The CCAT-prime Project and the Fred Young Submillimeter Telescope (FYST)
FYST will be a 6-meter diameter, 10 micron precision surface telescope operating at submillimeter to millimeter wavelengths and sited at 5.600 meters elevation on Cerro Chajnantor in the Atacama desert of northern Chile.
The novel crossed-Dragone optical design will deliver a high-throughput wide-field-of-view telescope capable of illuminating >105 (sub)millimeter wavelength detectors so that large areas of the sky can be scanned rapidly. The high altitude, dry site offers superb observing conditions, yielding routine access to the 350 micron atmospheric window as well as improved performance at longer wavelengths. Under the best conditions, observations in the 200 micron window will be possible. Deployment of FYST on Cerro Chajnantor will provide operational experience at high altitude, reducing risk for the future construction of a 25-meter class submillimeter telescope.
FYST will be ideally suited, due to its low error beam and large field of view, to probe tracers of the ISM and cloud/star formation over a range of environments in the Milky Way, the Magellanic Clouds and other nearby galaxies. Spectral large-scale imaging with CHAI (a high spectral resolution heterodyne array receiver being built at the Universität zu Köln, see below) of fine structure and mid- to high-excitation CO lines will serve as diagnostics of physical processes associated with star formation over large spatial scales.
FYST will measure the kinematic Sunyaev-Zel’dovich effect of galaxy clusters and will trace the appearance of the first population of star-forming galaxies through intensity mapping of their [CII] emission in the epoch of reionization. With FYST, scientists will be able to better measure the motions of clusters of galaxies under the influence of dark matter in relation to each other; study how galaxies and galaxy clusters first evolved; and study the properties of neutrinos, some of the lightest known particles.
The “crossed-Dragone” design establishes the FYST as a next-generation Cosmic Microwave Background (CMB) platform, capable of mapping the sky some 10 times faster than current CMB facilities. While other CMB efforts focus on wavelengths longer than one millimeter, the availability of simultaneous submillimeter imaging offered by CCAT-prime will allow precise separation of dust emission from the CMB signal. With its large flat focal plane, FYST will be ready to exploit the anticipated future advances in detector arrays.
FYST is being constructed as a partnership of Cornell University, the Universities of Cologne and Bonn in Germany and CATC, a consortium of 10 Canadian academic institutions. Researchers at additional institutes in the U.S. Canada, Germany and Chile are involved in science planning and instrument development.
The telescope is being designed and built by VERTEX Antennentechnik GmbH. The construction phase started in 2017 and is expected to lead to first light in 2022.
The scientific goals of the CCAT-prime Project motivate its unique characteristics of wide-field, high surface accuracy, high throughput and high altitude location and are encompassed in major legacy programs:
“Galactic Ecology” studies in multiple spectral lines the dynamic interstellar medium in a wide range of environments in the Milky Way, the Magellanic Clouds and other nearby galaxies. Spectral large-scale mapping with CHAI of fine structure and mid- to high-excitation CO lines are at the core of the Cologne/Bonn interests and activities as they trace the flows and accumulation of gas into cores and young stars. In detail, the GEco science case employs the following diagnostics:
- [CI] to trace cloud mass accretion, gas temperature and (dark) mass.
- Mid- and high-J CO/13CO to trace shocks and dissipation of turbulence, stellar feedback, gas excitation, density and mass.
- [NII] to trace embedded star forming regions and the number of ionizing photons.
- A dedicated monitoring of protostellar variability in the continuum near the peak of the protostellar SED on year timescales would provide a direct measure of the physical processes within the disk at ~AU scales, yielding important clues to the evolution of the protoplanetary disk.
Unique features of the planned observations are:
- Maps at (15'' x λ/350 μm) resolution over 200 deg2 scales of the Milky Way (Galactic plane and Gould Belt), Galactic Center, and Magellanic Clouds (low metallicity).
- Large scale mapping of the full area in CO 4-3 and [CI] 1-0. Zoom-ins at higher frequencies (12/13CO 6-5, 13CO 8-7, CI 2-1).
- High site provides unique access to shortest wavelengths at 200 μm for limited time and area coverage (high-J CO and [NII]).
Measurement of the velocities, temperatures and transparencies of galaxy clusters via the Sunyaev-Zel’dovich effect to place new constraints on dark energy and the sum of the neutrino masses.
Galaxy Evolution (GEvo)
“Galaxy Evolution” studies of dusty star-forming galaxies far surpassing the Herschel results in number counts and directly resolving (and characterizing) the population of faint sources responsible for most of the FIR counts/background.
Intensity mapping of the [CII] 158 micron line from star-forming galaxies in the epoch of reionization at redshifts of 5 to 9 to understand the topology and timescale of reionization.
Future prospects in CMB mapping
Its highly efficient mapping capability positions the FYST as a platform for next-generation Cosmic Microwave Background (CMB) experiments (Stage-4 CMB mapping). FYST will provide ~10 times the current CMB mapping speeds, to enable probes of inflationary gravity waves and constrain the neutrino mass sum.
FYST will be located near the summit of Cerro Chajnantor in the Atacama Desert in Chile. The extremely high elevation will allow observation of most northern and southern skies through all seasons due to the extremely dry atmosphere. Atmospheric studies over more than a decade at various sites includung Cerro Chajnantor and the ALMA site have shown that the FYST site has a median precipitable water vapor of 0.6 mm (vs. 1 mm at the ALMA site), thus giving a sensitivity gain of a factor of several (depending on wavelength) over ALMA.
In addition, FSYT will open the THz frequency range (the 200 μm atmospheric window) for about 10% of the time.
FYST site below the summit of Cerro Chajnantor in the Chilean Andes at 5600 m altitude will use a novel off-axis telescope design for its 6 m diameter telescope, the crossed-Dragone telescope. The design features:
- High surface accuracy (7–10 μm r.m.s.)
- High throughput
- Wide field-of-view
- Flat focal plane
- Accommodates > 105 detectors at longer wavelengths and even more at shorter wavelength.
First generation instruments
The FYST Heterodyne Array Instrument (CHAI)
CHAI is a heterodyne, dual frequency array receiver for FYST being developed at the Universität zu Köln. It will provide very high spectral resolution (>106) at two frequencies simultaneously. Its modular design allows fast switching between receiver arrays covering the atmospheric windows between 600, 350, and 200 μm. In detail, CHAI will feature:
- Heterodyne, dual frequency array
- 64 pixels (baseline, 128 goal) in each band
- 500 GHz (600 μm) & 850 GHz (350 μm) windows:
CO(4-3), CO(6-5), 13CO 8-7, [CI] 1-0 and 2-1
- Possiblility to access highest frequencies of the 1.5 THz (200 μm) and 1.3 THz (240 μm) windows under best atmospheric conditions:
high-J CO and [NII]
The FYST camera (p-Cam)
p-Cam is a modular, wide-field imaging camera primarily designed to measure the kinematic Sunyaev-Zel’dovich effect of galaxy clusters. The camera has ~1.5 λ/D pixel sizes with near unit filling factor in the image plane and is diffraction limited at all wavelengths.
- Seven subcamera “tubes”, pixels with dichroic polarization sensitive TES (Transition-Edge Sensed) bolometers or KIDs (Kinetic Inductance Detectors).
- FoV ~ 0.9 degree each → 20,000 pixels at 350 μm; 6,000 pixels at 1.1 mm
- Cameras are modular (size, optics, filtration), easily exchanged
The CCAT-prime consortium
The CCAT-prime consortium is a partnership of Cornell University, the Universities of Cologne and Bonn in Germany and CATC, a consortium of 10 Canadian academic institutions. Researchers at additional institutes in the U.S. Canada, Germany and Chile are involved in science planning and instrument development.
On the German side, groups at the Max Planck Institut für Astrophysik (Garching) and the Ludwig Maximilians Universität, München have expressed their interest to join the project. Negotiations are underway.