Performance of ChAOS on the Apache Point Observatory's 3.5-m telescope

Kibblewhite, E. J.; Chun, Mark; Larkin, James E.; Scor, Vijuna; Smutko, Michael F.; Wild, Walter J.

doi:10.1117/12.321726

Cited by 10 publications

(13 citation statements)

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“…From averaging of the between the CCD and PMT F/W March measurements reported in Table 2, it appears that circularly polarizing the beam produces 80% more return than linearly polarizing the outgoing laser. Ge et al (1998) obtained a 30% increase, and Rabien et al (1999) claimed a 30%-50% increase, but Kibblewhite & Shi (1998) reported an increase of 150%. At any rate, it is clear that maximum return will follow from sending the laser out of the telescope circularly polarized.…”

Section: Spot Brightnessmentioning

confidence: 98%

“…Note, however, that these sizes are not from deconvolved measurements; the spots' actual sizes are increased by the telescope point-spread function. Since both the stars and the spots Kibblewhite & Shi 1998;(6) Davies et al 1999;(7) Contos et al 2003;(8) were fit as Gaussians, and since the j of a convolution of two Gaussians is the quadrature sum of the two Gaussians' j's, to first order the spot's actual size ( ) in the mesosphere can be j deduced from Table 3 by decreasing the spot size by the mean star size. Using the star dimensions as listed in Figures 4-6, if the rms for the star is , then j p (j ϩ j )/2 2j p a b a * * *…”

Section: Spot Sizementioning

confidence: 99%

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Photometry of a Sodium Laser Guide Star at the Starfire Optical Range

Drummond¹,

Telle²,

Denman³

et al. 2004

PUBL ASTRON SOC PAC

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ABSTRACT. Measurements of a laser-pumped sodium guide star produced over the Starfire Optical Range in 2002 November show that the brightness of the spot produced by 11.5 W of linearly polarized power on the sky was equivalent to a mag star. However, taking into account that the transmission through a V filter V p 8.0 is only 55% at the wavelength of sodium, its corrected magnitude, , was 7.4, or 800 photons s Ϫ1 cm Ϫ2 at the V 1 top of the telescope. In 2003 March, tests with linearly and then circularly polarized beams out of the telescope showed that a circularly polarized beam from 12 W of power out of the telescope produced a spot with V p 1 (1015 photons s Ϫ1 cm Ϫ2 at the top of the telescope), 0.7 mag brighter than a linearly polarized beam from 7.1 11.1 W of power out of the telescope. Over the 4 nights of experiments over two seasons, the apparent 2j width of the spot varied between 3Љ .6 and 4Љ .6, or 1.6 and 2.0 m at 92 km altitude, and its length through the sodium layer was 4.6-8.5 km, but no variation of spot size with power on the sky was seen.

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Section: Spot Brightnessmentioning

confidence: 98%

Section: Spot Sizementioning

confidence: 99%

Photometry of a Sodium Laser Guide Star at the Starfire Optical Range

Drummond¹,

Telle²,

Denman³

et al. 2004

PUBL ASTRON SOC PAC

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“…1 Much of the technology necessary to correct these erected space systems can be derived from active optical ͑AcO͒ technologies proven in large, groundbased astronomical facilities. 2,3 These ground systems have led the way in showing how to use AcO technologies to maintain figures at low temporal bandwidth in the presence of wind, gravity, and structural disturbances. Additionally, most ground-based systems also exploit adaptive optical ͑AdO͒ technologies to correct higher temporal frequency effects from atmospheric turbulence.…”

Section: Introductionmentioning

confidence: 99%

Field-balanced adaptive optics error function for wide field-of-view space-based systems

McComas¹,

Friedman

2002

Opt. Eng

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Adaptive optics are regularly used in ground-based astronomical telescopes. These applications are characterized by a very narrow (ϳ1 arcmin) field of view. For economic reasons, commercial spacebased earth-observing optical systems must have a field of view as large as possible. We develop a new error function that is an extension of conventional adaptive optics for wide field-of-view optical systems and show that this new error function enables diffraction-limited performance across a large field of view with only one deformable mirror. This new error function allows for reprogramming of aberration control algorithms for particular applications by the use of an addressable weighting function.

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“…As a special kind of microsecond pulse sodium laser, the peak power for a macro-micro mode-locked pulse laser is N times higher than its non-mode-locked value, where N is determined by N = ν YAG /(c/2l), with c being the speed of light, l being the cavity length, and ν YAG being the spectral width of the fundamental laser. This result contributes to an increased SFG conversion efficiency and output power [18], while avoiding saturation of the sodium atoms, due to the chosen duty cycle being shorter than the lifetime of the sodium upper energy level [19].…”

Section: Introductionmentioning

confidence: 99%

High-power narrow-band mode-locked sodium laser via double-stage sum-frequency generation

Yao¹,

Zheng²,

Wang³

et al. 2020

Laser Phys.

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A high-power, narrow-band, mode-locked sodium D 2a laser with a high sum-frequency efficiency is demonstrated by mixing actively mode-locked Nd:YAG 1064 and 1319 nm lasers in two LiB 3 O 5 (LBO) crystals. The mode-locked lasers at 1064 nm (23.02 W output) and 1319 nm (17.98 W output) are generated from two diode, side-pumped, Nd:YAG, master oscillator power amplifier laser systems. A macro-micro pulse sodium beacon laser with a 30.2 W output power, 0.3 GHz (0.3 pm) linewidth, and a beam quality given by M 2 = 1.23 is obtained with a conversion efficiency of 73.6%. Compared with a single LBO crystal, the sum-frequency efficiency is enhanced by 14.5%. A laser coupled amplitude equation model, including the acousto-optic mode-locker, is applied for theoretical and numerical analyses of the sum-frequency conversion efficiency. The experimental results agree well with the theoretical calculations.

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Performance of ChAOS on the Apache Point Observatory's 3.5-m telescope

Cited by 10 publications

References 0 publications

Photometry of a Sodium Laser Guide Star at the Starfire Optical Range

Photometry of a Sodium Laser Guide Star at the Starfire Optical Range

Field-balanced adaptive optics error function for wide field-of-view space-based systems

High-power narrow-band mode-locked sodium laser via double-stage sum-frequency generation

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