TY - JOUR
T1 - Design of a 2-mm Wavelength KIDs Prototype Camera for the Large Millimeter Telescope
AU - Velázquez, M.
AU - Ferrusca, D.
AU - Castillo-Dominguez, E.
AU - Ibarra-Medel, E.
AU - Ventura, S.
AU - Gómez-Rivera, V.
AU - Hughes, D.
AU - Aretxaga, I.
AU - Grant, W.
AU - Doyle, S.
AU - Mauskopf, Philip
N1 - Publisher Copyright:
© 2016, Springer Science+Business Media New York.
PY - 2016/8/1
Y1 - 2016/8/1
N2 - A new camera is being developed for the Large Millimeter Telescope (Sierra Negra, México) by an international collaboration with the University of Massachusetts, the University of Cardiff, and Arizona State University. The camera is based on kinetic inductance detectors (KIDs), a very promising technology due to their sensitivity and especially, their compatibility with frequency domain multiplexing at microwave frequencies allowing large format arrays, in comparison with other detection technologies for mm-wavelength astronomy. The instrument will have a 100 pixels array of KIDs to image the 2-mm wavelength band and is designed for closed cycle operation using a pulse tube cryocooler along with a three-stage sub-kelvin 3He cooler to provide a 250 mK detector stage. RF cabling is used to readout the detectors from room temperature to 250 mK focal plane, and the amplification stage is achieved with a low-noise amplifier operating at 4 K. The readout electronics will be based on open-source reconfigurable open architecture computing hardware in order to perform real-time microwave transmission measurements and monitoring the resonance frequency of each detector, as well as the detection process.
AB - A new camera is being developed for the Large Millimeter Telescope (Sierra Negra, México) by an international collaboration with the University of Massachusetts, the University of Cardiff, and Arizona State University. The camera is based on kinetic inductance detectors (KIDs), a very promising technology due to their sensitivity and especially, their compatibility with frequency domain multiplexing at microwave frequencies allowing large format arrays, in comparison with other detection technologies for mm-wavelength astronomy. The instrument will have a 100 pixels array of KIDs to image the 2-mm wavelength band and is designed for closed cycle operation using a pulse tube cryocooler along with a three-stage sub-kelvin 3He cooler to provide a 250 mK detector stage. RF cabling is used to readout the detectors from room temperature to 250 mK focal plane, and the amplification stage is achieved with a low-noise amplifier operating at 4 K. The readout electronics will be based on open-source reconfigurable open architecture computing hardware in order to perform real-time microwave transmission measurements and monitoring the resonance frequency of each detector, as well as the detection process.
KW - Instrumentation
KW - KIDs
KW - Radio telescope
KW - Sub-mm astronomy
KW - Superconductor detectors
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U2 - 10.1007/s10909-016-1536-6
DO - 10.1007/s10909-016-1536-6
M3 - Article
AN - SCOPUS:84959178240
SN - 0022-2291
VL - 184
SP - 799
EP - 804
JO - Journal of Low Temperature Physics
JF - Journal of Low Temperature Physics
IS - 3-4
ER -