The Quijote Tgi

L. Piccirillo, R. Hoyland, M. Aguiar-González, R. Génova-Santosa, F. Gómez-Reñasco, C. López-Caraballo, R. Rebolo-López, J. A. Rubiño-Martín, V. Sánchez-de La Rosa, A. Vega-Moreno, T. Viera-Curbelo, A. Pelaez-Santos, R. Vignaga, D. Tramonte, F. Poidevin, M. R. Pérez-de-Taoro, E. Martínez-Gonzalez, B. Aja, E. Artal, J. CagigasJ. L. Cano-de-Diego, E. M. Cuerno, L. De-la-Fuente, A. Pérez, D. Ortiz, J. V. Terán, E. Villa, M. Hobson

    Research output: Contribution to journalArticlepeer-review


    The QUIJOTE TGI instrument is currently being assembled and tested at the IAC in Spain. The TGI is a 31 pixel 26-36 GHz polarimeter array designed to be mounted at the focus of the second QUIJOTE telescope. This follows a first telescope and multi-frequency instrument that have now been observing almost 2 years. The polarimeter design is based on the QUIET polarimeter scheme but with the addition of an extra 90º phase switch which allows for quasiinstantaneous complete QUI measurements through each detector. The advantage of this solution is a reduction in the systematics associated with differencing two independent radiometer channels. The polarimeters are split into a cold front end and a warm back end. The back end is a highly integrated design by the engineers at DICOM. It is also sufficiently modular for testing purposes. In this presentation the high quality wide band components used in the optical design (also designed in DICOM) are presented as well as the novel cryogenic modular design. Each polarimeter chain is accessible individually and can be removed from the cryostat and replaced without having to move the remaining pixels. The optical components work over the complete Ka band showing excellent performance. Results from the sub unit measurements are presented and also a description of the novel calibration technique that allows for bandpass measurement and polar alignment. Terrestrial Calibration for this instrument is very important and will be carried out at three points in the commissioning phase: in the laboratory, at the telescope site and finally a reduced set of calibrations will be carried out on the telescope before measurements of extraterrestrial sources begin. The telescope pointing model is known to be more precise than the expected calibration precision so no further significant error will be added through the telescope optics. The integrated back-end components are presented showing the overall arrangement for mounting on the cryostat. Many of the microwave circuits are in-house designs with performances that go beyond commercially available products.
    Original languageEnglish
    JournalProceedings of S P I E - International Society for Optical Engineering
    Publication statusPublished - Aug 2014


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