TY - GEN
T1 - MUSCAT focal plane verification
AU - Tapia, M.
AU - Ade, P. A.R.
AU - Barry, P. S.
AU - Brien, T. L.R.
AU - Castillo-Dominguez, E.
AU - Ferrusca, D.
AU - Gomez-Rivera, V.
AU - Hargrave, P.
AU - Hernandez-Rebollar, J. L.
AU - Hornsby, A.
AU - Hughes, D.
AU - Jauregui-Garcia, J. M.
AU - Mauskopf, P.
AU - Murias, D.
AU - Papageorgiou, A.
AU - Pascale, E.
AU - Perez, A.
AU - Rowe, S.
AU - Tucker, C.
AU - Velazquez, M.
AU - Ventura, S.
AU - Doyle, S.
N1 - Funding Information:
We acknowledge RCUK and CONACYT through the Newton Fund project ST/P002803/1, CONACYT for support the fellowship for the instrument scientist (grant no. 053), Chase Research Cryogenics for the development of the sub-kelvin coolers and to XILINX Inc. for the donation of the FPGAs used for the ROACH2 boards.
Publisher Copyright:
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PY - 2020
Y1 - 2020
N2 - 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.
AB - 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.
KW - 1/f noise
KW - KID detectors
KW - beam mapping
KW - focal plane characterisation
KW - noise equivalent power (NEP)
KW - spectral response
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U2 - 10.1117/12.2576219
DO - 10.1117/12.2576219
M3 - Conference contribution
AN - SCOPUS:85100002132
T3 - Proceedings of SPIE - The International Society for Optical Engineering
BT - Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X
A2 - Zmuidzinas, Jonas
A2 - Gao, Jian-Rong
PB - SPIE
T2 - Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X 2020
Y2 - 14 December 2020 through 22 December 2020
ER -