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Applied Optics
Vol. 46,
Issue 17,
pp. 3444-3454
(2007)
•https://doi.org/10.1364/AO.46.003444

Optical design of the Atacama Cosmology Telescope and the Millimeter Bolometric Array Camera

J. W. Fowler, M. D. Niemack, S. R. Dicker, A. M. Aboobaker, P. A. R. Ade, E. S. Battistelli, M. J. Devlin, R. P. Fisher, M. Halpern, P. C. Hargrave, A. D. Hincks, M. Kaul, J. Klein, J. M. Lau, M. Limon, T. A. Marriage, P. D. Mauskopf, L. Page, S. T. Staggs, D. S. Swetz, E. R. Switzer, R. J. Thornton, and C. E. Tucker

Author Information

Author Affiliations

J. W. Fowler,^1,^*M. D. Niemack,¹S. R. Dicker,²A. M. Aboobaker,^1,³P. A. R. Ade,⁴E. S. Battistelli,⁵M. J. Devlin,²R. P. Fisher,¹M. Halpern,⁵P. C. Hargrave,⁴A. D. Hincks,¹M. Kaul,²J. Klein,²J. M. Lau,¹M. Limon,²T. A. Marriage,^1,⁶P. D. Mauskopf,⁴L. Page,¹S. T. Staggs,¹D. S. Swetz,²E. R. Switzer,¹R. J. Thornton,²and C. E. Tucker⁴

¹Department of Physics, Princeton University, Jadwin Hall, Washington Road, Princeton, New Jersey 08544, USA

²Department of Physics and Astronomy, University of Pennsylvania, David Rittenhouse Laboratory, 209 South 33rd Street, Philadelphia, Pennsylvania 19104, USA

³Present address: School of Physics and Astronomy, University of Minnesota, 116 Church Street SE, Minneapolis, Minnesota 55455, USA

⁴School of Physics and Astronomy, Cardiff University, Queens Buildings, 5 The Parade, Cardiff CF24 3AA, Wales, UK

⁵Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada

⁶Present address: Department of Astrophysical Sciences, Princeton University, Peyton Hall, Ivy Lane, Princeton, New Jersey 08544, USA

^*Corresponding author:jfowler@princeton.edu

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J. W. Fowler, M. D. Niemack, S. R. Dicker, A. M. Aboobaker, P. A. R. Ade, E. S. Battistelli, M. J. Devlin, R. P. Fisher, M. Halpern, P. C. Hargrave, A. D. Hincks, M. Kaul, J. Klein, J. M. Lau, M. Limon, T. A. Marriage, P. D. Mauskopf, L. Page, S. T. Staggs, D. S. Swetz, E. R. Switzer, R. J. Thornton, and C. E. Tucker, "Optical design of the Atacama Cosmology Telescope and the Millimeter Bolometric Array Camera," Appl. Opt.46, 3444-3454 (2007)
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Table of Contents Category
- Geometrical optics
Optics & Photonics Topics
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The topics in this list come from theOptics and Photonics Topics applied to this article.

History
- Original Manuscript: December 20, 2006
- Manuscript Accepted: January 19, 2007
- Published: May 18, 2007

Abstract

The Atacama Cosmology Telescope is a 6 m telescope designed to mapthe cosmic microwave background simultaneously at 145, 215,and $280 GHz$ with arcminute resolution. Each frequency will have a 32 by32 element focal plane array of transition edge sensor bolometers. The telescope and the cold reimaging optics are optimized formillimeter-wave observations with these sensitive detectors. The design of each is described.

Full Article | PDF Article

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Applied Optics

Peter Andersen, Editor-in-Chief

Table 1

Requirements and Features of the Atacama Cosmology Telescope Optics

Warm Telescope Optics
• Clear aperture (off-axis optics) to minimize scattering and blockage.
• 6 m primary mirror and 2 m (maximum) secondary mirror diameters.
• Very fast primary focus (F ≤ 1) to keep the telescope compact.
• Large (1.0°) and fast (F ∼ 2.5) diffraction-limited focal plane.
• Ground loading (due to spillover) smaller than atmospheric loading.
• Space for structure and cryogenics between primary mirror and Gregorian focus.
• Entire telescope must scan several degrees in azimuth at 10 cycles per minute.
Cold Reimaging Optics for MBAC
• Bandpasses 20–30 GHz wide, centered near 145, 215, and 280 GHz.
• Approximately 22 arc min square field of view in each band.
• Diffraction-limited resolution on three 34 mm × 36 mm arrays.
• Well-defined Lyot stop in all bands to maximize illumination of the primary.
• Ghost images due to stray light no brighter than the diffraction-limited sidelobes.

Table 2

Atacama Cosmology Telescope Mirror Shapes^a

Mirror	z_vert (m)	R (m)	K	y₀ (m)	a (m)	b (m)
Primary	0.0000	−10.0000	−0.940935	5.000	3.000	3.000
Secondary	−6.6625	2.4938	−0.322366	−1.488	1.020	0.905
Gregorian focus^b	−1.6758

^a Eq. (1) gives the full shapes; parameters and axes are defined in the text.
^b Best-fit focal plane location for objects at infinity.

Tables (2)

Table 1

Requirements and Features of the Atacama Cosmology Telescope Optics

Warm Telescope Optics
• Clear aperture (off-axis optics) to minimize scattering and blockage.
• 6 m primary mirror and 2 m (maximum) secondary mirror diameters.
• Very fast primary focus (F ≤ 1) to keep the telescope compact.
• Large (1.0°) and fast (F ∼ 2.5) diffraction-limited focal plane.
• Ground loading (due to spillover) smaller than atmospheric loading.
• Space for structure and cryogenics between primary mirror and Gregorian focus.
• Entire telescope must scan several degrees in azimuth at 10 cycles per minute.
Cold Reimaging Optics for MBAC
• Bandpasses 20–30 GHz wide, centered near 145, 215, and 280 GHz.
• Approximately 22 arc min square field of view in each band.
• Diffraction-limited resolution on three 34 mm × 36 mm arrays.
• Well-defined Lyot stop in all bands to maximize illumination of the primary.
• Ghost images due to stray light no brighter than the diffraction-limited sidelobes.

Table 2

Atacama Cosmology Telescope Mirror Shapes^a

Mirror	z_vert (m)	R (m)	K	y₀ (m)	a (m)	b (m)
Primary	0.0000	−10.0000	−0.940935	5.000	3.000	3.000
Secondary	−6.6625	2.4938	−0.322366	−1.488	1.020	0.905
Gregorian focus^b	−1.6758

^a Eq. (1) gives the full shapes; parameters and axes are defined in the text.
^b Best-fit focal plane location for objects at infinity.

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