CCAT-prime: Designs and status of the first light 280 GHz MKID array and Mod-Cam receiver
Cody J. Duell, Eve M. Vavagiakis, Jason Austermann, Scott C. Chapman, Steve K. Choi, Nicholas F. Cothard, Brad Dober, Patricio Gallardo, Jiansong Gao, Christoph… 展开作者
Cody J. Duell, Eve M. Vavagiakis, Jason Austermann, Scott C. Chapman, Steve K. Choi, Nicholas F. Cothard, Brad Dober, Patricio Gallardo, Jiansong Gao, Christopher Groppi, Terry L. Herter, Gordon J. Stacey, Zachary Huber, Johannes Hubmayr, Doug Johnstone, Yaqiong Li, Philip Mauskopf, Jeff McMahon, Michael D. Niemack, Thomas Nikola, Kayla Rossi, Sara Simon, Adrian K. Sinclair, Michael Vissers, Jordan Wheeler, Bugao Zou
The CCAT-prime project's first light array will be deployed in Mod-Cam, a single-module testbed and first light cryostat, on the Fred Young Submillimeter Telescope (FYST) in Chile's high Atacama desert in late 2022. FYST is a six-meter aperture telescope being built on Cerro Chajnantor at an elevation of 5600 meters to observe at millimeter and submillimeter wavelengths.1 Mod-Cam will pave the way for Prime-Cam, the primary first generation instrument, which will house up to seven instrument modules to simultaneously observe the sky and study a diverse set of science goals from monitoring protostars to probing distant galaxy clusters and characterizing the cosmic microwave background (CMB). At least one feedhorn-coupled array of microwave kinetic inductance detectors (MKIDs) centered on 280 GHz will be included in Mod-Cam at first light, with additional instrument modules to be deployed along with Prime-Cam in stages. The first 280 GHz detector array was fabricated by the Quantum Sensors Group at NIST in Boulder, CO and includes 3,456 polarization-sensitive MKIDs. Current mechanical designs allow for up to three hexagonal arrays to be placed in each single instrument module. We present details on this first light detector array, including mechanical designs and cold readout plans, as well as introducing Mod-Cam as both a testbed and predecessor to Prime-Cam.
The Prime-Cam receiver on the Fred Young Submillimeter Telescope for the CCAT-prime project aims to address important astrophysical and cosmological questions with sensitive broadband, polarimetric, and spectroscopic measurements. The primary frequency bands in development include 280, 350, and 850 GHz for the polarization-sensitive broadband channels and 210--420 GHz for the spectrometers. Microwave kinetic inductance detectors (MKIDs) are a natural choice of detector technology for the simplicity in multiplexed readout needed for large format arrays at these high frequencies. We present here…
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 ga…
CCAT: The 410 GHz camera module for FYST - design and testing of the MKID focal plane
Dalhousie University（达尔豪斯大学）；University of British Columbia（不列颠哥伦比亚大学）；University of Victoria（维多利亚大学）；National Institute of Standards and Technology（美国国家标准与技术研究院）；McGill University（麦吉尔大学）；NRC Herzberg Astronomy & Astrophysics Research Centre（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究中心）；Cornell University（康奈尔大学）；Duke University（杜克大学）；Johns Hopkins University（约翰斯·霍普金斯大学）
CCAT: Characterization of the first science-grade MKID array for the Prime-Cam 850 GHz module
University of British Columbia（不列颠哥伦比亚大学）；National Institute of Standards and Technology（美国国家标准与技术研究院）；Dalhousie University（达尔豪斯大学）；NRC Herzberg Astronomy & Astrophysics Research Centre（NRC赫茨伯格天文学与天体物理学研究中心）；University of California, Riverside（加州大学河滨分校）；Cornell University（康奈尔大学）；Duke University（杜克大学）；Johns Hopkins University（约翰斯·霍普金斯大学）
CCAT-prime is a new 6 m crossed Dragone telescope designed to characterize the Cosmic Microwave Background (CMB) polarization and foregrounds, measure the Sunyaev-Zel'dovich effects of galaxy clusters, map the [CII] emission intensity from the Epoch of Reionization (EoR), and monitor accretion luminosity over multi-year timescales of hundreds of protostars in the Milky Way. CCAT-prime will make observations from a 5,600 m altitude site on Cerro Chajnantor in the Atacama Desert of northern Chile. The novel optical design of the telescope combined with high surface accuracy ($<$10 $μ$m) mirrors …
CCAT is a large submillimetre telescope to be built near the ALMA site in northern Chile. A large-format KID camera, with up to 48,000 detectors at a single waveband sampled at about 1 kHz, will have a data rate about 50 times larger than SCUBA-2, the largest existing submillimetre camera. Creating a map from this volume of data will be a challenge, both in terms of memory and processing time required. We investigate how to extend SMURF, the iterative map-maker used for reducing SCUBA-2 observations, to a distributed-node parallel system, and estimate how the processing time scales with the nu…
CCAT: Mod-Cam Readout Overview and Flexible Stripline Performance
Cornell University（康奈尔大学）；University of British Columbia（不列颠哥伦比亚大学）；Dalhousie University（达尔豪斯大学）；University of California, Riverside（加州大学河滨分校）；Arizona State University（亚利桑那州立大学）；Duke University（杜克大学）
CCAT will be a large sub-millimeter telescope to be built near the ALMA site in northern Chile. The telescope must support a varied set of instrumentation including large format KID cameras, a large heterodyne array and a KID-based direct detection multi-object spectrometer. We are developing a new raw data model based on HDF5 that can cope with the expected data rates of order Gbit/s and is flexible enough to hold raw data from all planned instruments.
New challenges in submillimeter wave astronomy require instruments with a combination of high sensitivity and angular resolution, wide field of view and multiwave (multicolor) spectral range. New large single mm/submm telescopes are in high demand, as well as their inclusion in the global Event Horizon Telescope (EHT) VLBI network. At the same time, there are no large mm/submm telescopes in Asia at all while appropriate sites exist and their appearance in Asia or Eurasia is long overdue. Kinetic inductance detectors (KID) are ideal for large-format array implementation, which will be necessary…
CCAT will be a 25m diameter sub-millimeter telescope capable of operating in the 0.2 to 2.1mm wavelength range. It will be located at an altitude of 5600m on Cerro Chajnantor in northern Chile near the ALMA site. The anticipated first generation instruments include large format (60,000 pixel) kinetic inductance detector (KID) cameras, a large format heterodyne array and a direct detection multi-object spectrometer. The paper describes the architecture of the CCAT software and the development strategy.
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 F$λ$ 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 detecto…
CCAT: The Prime-Cam Instrument for the Fred Young Submillimeter Telescope -- Overview and Status
Duke University（杜克大学）；Cornell University（康奈尔大学）；Universidad Diego Portales（迭戈·波特莱斯大学）；National Institute of Standards and Technology（美国国家标准与技术研究院）；Universität Bonn（波恩大学）；University of British Columbia（不列颠哥伦比亚大学）；Dalhousie University（达尔豪斯大学）；University of California, Riverside（加州大学河滨分校）；University of Waterloo（滑铁卢大学）；Queen’s University（女王大学）；NRC Herzberg Astronomy and Astrophysics（NRC赫茨伯格天体物理学研究所）；University of Victoria（维多利亚大学）；Cornell Center for Astrophysics and Planetary Sciences, Cornell University（康奈尔大学天体物理学与行星科学中心）；University of Cologne（科隆大学）
CCAT will be a 25-meter telescope for sub millimeter astronomy located at 5600m altitude on Cerro Chajnantor in northern Chile. CCAT will combine high sensitivity, a wide field of view, and a broad wavelength range (0.35 to 2.1mm) to provide an unprecedented capability for deep, large-area multicolor submillimeter surveys. It is planned to have a suite of instruments including large format KID cameras, a large heterodyne array and a KID-based direct detection multi-object spectrometer. The remote location drives a desire for fully autonomous observing coupled with data reduction pipelines and …
The Array Camera for Optical to Near-IR Spectrophotometry, or ARCONS, is a camera based on Microwave Kinetic Inductance Detectors (MKIDs), a new technology that has the potential for broad application in astronomy. Using an array of MKIDs, the instrument is able to produce time-resolved imaging and low-resolution spectroscopy constructed from detections of individual photons. The arrival time and energy of each photon are recorded in a manner similar to X-ray calorimetry, but at higher photon fluxes. The technique works over a very large wavelength range, is free from fundamental read noise an…
CCAT: Optical Responsivity, Noise, and Readout Optimization of KIDs for Prime-Cam
University of California, Riverside（加州大学河滨分校）；Cornell University（康奈尔大学）；University of British Columbia（不列颠哥伦比亚大学）；Dalhousie University（达尔豪斯大学）；Duke University（杜克大学）
CCAT-prime will be a 6-meter aperture telescope operating from sub-mm to mm wavelengths, located at 5600 meters elevation on Cerro Chajnantor in the Atacama Desert in Chile. Its novel crossed-Dragone optical design will deliver a high throughput, wide field of view capable of illuminating much larger arrays of sub-mm and mm detectors than can existing telescopes. We present an overview of the motivation and design of Prime-Cam, a first-light instrument for CCAT-prime. Prime-Cam will house seven instrument modules in a 1.8 meter diameter cryostat, cooled by a dilution refrigerator. The optical …
CCAT: Silicon-Platelet Feedhorns for Submillimeter Wavelengths
National Institute of Standards and Technology（美国国家标准与技术研究院）；University of Colorado（科罗拉多大学）；University of British Columbia（不列颠哥伦比亚大学）；Dalhousie University（达尔豪斯大学）；University of California, Riverside（加州大学河滨分校）；Cornell University（康奈尔大学）
The Fred Young Submillimeter Telescope (FYST) at the Cerro-Chajnantor Atacama Telescope prime (CCAT- prime) Facility will host Prime-Cam as a powerful, first generation camera with imaging polarimeters working at several wavelengths and spectroscopic instruments aimed at intensity mapping during the Epoch of Reionization. Here we introduce the 850 GHz (350 micron) instrument module. This will be the highest frequency module in Prime-Cam and the most novel for astronomical and cosmological surveys, taking full advantage of the atmospheric transparency at the high 5600 meter CCAT-prime siting on…
CCAT: Magnetic Sensitivity Measurements of Kinetic Inductance Detectors
National Institutes of Standards and Technology（国家标准与技术研究院）；University of California, Riverside（加州大学河滨分校）；Dalhousie University（达尔豪斯大学）；University of British Columbia（不列颠哥伦比亚大学）；Duke University（杜克大学）
We present the design, construction, and commissioning results of ARCONS, the Array Camera for Optical to Near-IR Spectrophotometry. ARCONS is the first ground-based instrument in the optical through near-IR wavelength range based on Microwave Kinetic Inductance Detectors (MKIDs). MKIDs are revolutionary cryogenic detectors, capable of detecting single photons and measuring their energy without filters or gratings, similar to an X-ray microcalorimeter. MKIDs are nearly ideal, noiseless photon detectors, as they do not suffer from read noise or dark current and have nearly perfect cosmic ray re…
The Epoch of Reionization Spectrometer (EoR-Spec) is an instrument module for the Prime-Cam receiver of the 6 m aperture CCAT-prime Telescope at 5600 m in Chile. EoR-Spec will perform 158 $μ$m [CII] line intensity mapping of star-forming regions at redshifts between 3.5 and 8 (420 - 210 GHz), tracing the evolution of structure during early galaxy formation. At lower redshifts, EoR-Spec will observe galaxies near the period of peak star formation - when most stars in today's universe were formed. At higher redshifts, EoR-Spec will trace the late stages of reionization, the early stages of galax…
We present a detailed overview of the science goals and predictions for the Prime-Cam direct detection camera/spectrometer being constructed by the CCAT-prime collaboration for dedicated use on the Fred Young Submillimeter Telescope (FYST). The FYST is a wide-field, 6-m aperture submillimeter telescope being built (first light in mid-2024) by an international consortium of institutions led by Cornell University and sited at more than 5600 meters on Cerro Chajnantor in northern Chile. Prime-Cam is one of two instruments planned for FYST and will provide unprecedented spectroscopic and broadband…
The Epoch of Reionization Spectrometer (EoR-Spec) is one of the instrument modules to be installed in the Prime-Cam receiver of the Fred Young Submillimeter Telescope (FYST). This six-meter aperture telescope will be built on Cerro Chajnantor in the Atacama Desert in Chile. EoR-Spec is designed to probe early star-forming regions by measuring the [CII] fine-structure lines between redshift z = 3.5 and z = 8 using the line intensity mapping technique. The module is equipped with a scanning Fabry-Perot interferometer (FPI) to achieve the spectral resolving power of about RP = 100. The FPI consis…
University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Jet Propulsion Laboratory（喷气推进实验室）；California Institute of Technology（加州理工学院）
We present the development of a machine learning based pipeline to fully automate the calibration of the frequency comb used to read out optical/IR Microwave Kinetic Inductance Detector (MKID) arrays. This process involves determining the resonant frequency and optimal drive power of every pixel (i.e. resonator) in the array, which is typically done manually. Modern optical/IR MKID arrays, such as DARKNESS (DARK-speckle Near-infrared Energy-resolving Superconducting Spectrophotometer) and MEC (MKID Exoplanet Camera), contain 10-20,000 pixels, making the calibration process extremely time consu…
Microwave Kinetic Inductance Detectors (MKIDs) are superconducting detectors capable of counting single photons and measuring their energy in the UV, optical, and near-IR. MKIDs feature intrinsic frequency domain multiplexing (FDM) at microwave frequencies, allowing the construction and readout of large arrays. Due to the microwave FDM, MKIDs do not require the complex cryogenic multiplexing electronics used for similar detectors, such as Transition Edge Sensors (TESs), but instead transfer this complexity to room temperature electronics where they present a formidable signal processing challe…
We present the detailed science case, and brief descriptions of the telescope design, site, and first light instrument plans for a new ultra-wide field submillimeter observatory, CCAT-prime, that we are constructing at a 5600 m elevation site on Cerro Chajnantor in northern Chile. Our science goals are to study star and galaxy formation from the epoch of reionization to the present, investigate the growth of structure in the Universe, improve the precision of B-mode CMB measurements, and investigate the interstellar medium and star formation in the Galaxy and nearby galaxies through spectrosco…
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 $μ$m [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 modu…
CCAT: Detector Noise Limited Performance of the RFSoC-based Readout Electronics for mm/sub-mm/far-IR KIDs
University of British Columbia（不列颠哥伦比亚大学）；University of Victoria（维多利亚大学）；Herzberg Astronomy and Astrophysics Research Centre, National Research Council Canada（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究中心）；Cornell University（康奈尔大学）；National Institute of Standards and Technology（美国国家标准与技术研究院）；University of California, Riverside（加州大学河滨分校）；Arizona State University（亚利桑那州立大学）
CCAT: Design and Characterization of the 350 GHz Instrument Module
Cornell University（康奈尔大学）；National Institute of Standards and Technology（美国国家标准与技术研究院）；University of British Columbia（不列颠哥伦比亚大学）；Dalhousie University（达尔豪斯大学）；University of California, Riverside（加州大学河滨分校）；Duke University（杜克大学）；University of Colorado, Boulder（科罗拉多大学博尔德分校）
The Prime-Cam instrument on the Fred Young Submillimeter Telescope (FYST) is expected to be the largest deployment of millimeter and submillimeter sensitive kinetic inductance detectors to date. To read out these arrays efficiently, a microwave frequency multiplexed readout has been designed to run on the Xilinx Radio Frequency System on a Chip (RFSoC). The RFSoC has dramatically improved every category of size, weight, power, cost, and bandwidth over the previous generation readout systems. We describe a baseline firmware design which can read out four independent RF networks each with 500 MH…
We have fabricated and characterized 10,000 and 20,440 pixel Microwave Kinetic Inductance Detector (MKID) arrays for the Dark-speckle Near-IR Energy-resolved Superconducting Spectrophotometer (DARKNESS) and the MKID Exoplanet Camera (MEC). These instruments are designed to sit behind adaptive optics systems with the goal of directly imaging exoplanets in a 800-1400 nm band. Previous large optical and near-IR MKID arrays were fabricated using substoichiometric titanium nitride (TiN) on a silicon substrate. These arrays, however, suffered from severe non-uniformities in the TiN critical temperat…
CCAT: Design, Implementation, and Testing of a System to Read Out over 10,000 280 GHz KIDs using RFSoC Electronics
Cornell University（康奈尔大学）；National Institute of Standards and Technology（美国国家标准与技术研究院）；University of British Columbia（不列颠哥伦比亚大学）；Dalhousie University（达尔豪斯大学）；University of California, Riverside（加州大学河滨分校）；Arizona State University（亚利桑那州立大学）
Large-scale arrays of Microwave Kinetic Inductance Detectors (MKIDs) are attractive candidates for use in imaging instruments for next generation submillimeter-wave telescopes such as CCAT. We have designed and fabricated tightly packed ~250-pixel MKID arrays using lumped-element resonators etched from a thin layer of superconducting TiNx deposited on a silicon substrate. The high pixel packing density in our initial design resulted in large microwave crosstalk due to electromagnetic coupling between the resonators. Our second design eliminates this problem by adding a grounding shield and usi…
CCAT: a two-octave 1.024 GHz KID readout featuring an overlap-channel polyphase synthesis filter bank on RFSoC
University of British Columbia（不列颠哥伦比亚大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；Dalhousie University（达尔豪斯大学）；McGill University（麦吉尔大学）；University of California, Riverside（加州大学河滨分校）；Cornell University（康奈尔大学）
The main advantage of Microwave Kinetic Inductance Detector arrays (MKID) is their multiplexing capability, which allows for building cameras with a large number of pixels and good sensitivity, particularly suitable to perform large blank galaxy surveys. However, to have as many pixels as possible it is necessary to arrange detectors close in readout frequency. Consequently KIDs overlap in frequency and are coupled to each other producing crosstalk. Because crosstalk can be only minimised by improving the array design, in this work we aim to correct for this effect a posteriori. We analysed a …
Submillimeter cameras now have up to $10^4$ pixels (SCUBA 2). The proposed CCAT 25-meter submillimeter telescope will feature a 1 degree field-of-view. Populating the focal plane at 350 microns would require more than $10^6$ photon-noise limited pixels. To ultimately achieve this scaling, simple detectors and high-density multiplexing are essential. We are addressing this long-term challenge through the development of frequency-multiplexed superconducting microresonator detector arrays. These arrays use lumped-element, direct-absorption resonators patterned from titanium nitride films. We will…
We report on the development of ARCONS, the ARray Camera for Optical to Near-IR Spectrophotometry. This photon counting integral field unit (IFU), being built at UCSB and Caltech with detectors fabricated at JPL, will use a unique, highly multiplexed low temperature detector technology known as Microwave Kinetic Inductance Detectors (MKIDs). These detectors, which operate at 100 mK, should provide photon counting with energy resolution of R = E/δE > 20 and time resolution of a microsecond, with a quantum efficiency of around 50%. We expect to field the instrument at the Palomar 200" telescope …
Laser-micromachined silicon-platelet feedhorns for large-scale submillimeter and millimeter-wave focal planes
Quantum Sensors Division, National Institute of Standards and Technology（美国国家标准与技术研究院量子传感器部）；Inertial Fusion Technology Division, Energy Group, General Atomics（通用原子能公司惯性聚变技术部能源组）；Department of Physics, University of Colorado, Boulder（科罗拉多大学博尔德分校物理系）；Fermi National Accelerator Laboratory（费米国家加速器实验室）
