Cold optical design for the large aperture Simons' Observatory telescope

Dicker, Simon; Gallardo, Patricio A.; Gudmundsson, J. E.; Mauskopf, Philip Daniel; Ali, Aamir; Ashton, Peter; Coppi, Gabriele; Devlin, Mark J.; Galitzki, Nicholas; Ho, Shuay Pwu Patty; Hill, Charles A.; Hubmayr, Johannes; Keating, Brian; Lee, A. T.; Limon, M.; Matsuda, Frederick; McMahon, Jeffrey; Niemack, Michael D.; Orlowski-Scherer, John; Piccirillo, L.; Salatino, Maria; Simon, Sara M.; Staggs, Suzanne T.; Thornton, Robert J.; Ullom, Joel N.; Vavagiakis, Eve M.; Wollack, Edward J.; Xu, Zhilei; Zhu, Ningfeng

doi:10.1117/12.2313444

Cited by 19 publications

(43 citation statements)

References 12 publications

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“…This calculation is combined with the results of ray-trace simulations to evaluate the performance of various camera optical designs. 43 The impact of F/# on MS is most pronounced at low frequencies, where the spillover fraction and optical correlations tend to be largest. In contrast, the impact of F/# on sensitivity is minimal at high frequencies where stop spillover and optical correlations tend to be small.…”

Section: Camera Magnificationmentioning

confidence: 96%

“…The LAT has a 6 m-diameter primary mirror, a 7.8 degree FOV, and up to 13 cameras in a 2.4 m diameter receiver that cover more than a decade in frequency. 15,41,43 Motivated by the immensity and complexity of the LAT system, effort has been devoted to understanding and controlling ambient-temperature spillover and scattering, 40 as minimizing optical loading is critical to maintaining low NEP ph . Figure 6 shows relative in-band optical power and MS in each frequency band as a function of LAT primary spillover fraction.…”

Section: Lat Primary Spillovermentioning

confidence: 99%

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BoloCalc: a sensitivity calculator for the design of Simons Observatory

Hill

Bruno

Simon

et al. 2018

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX

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The Simons Observatory (SO) is an upcoming experiment that will study temperature and polarization fluctuations in the cosmic microwave background (CMB) from the Atacama Desert in Chile. SO will field both a large aperture telescope (LAT) and an array of small aperture telescopes (SATs) that will observe in six bands with center frequencies spanning from 27 to 270 GHz. Key considerations during the SO design phase are vast, including the number of cameras per telescope, focal plane magnification and pixel density, in-band optical power and camera throughput, detector parameter tolerances, and scan strategy optimization. To inform the SO design in a rapid, organized, and traceable manner, we have created a Python-based sensitivity calculator with several state-of-the-art features, including detector-to-detector optical white-noise correlations, a handling of simulated and measured bandpasses, and propagation of low-level parameter uncertainties to uncertainty in on-sky noise performance. We discuss the mathematics of the sensitivity calculation, the calculator's object-oriented structure and key features, how it has informed the design of SO, and how it can enhance instrument design in the broader CMB community, particularly for CMB-S4. Seven cameras are planned for initial deployment within the LAT receiver.† The LAT is designed with a larger FOV that can accommodate up to nineteen cameras, allowing for future LAT receiver upgrades.

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Section: Camera Magnificationmentioning

confidence: 96%

Section: Lat Primary Spillovermentioning

confidence: 99%

BoloCalc: a sensitivity calculator for the design of Simons Observatory

Hill

Bruno

Simon

et al. 2018

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX

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“…The effective focal length of the telescope is f eff = 14.4 m, which means that the ratio f eff / Dm = 2.4. 10 .) The classical crossed-Dragone design is known for having a large FOV, but it is still a "classical" design, in that the primary is a paraboloid and the secondary is a hyperboloid.…”

Section: Optical Designmentioning

confidence: 98%

“…A CCAT first-light camera design is discussed in Vavagiakis et al 2018 7 . An SO science book is in development, an overview of SO instrumentation is presented in Galitzki et al 2018 8 , optical systematics for this telescope design are described in Gallardo et al 2018 9 , cryogenic optics designs are in Dicker et al 2018 10 , and design analyses for the SO LAT receiver are presented in Zhu et al 2018 11 , Orlowski-Scherer et al 2018 12 , and Coppi et al 2018 13 .…”

Section: Introductionmentioning

confidence: 99%

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

Parshley¹,

Niemack²,

Hills³

et al. 2018

Ground-Based and Airborne Telescopes VII

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A common optical design for a coma-corrected, 6-meter aperture, crossed-Dragone telescope has been adopted for the CCAT-prime telescope of CCAT Observatory, Inc., and for the Large Aperture Telescope of the Simons Observatory. Both are to be built in the high altitude Atacama Desert in Chile for submillimeter and millimeter wavelength observations, respectively. The design delivers a high throughput, relatively flat focal plane, with a field of view 7.8 degrees in diameter for 3 mm wavelengths, and the ability to illuminate >100k diffraction-limited beams for < 1 mm wavelengths. The optics consist of offset reflecting primary and secondary surfaces arranged in such a way as to satisfy the Mizuguchi-Dragone criterion, suppressing first-order astigmatism and maintaining high polarization purity. The surface shapes are perturbed from their standard conic forms in order to correct coma aberrations. We discuss the optical design, performance, and tolerancing sensitivity. More information about CCAT-prime can be found at ccatobservatory.org and about Simons Observatory at simonsobservatory.org.

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“…A description of the SO instrument optical design is given in Dicker et al 2018. 10 In Sec. 2 we discuss optical distortions, cross-polar response is discussed in Sec.…”

Section: Introductionmentioning

confidence: 99%

Systematic uncertainties in the Simons Observatory: optical effects and sensitivity considerations

Gallardo¹,

Gudmundsson²,

Koopman³

et al. 2018

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX

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The Simons Observatory (SO) is a new experiment that aims to measure the cosmic microwave background (CMB) in temperature and polarization. SO will measure the polarized sky over a large range of microwave frequencies and angular scales using a combination of small (∼0.5 m) and large (∼6 m) aperture telescopes and will be located in the Atacama Desert in Chile. This work is part of a series of papers studying calibration, sensitivity, and systematic errors for SO. In this paper, we discuss current efforts to model optical systematic effects, how these have been used to guide the design of the SO instrument, and how these studies can be used to inform instrument design of future experiments like CMB-S4. While optical systematics studies are underway for both the small aperture and large aperture telescopes, we limit the focus of this paper to the more mature large aperture telescope design for which our studies include: pointing errors, optical distortions, beam ellipticity, cross-polar response, instrumental polarization rotation and various forms of sidelobe pickup.

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Cold optical design for the large aperture Simons' Observatory telescope

Cited by 19 publications

References 12 publications

BoloCalc: a sensitivity calculator for the design of Simons Observatory

BoloCalc: a sensitivity calculator for the design of Simons Observatory

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

Systematic uncertainties in the Simons Observatory: optical effects and sensitivity considerations

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