The optical design of the six-meter CCAT-prime and Simons Observatory telescopes

Parshley, Stephen C.; Niemack, Michael D.; Hills, R. E.; Dicker, Simon; Dünner, Rolando; Erler, Jens; Gallardo, Patricio A.; Gudmundsson, J. E.; Herter, T.; Koopman, Brian J.; Limon, M.; Matsuda, Frederick; Mauskopf, Philip Daniel; Riechers, Dominik A.; Stacey, G. J.; Vavagiakis, Eve M.

doi:10.1117/12.2314073

Cited by 40 publications

(36 citation statements)

References 21 publications

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“…The collaboration is building a Large Aperture Telescope (LAT) with a 6-meter primary mirror similar in size to ACT, and three 0.5-meter refracting Small Aperture Telescopes (SATs) similar in size to BICEP3. New optical designs (Niemack 2016;Parshley et al 2018) will provide much larger focal planes for the LAT than current experiments. We initially plan to deploy a total of 60,000 detectors, approximately evenly split between the LAT and the set of SATs.…”

Section: Introductionmentioning

confidence: 99%

The Simons Observatory: science goals and forecasts

Ade

Aguirre

Ahmed

et al. 2019

J. Cosmol. Astropart. Phys.

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The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping ≈ 10% of the sky to a white noise level of 2 µK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r) = 0.003. The large aperture telescope will map ≈ 40% of the sky at arcminute angular resolution to an expected white noise level of 6 µK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensorto-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources a .

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Section: Introductionmentioning

confidence: 99%

The Simons Observatory: science goals and forecasts

Ade

Aguirre

Ahmed

et al. 2019

J. Cosmol. Astropart. Phys.

Self Cite

1,299

1,070

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“…The classic CD design consists of a parabolic primary and a hyperbolic secondary. As described in Parshley et al, 7 it is possible to add canceling spherical terms to each mirror which cancel out comma in off-axis fields. With these corrections the primary aberration left is astigmatism ( Figure 1).…”

Section: Designmentioning

confidence: 99%

Cold optical design for the large aperture Simons' Observatory telescope

Dicker¹,

Gallardo²,

Gudmundsson³

et al. 2018

Ground-Based and Airborne Telescopes VII

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The Simons Observatory will consist of a single large (6 m diameter) telescope and a number of smaller (∼0.5 m diameter) refracting telescopes designed to measure the polarization of the Cosmic Microwave Background to unprecedented accuracy. The large aperture telescope is the same design as the CCAT-prime telescope, a modified Crossed Dragone design with a field-of-view of over 7.8 degrees diameter at 90 GHz. This paper presents an overview of the cold reimaging optics for this telescope and what drove our choice of 350-400 mm diameter silicon lenses in a 2.4 m cryostat over other possibilities. We will also consider the future expandability of this design to CMB Stage-4 and beyond.

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“…The optics are unique for this size (~6 m) and type of telescope (crossed-Dragone). The optical design is based on one put forward by Niemack 2 and described in detail in Parshley et al 4 The basic telescope optics are presented here ( Figure 3). The system consists of two reflectors, arranged in a crossed-Dragone configuration providing an unobstructed aperture and low cross polarization.…”

Section: Opticsmentioning

confidence: 99%

CCAT-prime: a novel telescope for sub-millimeter astronomy

Parshley¹,

Kronshage²,

Blair³

et al. 2018

Ground-Based and Airborne Telescopes VII

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The CCAT-prime telescope is a 6-meter aperture, crossed-Dragone telescope, designed for millimeter and sub-millimeter wavelength observations. It will be located at an altitude of 5600 meters, just below the summit of Cerro Chajnantor in the high Atacama region of Chile. The telescope's unobscured optics deliver a field of view of almost 8 degrees over a large, flat focal plane, enabling it to accommodate current and future instrumentation fielding >100k diffraction-limited beams for wavelengths less than a millimeter. The mount is a novel design with the aluminum-tiled mirrors nested inside the telescope structure. The elevation housing has an integrated shutter that can enclose the mirrors, protecting them from inclement weather. The telescope is designed to co-host multiple instruments over its nominal 15 year lifetime. It will be operated remotely, requiring minimum maintenance and on-site activities due to the harsh working conditions on the mountain. The design utilizes nickel-iron alloy (Invar) and carbon-fiber-reinforced polymer (CFRP) materials in the mirror support structure, achieving a relatively temperature-insensitive mount. We discuss requirements, specifications, critical design elements, and the expected performance of the CCAT-prime telescope. The telescope is being built by CCAT Observatory, Inc., a corporation formed by an international partnership of universities. More information about CCAT and the CCAT-prime telescope can be found at www.ccatobservatory.org.

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The optical design of the six-meter CCAT-prime and Simons Observatory telescopes

Cited by 40 publications

References 21 publications

The Simons Observatory: science goals and forecasts

The Simons Observatory: science goals and forecasts

Cold optical design for the large aperture Simons' Observatory telescope

CCAT-prime: a novel telescope for sub-millimeter astronomy

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