MUSCAT focal plane verification

Tapia, Marcial, Ade, Peter ORCID: https://orcid.org/0000-0002-5127-0401, Barry, Peter, Brien, Thomas, Castillo-Domínguez, Edgar, Ferrusca, Daniel, Gómez-Rivera, Víctor, Hargrave, Peter ORCID: https://orcid.org/0000-0002-3109-6629, Hernández Rebollar, Jose Luis, Hornsby, Amber ORCID: https://orcid.org/0000-0002-9998-1720, Murias, Dolce, Hughes, David, Jáuregui-García, José Miguel, Mauskopf, Philip, Pérez, Abel, Papageorgiou, Andreas, Pascale, Enzo, Rowe, Samuel, Tucker, Carole ORCID: https://orcid.org/0000-0002-1851-3918, Ventura, Salvador, Miguel, Velázquez and Doyle, Simon ORCID: https://orcid.org/0000-0002-9054-986X 2020. MUSCAT focal plane verification. Presented at: SPIE Astronomical Telescopes + Instrumentation 2020, Virtual, 14-18 December 2020. Proceedings Volume 11453, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X;. , vol.11453 SPIE, p. 1145309. 10.1117/12.2576219

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Abstract

The Mexico-UK Submillimetre Camera for Astronomy (MUSCAT) is the second-generation large-format continuum camera operating in the 1.1 mm band to be installed on the 50-m diameter Large Millimeter Telescope (LMT) in Mexico. The focal plane of the instrument is made up of 1458 horn coupled lumped-element kinetic inductance detectors (LEKID) divided equally into six channels deposited on three silicon wafers. Here we present the preliminary results of the complete characterisation in the laboratory of the MUSCAT focal plane. Through the instrument's readout system, we perform frequency sweeps of the array to identify the resonance frequencies, and continuous timestream acquisitions to measure and characterise the intrinsic noise and 1/f knee of the detectors. Subsequently, with a re-imaging lens and a blackbody point source, the beams of every detector are mapped, obtaining a mean FWHM size of ~3.27 mm, close to the expected 3.1 mm. Then, by varying the intensity of a beam filling blackbody source, we measure the responsivity and noise power spectral density (PSD) for each detector under an optical load of 300 K, obtaining the noise equivalent power (NEP), with which we verify that the majority of the detectors are photon noise limited. Finally, using a Fourier Transform Spectrometer (FTS), we measure the spectral response of the instrument, which indicate a bandwidth of 1.0-1.2 mm centred on 1.1 mm, as expected.

Item Type:	Conference or Workshop Item (Paper)
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Publisher:	SPIE
Funders:	RCUK, CONACYT
Date of First Compliant Deposit:	15 December 2020
Date of Acceptance:	30 November 2020
Last Modified:	27 Oct 2023 06:17
URI:	https://orca.cardiff.ac.uk/id/eprint/136982

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