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A full-Stokes polarimeter for the GREGOR Fabry-Perot interferometer

Published online by Cambridge University Press:  01 November 2008

Horst Balthasar
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: hbalthasar@aip.de; cdenker@aip.de; ahofmann@aip.de
N. Bello González
Affiliation:
Institut für Astrophysik, Friedrich-Hund-Platz 1, D-37077 Göttingen, Germany email: nazaret@astro.physik.uni-goettingen.de; kneer@astro.physik.uni-goettingen.de
M. Collados
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain email: mcv@iac.es; kgp@iac.es
C. Denker
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: hbalthasar@aip.de; cdenker@aip.de; ahofmann@aip.de
A. Hofmann
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: hbalthasar@aip.de; cdenker@aip.de; ahofmann@aip.de
F. Kneer
Affiliation:
Institut für Astrophysik, Friedrich-Hund-Platz 1, D-37077 Göttingen, Germany email: nazaret@astro.physik.uni-goettingen.de; kneer@astro.physik.uni-goettingen.de
K. G. Puschmann
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain email: mcv@iac.es; kgp@iac.es
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Abstract

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One of the first post-focus instruments of the new solar telescope GREGOR will be a Fabry-Perot spectrometer, which is an upgrade of the Göttingen Fabry-Perot interferometer at the Vacuum Tower Telescope (VTT) on Tenerife. This spectrometer is equipped with a full-Stokes polarimeter. The modulation is performed with two ferroelectric liquid crystals, one acting nominally as quarter-wave plate, and the other as half-wave plate. A modified Savart plate serves as polarimetric beam splitter. With the present liquid crystals, the optimum wavelength range of this polarimeter is between 580 and 660 nm. The spectro-polarimeter will benefit from the capabilities of the new telescope GREGOR which will provide a spatial resolution of about 0″.1 (75 km on the solar surface). Thus we will be able to investigate small magnetic features, and we will study their development with high cadence.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2009

References

Bello González, N. & Kneer, F. 2008, A&A 480, 265Google Scholar
Bendlin, C., Volkmer, R., & Kneer, F. 1992, A&A 257, 817Google Scholar
Keller, C. U. 2006, private communicationGoogle Scholar
Keller, C. U. & von der Lühe, O. 1992, A&A 261, 321Google ScholarPubMed
Hofmann, A., Rendtel, J., & Arlt, K. 2008, Cent. Eur. Astrophys. Bull., submittedGoogle Scholar
Puschmann, K. G., Kneer, F., Seelemann, T., & Wittmann, A. D. 2006, A&A 451, 1151Google Scholar
Volkmer, R., von der Lühe, O., Kneer, F., and 17 coauthors 2007, in Kneer, F., Puschmann, K. G., Wittmann, A. D. (eds.) Modern Solar Facilities - Advanced Solar Science, Universitätsverlag Göttingen, p. 39.Google Scholar
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A full-Stokes polarimeter for the GREGOR Fabry-Perot interferometer
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