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Title

General formulation for the calibration and characterization of narrow-gap etalons: the OSIRIS/GTC tunable filters case

AuthorsGonzález-González, J. J.; Cepa, Jordi; González-Serrano, José Ignacio ; Sánchez-Portal, Miguel
KeywordsInstrumentation: interferometers
Instrumentation: spectrographs
Issue Date2014
PublisherOxford University Press
Royal Astronomical Society
CitationMonthly Notices of the Royal Astronomical Society 443(4): 3289-3301 (2014)
AbstractTunable filters (TFs) are a powerful way of implementing narrow-band imaging mode over wide wavelength ranges, without the need of purchasing a large number of narrow-band filters covering all strong emission or absorption lines at any redshift. However, one of its main features is a wavelength variation across the field of view, sometimes termed the phase effect. In thiswork, an anomalous phase effect is reported and characterized for the Optical System for Imaging and low Resolution Integrated Spectroscopy (OSIRIS) instrument at the 10.4 m Gran Telescopio Canarias. The transmitted wavelength across the field of view of the instrument depends, not only on the distance to the optical centre, but on wavelength. This effect is calibrated for the red TF of OSIRIS by measuring both normal-incidence light at laboratory and spectral lamps at the telescope at non-normal incidence. This effect can be explained by taking into account the inner coatings of the etalon. In a high spectral resolution etalon, the gap between plates is much larger than the thickness of the inner reflective coatings. In the case of a TF, like that in OSIRIS, the coatings thickness could be of the order of the cavity, which changes drastically the effective gap of the etalon.We show that by including thick and dispersive coatings into the interference equations, the observed anomalous phase effect can be perfectly reproduced. In fact, we find that, for the OSIRIS red TF, a two-coatings model fits the data with an rms of 0.5 Å at all wavelengths and incidence angles. This is a general physical model that can be applied to other TF instruments. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Publisher version (URL)http://dx.doi.org/10.1093/mnras/stu1310
URIhttp://hdl.handle.net/10261/110515
DOIhttp://dx.doi.org/10.1093/mnras/stu1310
Identifiersdoi: 10.1093/mnras/stu1310
issn: 0035-8711
e-issn: 1365-2966
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