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1. Cold optical design for the Large Aperture Simons Observatory telescope

Author

Dicker, S. R., Gallardo, P. A., Gudmundsson, J. E, Mauskopf, P. D., Ali, A., Ashton, P. C., Coppi, G., Devlin, M. J., Galitzki, N., Ho, S. P., Hill, C. A., Hubmayr, J., Keating, B., Lee, A. T., Limon, M., Matsuda, F., McMahon, J., Niemack, M. D., Orlowski-Scherer, J. L., Piccirillo, L., Salatino, M., Simon, S. M., Staggs, S. T., Thornton, R., Ullom, J. N., Vavagiakis, E. M., Wollack, E. J., Xu, Z., and Zhu, N.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

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.

Published
2018

2. Erratum: The Simons Observatory Large Aperture Telescope Receiver (ApJS (2021) 256: 23 DOI: 10.3847/1538-4365/ac0db7)

Author

Zhu N., Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dunner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keating, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Zhu N., Bhandarkar T., Coppi G., Kofman A. M., Orlowski-Scherer J. L., Xu Z., Adachi S., Ade P., Aiola S., Austermann J., Bazarko A. O., Beall J. A., Bhimani S., Bond J. R., Chesmore G. E., Choi S. K., Connors J., Cothard N. F., Devlin M., Dicker S., Dober B., Duell C. J., Duff S. M., Dunner R., Fabbian G., Galitzki N., Gallardo P. A., Golec J. E., Haridas S. K., Harrington K., Healy E., Patty Ho S. -P., Huber Z. B., Hubmayr J., Iuliano J., Johnson B. R., Keating B., Kiuchi K., Koopman B. J., Lashner J., Lee A. T., Li Y., Limon M., Link M., Lucas T. J., McCarrick H., Moore J., Nati F., Newburgh L. B., Niemack M. D., Pierpaoli E., Randall M. J., Sarmiento K. P., Saunders L. J., Seibert J., Sierra C., Sonka R., Spisak J., Sutariya S., Tajima O., Teply G. P., Thornton R. J., Tsan T., Tucker C., Ullom J., Vavagiakis E. M., Vissers M. R., Walker S., Westbrook B., Wollack E. J., Zannoni M., Zhu N., Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dunner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keating, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Zhu N., Bhandarkar T., Coppi G., Kofman A. M., Orlowski-Scherer J. L., Xu Z., Adachi S., Ade P., Aiola S., Austermann J., Bazarko A. O., Beall J. A., Bhimani S., Bond J. R., Chesmore G. E., Choi S. K., Connors J., Cothard N. F., Devlin M., Dicker S., Dober B., Duell C. J., Duff S. M., Dunner R., Fabbian G., Galitzki N., Gallardo P. A., Golec J. E., Haridas S. K., Harrington K., Healy E., Patty Ho S. -P., Huber Z. B., Hubmayr J., Iuliano J., Johnson B. R., Keating B., Kiuchi K., Koopman B. J., Lashner J., Lee A. T., Li Y., Limon M., Link M., Lucas T. J., McCarrick H., Moore J., Nati F., Newburgh L. B., Niemack M. D., Pierpaoli E., Randall M. J., Sarmiento K. P., Saunders L. J., Seibert J., Sierra C., Sonka R., Spisak J., Sutariya S., Tajima O., Teply G. P., Thornton R. J., Tsan T., Tucker C., Ullom J., Vavagiakis E. M., Vissers M. R., Walker S., Westbrook B., Wollack E. J., and Zannoni M.

Abstract

After the publication of the article, it was brought to our attention that the description of Equation (1) may cause potential confusion. Thus, we have decided to provide a newer reference and added a unit for qtot in the description. The updated paragraph should read as the following:.

Published
2021

3. Simons Observatory large aperture receiver simulation overview

Author

Orlowski-Scherer, J, Zhu, N, Xu, Z, Ali, A, Arnold, K, Ashton, P, Coppi, G, Devlin, M, Dicker, S, Galitzki, N, Gallardo, P, Keating, B, Lee, A, Limon, M, Lungu, M, May, A, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Salatino, M, Silva-Feaver, M, Simon, S, Thornton, R, Vavagiakis, E, Orlowski-Scherer J. L., Zhu N., Xu Z., Ali A., Arnold K. S., Ashton P. C., Coppi G., Devlin M., Dicker S., Galitzki N., Gallardo P. A., Keating B., Lee A. T., Limon M., Lungu M., May A., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Salatino M., Silva-Feaver M., Simon S. M., Thornton R., Vavagiakis E. M., Orlowski-Scherer, J, Zhu, N, Xu, Z, Ali, A, Arnold, K, Ashton, P, Coppi, G, Devlin, M, Dicker, S, Galitzki, N, Gallardo, P, Keating, B, Lee, A, Limon, M, Lungu, M, May, A, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Salatino, M, Silva-Feaver, M, Simon, S, Thornton, R, Vavagiakis, E, Orlowski-Scherer J. L., Zhu N., Xu Z., Ali A., Arnold K. S., Ashton P. C., Coppi G., Devlin M., Dicker S., Galitzki N., Gallardo P. A., Keating B., Lee A. T., Limon M., Lungu M., May A., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Salatino M., Silva-Feaver M., Simon S. M., Thornton R., and Vavagiakis E. M.

Abstract

The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales between one arcminute and tens of degrees, contain over 60,000 detectors, and sample frequencies between 27 and 270 GHz. SO will consist of a six-meter-aperture telescope coupled to over 30,000 detectors along with an array of half-meter aperture refractive cameras, which together couple to an additional 30,000+ detectors. SO will measure fundamental cosmological parameters of our universe, find high redshift clusters via the Sunyaev-Zeldovich effect, constrain properties of neutrinos, and seek signatures of dark matter through gravitational lensing. In this paper we will present results of the simulations of the SO large aperture telescope receiver (LATR). We will show details of simulations performed to ensure the structural integrity and thermal performance of our receiver, as well as will present the results of finite element analyses (FEA) of designs for the structural support system. Additionally, a full thermal model for the LATR will be described. The model will be used to ensure we meet our design requirements. Finally, we will present the results of FEA used to identify the primary vibrational modes, and planned methods for suppressing these modes. Design solutions to each of these problems that have been informed by simulation will be presented.

Published
2018

4. Simons Observatory large aperture telescope receiver design overview

Author

Zmuidzinas J.,Gao J.-R., Zhu, N, Orlowski-Scherer, J, Xu, Z, Ali, A, Arnold, K, Ashton, P, Coppi, G, Devlin, M, Dicker, S, Galitzki, N, Gallardo, P, Henderson, S, Ho, S, Hubmayr, J, Keating, B, Lee, A, Limon, M, Lungu, M, Mauskopf, P, May, A, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Rao, M, Salatino, M, Silva-Feaver, M, Simon, S, Staggs, S, Thornton, R, Ullom, J, Vavagiakis, E, Westbrook, B, Wollack, E, Zhu N., Orlowski-Scherer J. L., Xu Z., Ali A., Arnold K. S., Ashton P. C., Coppi G., Devlin M. J., Dicker S., Galitzki N., Gallardo P. A., Henderson S. W., Ho S. -P. P., Hubmayr J., Keating B., Lee A. T., Limon M., Lungu M., Mauskopf P. D., May A. J., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Rao M. S., Salatino M., Silva-Feaver M., Simon S. M., Staggs S., Thornton R., Ullom J. N., Vavagiakis E. M., Westbrook B., Wollack E. J., Zmuidzinas J.,Gao J.-R., Zhu, N, Orlowski-Scherer, J, Xu, Z, Ali, A, Arnold, K, Ashton, P, Coppi, G, Devlin, M, Dicker, S, Galitzki, N, Gallardo, P, Henderson, S, Ho, S, Hubmayr, J, Keating, B, Lee, A, Limon, M, Lungu, M, Mauskopf, P, May, A, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Rao, M, Salatino, M, Silva-Feaver, M, Simon, S, Staggs, S, Thornton, R, Ullom, J, Vavagiakis, E, Westbrook, B, Wollack, E, Zhu N., Orlowski-Scherer J. L., Xu Z., Ali A., Arnold K. S., Ashton P. C., Coppi G., Devlin M. J., Dicker S., Galitzki N., Gallardo P. A., Henderson S. W., Ho S. -P. P., Hubmayr J., Keating B., Lee A. T., Limon M., Lungu M., Mauskopf P. D., May A. J., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Rao M. S., Salatino M., Silva-Feaver M., Simon S. M., Staggs S., Thornton R., Ullom J. N., Vavagiakis E. M., Westbrook B., and Wollack E. J.

Abstract

The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales between one arcminute and tens of degrees and sample frequencies between 27 and 270 GHz. Here we present the current design of the large aperture telescope receiver (LATR), a 2.4m diameter cryostat that will be mounted on the SO 6m telescope and will be the largest CMB receiver to date. The cryostat size was chosen to take advantage of the large focal plane area having high Strehl ratios, which is inherent to the Cross-Dragone telescope design. The LATR will be able to accommodate thirteen optics tubes, each having a 36 cm diameter aperture and illuminating several thousand transition-edge sensor (TES) bolometers. This set of equipment will provide an opportunity to make measurements with unparalleled sensitivity. However, the size and complexity of the LATR also pose numerous technical challenges. In the following paper, we present the design of the LATR and include how we address these challenges. The solutions we develop in the process of designing the LATR will be informative for the general CMB community, and for future CMB experiments like CMB-S4.

Published
2018

5. Cooldown strategies and transient thermal simulations for the Simons Observatory

Author

Coppi, G, Xu, Z, Ali, A, Galitzki, N, Gallardo, P, May, A, Orlowski-Scherer, J, Zhu, N, Devlin, M, Dicker, S, Keating, B, Limon, M, Lungu, M, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Salatino, M, Simon, S, Teply, G, Thornton, R, Vavagiakis, E, Coppi G., Xu Z., Ali A., Galitzki N., Gallardo P. A., May A. J., Orlowski-Scherer J. L., Zhu N., Devlin M. J., Dicker S., Keating B., Limon M., Lungu M., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Salatino M., Simon S. M., Teply G., Thornton R., Vavagiakis E. M., Coppi, G, Xu, Z, Ali, A, Galitzki, N, Gallardo, P, May, A, Orlowski-Scherer, J, Zhu, N, Devlin, M, Dicker, S, Keating, B, Limon, M, Lungu, M, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Salatino, M, Simon, S, Teply, G, Thornton, R, Vavagiakis, E, Coppi G., Xu Z., Ali A., Galitzki N., Gallardo P. A., May A. J., Orlowski-Scherer J. L., Zhu N., Devlin M. J., Dicker S., Keating B., Limon M., Lungu M., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Salatino M., Simon S. M., Teply G., Thornton R., and Vavagiakis E. M.

Abstract

The Simons Observatory (SO) will provide precision polarimetry of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales from arc-minutes to tens of degrees, contain over 60,000 detectors, and observe in frequency bands between 27 GHz and 270 GHz. SO will consist of a six-meter-aperture telescope initially coupled to roughly 35,000 detectors along with an array of half-meter aperture refractive cameras, coupled to an additional 30,000+ detectors. The large aperture telescope receiver (LATR) is coupled to the SO six-meter crossed Dragone telescope and will be 2.4 m in diameter, weigh over 3 metric tons, and have five cryogenic stages (80 K, 40 K, 4 K, 1 K and 100 mK). The LATR is coupled to the telescope via 13 independent optics tubes containing cryogenic optical elements and detectors. The cryostat will be cooled by two Cryomech PT90 (80 K) and three Cryomech PT420 (40 K and 4 K) pulse tube cryocoolers, with cooling of the 1 K and 100 mK stages by a commercial dilution refrigerator system. The secondo component, the small aperture telescope (SAT), is a single optics tube refractive cameras of 42 cm diameter. Cooling of the SAT stages will be provided by two Cryomech PT420, one of which is dedicated to the dilution refrigeration system which will cool the focal plane to 100 mK. SO will deploy a total of three SATs. In order to estimate the cool down time of the camera systems given their size and complexity, a finite difference code based on an implicit solver has been written to simulate the transient thermal behavior of both cryostats. The result from the simulations presented here predict a 35 day cool down for the LATR. The simulations suggest additional heat switches between stages would be effective in distribution cool down power and reducing the time it takes for the LATR to reach its base temperatures. The SAT is predicted to cool down in one week, which meets the SO design goals.

Published
2018

6. Cold optical design for the large aperture Simons' Observatory telescope

Author

Dicker, S, Gallardo, P, Gudmudsson, J, Mauskopf, P, Ali, A, Ashton, P, Coppi, G, Devlin, M, Galitzki, N, Ho, S, Hill, C, Hubmayr, J, Keating, B, Lee, A, Limon, M, Matsuda, F, Mcmahon, J, Niemack, M, Orlowski-Scherer, J, Piccirillo, L, Salatino, M, Simon, S, Staggs, S, Thornton, R, Ullom, J, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Dicker S. R., Gallardo P. A., Gudmudsson J. E., Mauskopf P. D., Ali A., Ashton P. C., Coppi G., Devlin M. J., Galitzki N., Ho S. P., Hill C. A., Hubmayr J., Keating B., Lee A. T., Limon M., Matsuda F., McMahon J., Niemack M. D., Orlowski-Scherer J. L., Piccirillo L., Salatino M., Simon S. M., Staggs S. T., Thornton R., Ullom J. N., Vavagiakis E. M., Wollack E. J., Xu Z., Zhu N., Dicker, S, Gallardo, P, Gudmudsson, J, Mauskopf, P, Ali, A, Ashton, P, Coppi, G, Devlin, M, Galitzki, N, Ho, S, Hill, C, Hubmayr, J, Keating, B, Lee, A, Limon, M, Matsuda, F, Mcmahon, J, Niemack, M, Orlowski-Scherer, J, Piccirillo, L, Salatino, M, Simon, S, Staggs, S, Thornton, R, Ullom, J, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Dicker S. R., Gallardo P. A., Gudmudsson J. E., Mauskopf P. D., Ali A., Ashton P. C., Coppi G., Devlin M. J., Galitzki N., Ho S. P., Hill C. A., Hubmayr J., Keating B., Lee A. T., Limon M., Matsuda F., McMahon J., Niemack M. D., Orlowski-Scherer J. L., Piccirillo L., Salatino M., Simon S. M., Staggs S. T., Thornton R., Ullom J. N., Vavagiakis E. M., Wollack E. J., Xu Z., and Zhu N.

Abstract

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.

Published
2018

7. Studies of Systematic uncertainties in the Simons Observatory: Optical effects and sensitivity considerations

Author

Gallardo, P, Gudmundsson, J, Koopman, B, Matsuda, F, Simon, S, Ali, A, Bryan, S, Chinone, Y, Coppi, G, Cothard, N, Devlin, M, Dicker, S, Fabbian, G, Galitzki, N, Hill, C, Keating, B, Kusaka, A, Lashner, J, Lee, A, Limon, M, Mauskopf, P, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Puglisi, G, Reichardt, C, Salatino, M, Staggs, S, Suzuki, A, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Gallardo P. A., Gudmundsson J., Koopman B. J., Matsuda F. T., Simon S. M., Ali A., Bryan S., Chinone Y., Coppi G., Cothard N., Devlin M. J., Dicker S., Fabbian G., Galitzki N., Hill C. A., Keating B., Kusaka A., Lashner J., Lee A. T., Limon M., Mauskopf P. D., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Puglisi G., Reichardt C. L., Salatino M., Staggs S., Suzuki A., Vavagiakis E. M., Wollack E. J., Xu Z., Zhu N., Gallardo, P, Gudmundsson, J, Koopman, B, Matsuda, F, Simon, S, Ali, A, Bryan, S, Chinone, Y, Coppi, G, Cothard, N, Devlin, M, Dicker, S, Fabbian, G, Galitzki, N, Hill, C, Keating, B, Kusaka, A, Lashner, J, Lee, A, Limon, M, Mauskopf, P, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Puglisi, G, Reichardt, C, Salatino, M, Staggs, S, Suzuki, A, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Gallardo P. A., Gudmundsson J., Koopman B. J., Matsuda F. T., Simon S. M., Ali A., Bryan S., Chinone Y., Coppi G., Cothard N., Devlin M. J., Dicker S., Fabbian G., Galitzki N., Hill C. A., Keating B., Kusaka A., Lashner J., Lee A. T., Limon M., Mauskopf P. D., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Puglisi G., Reichardt C. L., Salatino M., Staggs S., Suzuki A., Vavagiakis E. M., Wollack E. J., Xu Z., and Zhu N.

Abstract

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.

Published
2018

8. The Simons Observatory: Instrument overview

Author

Jonas Zmuidzinas, Jian-Rong Gao, Galitzki, N, Ali, A, Arnold, K, Ashton, P, Austermann, J, Baccigalupi, C, Baildon, T, Barron, D, Beall, J, Beckman, S, Bruno, S, Bryan, S, Calisse, P, Chesmore, G, Chinone, Y, Choi, S, Coppi, G, Crowley, K, Cukierman, A, Devlin, M, Dicker, S, Dober, B, Duff, S, Dunkley, J, Fabbian, G, Gallardo, P, Gerbino, M, Goeckner-Wald, N, Golec, J, Gudmundsson, J, Healy, E, Henderson, S, Hill, C, Hilton, G, Ho, S, Howe, L, Hubmayr, J, Jeong, O, Keating, B, Koopman, B, Kiuchi, K, Kusaka, A, Lashner, J, Lee, A, Li, Y, Limon, M, Lungu, M, Matsuda, F, Mauskopf, P, May, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Piccirillo, L, Sathyanarayana Rao, M, Raum, C, Salatino, M, Seibert, J, Sierra, C, Silva-Feaver, M, Simon, S, Staggs, S, Stevens, J, Suzuki, A, Teply, G, Thornton, R, Tsai, C, Ullom, J, Vavagiakis, E, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, Galitzki N., Ali A., Arnold K. S., Ashton P. C., Austermann J. E., Baccigalupi C., Baildon T., Barron D., Beall J. A., Beckman S., Bruno S. M. M., Bryan S., Calisse P. G., Chesmore G. E., Chinone Y., Choi S. K., Coppi G., Crowley K. D., Crowley K. T., Cukierman A., Devlin M. J., Dicker S., Dober B., Duff S. M., Dunkley J., Fabbian G., Gallardo P. A., Gerbino M., Goeckner-Wald N., Golec J. E., Gudmundsson J. E., Healy E. E., Henderson S., Hill C. A., Hilton G. C., Ho S. -P. P., Howe L. A., Hubmayr J., Jeong O., Keating B., Koopman B. J., Kiuchi K., Kusaka A., Lashner J., Lee A. T., Li Y., Limon M., Lungu M., Matsuda F., Mauskopf P. D., May A. J., McCallum N., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Piccirillo L., Sathyanarayana Rao M., Raum C., Salatino M., Seibert J. S., Sierra C., Silva-Feaver M., Simon S. M., Staggs S. T., Stevens J. R., Suzuki A., Teply G., Thornton R., Tsai C., Ullom J. N., Vavagiakis E. M., Vissers M. R., Westbrook B., Wollack E. J., Xu Z., Zhu N., Jonas Zmuidzinas, Jian-Rong Gao, Galitzki, N, Ali, A, Arnold, K, Ashton, P, Austermann, J, Baccigalupi, C, Baildon, T, Barron, D, Beall, J, Beckman, S, Bruno, S, Bryan, S, Calisse, P, Chesmore, G, Chinone, Y, Choi, S, Coppi, G, Crowley, K, Cukierman, A, Devlin, M, Dicker, S, Dober, B, Duff, S, Dunkley, J, Fabbian, G, Gallardo, P, Gerbino, M, Goeckner-Wald, N, Golec, J, Gudmundsson, J, Healy, E, Henderson, S, Hill, C, Hilton, G, Ho, S, Howe, L, Hubmayr, J, Jeong, O, Keating, B, Koopman, B, Kiuchi, K, Kusaka, A, Lashner, J, Lee, A, Li, Y, Limon, M, Lungu, M, Matsuda, F, Mauskopf, P, May, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Piccirillo, L, Sathyanarayana Rao, M, Raum, C, Salatino, M, Seibert, J, Sierra, C, Silva-Feaver, M, Simon, S, Staggs, S, Stevens, J, Suzuki, A, Teply, G, Thornton, R, Tsai, C, Ullom, J, Vavagiakis, E, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, Galitzki N., Ali A., Arnold K. S., Ashton P. C., Austermann J. E., Baccigalupi C., Baildon T., Barron D., Beall J. A., Beckman S., Bruno S. M. M., Bryan S., Calisse P. G., Chesmore G. E., Chinone Y., Choi S. K., Coppi G., Crowley K. D., Crowley K. T., Cukierman A., Devlin M. J., Dicker S., Dober B., Duff S. M., Dunkley J., Fabbian G., Gallardo P. A., Gerbino M., Goeckner-Wald N., Golec J. E., Gudmundsson J. E., Healy E. E., Henderson S., Hill C. A., Hilton G. C., Ho S. -P. P., Howe L. A., Hubmayr J., Jeong O., Keating B., Koopman B. J., Kiuchi K., Kusaka A., Lashner J., Lee A. T., Li Y., Limon M., Lungu M., Matsuda F., Mauskopf P. D., May A. J., McCallum N., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Piccirillo L., Sathyanarayana Rao M., Raum C., Salatino M., Seibert J. S., Sierra C., Silva-Feaver M., Simon S. M., Staggs S. T., Stevens J. R., Suzuki A., Teply G., Thornton R., Tsai C., Ullom J. N., Vavagiakis E. M., Vissers M. R., Westbrook B., Wollack E. J., Xu Z., and Zhu N.

Abstract

The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales between 1 arcminute and tens of degrees, contain over 40,000 detectors, and sample frequencies between 27 and 270 GHz. SO will consist of a six-meter-aperture telescope coupled to over 20,000 detectors along with an array of half-meter aperture refractive cameras, coupled to an additional 20,000+ detectors. The unique combination of large and small apertures in a single CMB observatory, which will be located in the Atacama Desert at an altitude of 5190 m, will allow us to sample a wide range of angular scales over a common survey area. SO will measure fundamental cosmological parameters of our universe, find high redshift clusters via the Sunyaev-Zeldovich effect, constrain properties of neutrinos, and seek signatures of dark matter through gravitational lensing. The complex set of technical and science requirements for this experiment has led to innovative instrumentation solutions which we will discuss. The large aperture telescope will couple to a cryogenic receiver that is 2.4 m in diameter and over 2 m long, creating a number of interesting technical challenges. Concurrently, we are designing an array of half-meter-aperture cryogenic cameras which also have compelling design challenges. We will give an overview of the drivers for and designs of the SO telescopes and the cryogenic cameras that will house the cold optical components and detector arrays.

Published
2018

10. Cold optical design for the large aperture Simons' Observatory telescope

Author

Marshall, Heather K., Spyromilio, Jason, Dicker, S. R., Gallardo, P. A., Gudmudsson, J. E., Mauskopf, P. D., Ali, A., Ashton, P. C., Coppi, G., Devlin, M. J., Galitzki, N., Ho, S. P., Hill, C. A., Hubmayr, J., Keating, B., Lee, A. T., Limon, M., Matsuda, F., McMahon, J., Niemack, M. D., Orlowski-Scherer, J. L., Piccirillo, L., Salatino, M., Simon, S. M., Staggs, S. T., Thornton, R., Ullom, J. N., Vavagiakis, E. M., Wollack, E. J., Xu, Z., and Zhu, N.

Published
2018
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