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By Allington-Smith J.

ISBN-10: 3527402896

ISBN-13: 9783527402892

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Because of its flexibility, IFS is suited 46 S. di Serego Alighieri to a large number of applications, from kinematical studies of the Galactic centre to stellar population and kinematical studies of distant galaxies (10). Also slitless spectroscopy is capable of simultaneously recording a (x,y,λ) data cube: originating from the objective prism technique, used on Schmidt telescopes for more than fifty years, it is easily implemented in modern imaging (focal reducer) spectrographs by removing the slit.

OSIRIS can perform detailed studies of the stellar content and dynamical properties of galaxies in the early Universe. In quasars, radio galaxies, and nearby active galactic nuclei, OSIRIS can elucidate the relation of the central black hole to the properties of the host galaxy, and the mechanism feeding gas into the central engine. In the center of our own Galaxy, it is possible to investigate the properties of the massive black hole and the stars in its immediate vicinity. OSIRIS can perform spectroscopic observations of young stars and their environment, and of brown dwarfs.

19 · 10−4 , while 79 percent of the signal is preserved after decorrelation. 5 Time Series Figure 4 (upper panel) shows the time series data values. Vertical lines indicate the contacts. Following Charbonneau et al. e. e. ). IFS of Transits 59 Fig. 3. Temporal variation of the index Ic . The upper panels indicate the original distribution of values. e. left: airmass; center: the 15 variables described in Table 1, excluding the airmass; and right: the 15 variables). The lower panels show the decorrelated distribution, which is obtained subtracting the fit to the original values.

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3D Instrumentation by Allington-Smith J.


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