By Evencio Mediavilla, Santiago Arribas, Martin Roth, Jordi Cepa-Nogué, Francisco Sánchez
At the same time storing either spectral and spatial info, 3D spectroscopy bargains a brand new approach to take on astrophysical difficulties, and opens up new strains of study. considering the fact that its inception within the eighties and early nineties, examine during this box has grown significantly. huge telescopes all over the global at the moment are built with vital box devices, and tools of the long run James Webb area Telescope can have crucial box spectroscopic services. these days, extra attempt is devoted to refining options for decreasing, examining and studying the information received with 3D spectrographs. Containing lectures from the 17th wintry weather university of the Canary Islands Astrophysics Institute, this e-book explores new 3D spectroscopy thoughts and information. A huge and balanced presentation of analysis during this box, it introduces astronomers to a brand new new release of tools, widening the attraction of vital box spectroscopy and supporting it develop into a strong software in tackling astrophysical difficulties.
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Extra info for 3D Spectroscopy in Astronomy (Canary Islands Winter School of Astrophysics)
ET AL. M. ET AL. , Taylor, K. M. , Krabbe, A. ET AL. , Allington-Smith, J. , Mancini, D. ET AL. (2003), SPIE, 4841, p. 1670 Mediavilla, E, Arribas, S. , Hippelein, H. (1992), A&A, 264s, 455 Michlovic, J. T.
40. Discrete Zerodur slicer element (MUSE prototype). 41. FP-principle. 3D, SINFONI. g. , 2004). In summary, slicers provide high density of spectra, high eﬃciency, and a compact optomechanical design for high stability. Slicers have been manufactured from Zerodur, and from metal as monolithic devices. Slicers are routinely operated in the NIR, and there are ongoing research and development eﬀorts to optimize metallic slicers for operation in the visual. In contrast to ﬁber and lens array IFUs, no scrambling is involved, and the telescope focal plane is projected directly onto the detector.
The direction of dispersion is approximately 2 pixels, and given the more or less Gaussian proﬁle of the spectrograph point-spread function (PSF), there is considerable overlap between adjacent spectra. The average inter-spectra minimum intensity is ≈ 65% of the average peak intensity, while the spectrum-to-spectrum intensity variation is > 20%. Ideally, the data reduction algorithm must: (1) ﬁnd the exact location of all spectra (tracing); (2) extract the ﬂux per wavelength bin for each spectrum; (3) compensate for diﬀerent amount of cross-talk introduced by the overlap of spectra; (4) apply a ‘ﬁber-ﬂat-ﬁeld’ correction to compensate for the variation of throughput over diﬀerent ﬁbers; and (5) rebin all spectra to a common wavelength scale, before the set of spectra can be used to reconstruct maps, etc.