The epoch of reionization spectrometer (EoR-Spec) is an instrument module that will be deployed in the Prime-Cam receiver on the Fred Young Submillimeter Telescope (FYST), which is a 6m off-axis telescope for the CCAT-prime facility. FYST is currently being built in the Atacama Desert in Chile at an altitude of 5600 m. With the Fabry-Perot interferometer (FPI), EoR-Spec will measure the 158 µm [CII] line intensity at redshifts from 3.5 to 8 (420 to 210 GHz), with the lower redshifts tracing star formation and higher redshifts tracing the late stages of reionization. An EoR-Spec module includes three monolithic and monochroic feedhorn-coupled arrays of kinetic inductance detectors (KIDs), two of which are centered at 260 GHz with the other centered at 370 GHz. We present the design and integration process of the EoR-Spec detector array at both bands. The 370 GHz detector array will consist of 3072 detectors and each of the 260 GHz arrays will consist of 1728 detectors. Each of the detector arrays contains an aluminum feedhorn array and is read out by a few pairs of coaxial cables.
The Epoch of Reionization Spectrometer (EoR-Spec) will be an instrument module for the Prime-Cam receiver on the CCAT-prime Collaboration’s Fred Young Submillimeter Telescope (FYST), a 6-m primary mirror Crossed Dragone telescope. With its Fabry-Perot interferometer (FPI), EoR-Spec will step through frequencies between 210 and 420 GHz to perform line intensity mapping of the 158 µm [CII] line in aggregates of star-forming galaxies between redshifts of 3.5 and 8 to trace the evolution of structure in the Universe during the epoch of reionization. Here we present the optical design of the module including studies of the optical quality and other key parameters at the image surface. In order to achieve the optimal resolving power (R∼100) with the FPI, it is important to have a highly collimated beam at the Lyot stop of the system; the optimization process to achieve this goal with four lenses instead of three as used in other Prime-Cam modules is outlined. As part of the optimization, we test the effect of replacing some of the aspheric lenses with biconic lenses in this Crossed Dragone design and find that the biconic lenses tends to improve the image quality across the focal plane of the module.
Mod-Cam is a first light and commissioning instrument for the CCAT-prime project’s six-meter aperture Fred Young Submillimeter Telescope (FYST), currently under construction at 5600 m on Cerro Chajnantor in Chile’s Atacama Desert. Prime-Cam, a first-generation science instrument for FYST, will deliver over ten times greater mapping speed than current and near-term facilities for unprecedented 280–850 GHz broadband and spectroscopic measurements with microwave kinetic inductance detectors (MKIDs). CCAT-prime will address a suite of science goals, from Big Bang cosmology to star formation and galaxy evolution over cosmic time. Mod-Cam deployment on FYST with a 280 GHz instrument module containing MKID arrays is planned for early science observations in 2024. Mod-Cam will be used to test instrument modules for Prime-Cam, which can house up to seven instrument modules. We discuss the design and status of the 0.9 m diameter, 1.8 m long Mod-Cam receiver and 40 cm diameter 280 GHz instrument module, with cold stages at 40 K, 4 K, 1 K, and 100 mK. We also describe the instrument module’s cryogenic readout designs to enable the readout of more than 10,000 MKIDs across 18 networks.
Prime-Cam is a first-generation instrument for the Cerro Chajnantor Atacama Telescope-prime (CCAT-prime) Facility. The 850 GHz module for Prime-Cam will probe the highest frequency of all the instrument modules. We describe the parameter space of the 850 GHz optical system between the Fλ spacing, beam size, pixel sensitivity, and detector count. We present the optimization of an optical design for the 850 GHz instrument module for CCAT-prime. We further describe the development of the cryogenic RF chain design to accommodate 30 readout lines to read 41,400 kinetic inductance detectors (KIDs) within the cryogenic testbed.
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