamination problem. We have been working to determine how close together can be the fibers at the slit plane of a spectrograph, and yet have an acceptable amount of contamination.

Di Serego Alighieri most cases the data cube is largely empty. However it is exactly in these empty spaces that one can make serendipitous discoveries. Table 1. Synopsis of the techniques for 3D spectroscopy Technique Advantages IFS Simultaneous (x,y,λ) Spectral flexibility Disjoint regions possible Slitless spectr. v. Energy–res. det. Simultaneous (x,y,λ) No spectrograph Good temporal res. v. Tunable im. 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.

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