Intensity fluctuations in laser links between the ground and a satellite

Masahiro Toyoda

doi:10.1364/AO.44.007364

Applied Optics
Vol. 44,
Issue 34,
pp. 7364-7370
(2005)
•https://doi.org/10.1364/AO.44.007364

Intensity fluctuations in laser links between the ground and a satellite

Masahiro Toyoda

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Masahiro Toyoda, "Intensity fluctuations in laser links between the ground and a satellite," Appl. Opt. 44, 7364-7370 (2005)

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Abstract

Laser-beam-intensity fluctuations between an uplink (ground to satellite) and a downlink (satellite to ground) are described. The dependence of the beam radius on log-intensity variance in the uplink and the dependence of receiving-aperture diameter on the log-intensity variance in the downlink using a known theory were calculated. Statistical analysis of the experimental data on the laser links was performed, and high correlation coefficients of 0.94 between the normalized intensity variances of the uplink and those of the stellar scintillation were obtained. The beam-pointing error in the satelliteborne laser transmitter chiefly caused fluctuations in the downlink.

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Component	Characteristics
Transmitting part
Laser	AlGaAs–LD
Wavelength	0.83 µm
Transmitting power	4.1 mW
Beam diameter	7.5 cm
Divergence (full width)	30 µrad
Polarization	Circular
Receiving part
Telescope type	Galilean
Telescope aperture diameter	7.5 cm
Optical detector	Si–APD
Field of view	± 100 µrad
Optical efficiency (at 0.514 µm)	0.098
Minimum detecting power	0.1 nW
Electrical circuit 3 dB Frequency bandwidth	dc −0.4 kHz
Data sampling interval	2 ms

Component	Characteristics
Transmitting part
Laser	Argon-ion laser
Wavelength	0.51 µm
Transmitting power	7.1 W
Beam radius	5.5 cm
Divergence (full width)	23 µrad
Polarization	Linear
Receiving part
Telescope aperture diameter	1.5 m	0.206 m
Telescope type	Cassegrain	Off-axis Mersenne
Optical detector	Si–APD	Si–QD
Field of view	±41 µrad	±70 µrad
Optical efficiency (at 0.83 µm)	0.62	0.24
Electrical circuit 3 dB frequency bandwidth	dc −1 kHz	dc −2.3 kHz
Data sampling interval	1 ms	1 ms

Item	Condition
Time and date	0:28;^a 28 January 1996
Temperature	−0.1 °C
Humidity	64%
Observed star	alpha-UMi (Polaris)
Effective temperature	6300 K
Stellar visual magnitude	2.0
Zenith angle	53°
Wavelength range (FWHM)	0.7–0.9 µm
Noise equivalent power	0.18 pW (0.2 m telescope)
	2.0 pW (1.5 m telescope)
Nominal received power	8.2 pW (0.2 m telescope)
	0.98 nW (1.5 m telescope)

Date	Uplink			Stellar Scintillation

	Time^a	Θ(deg)	$\frac{{σ_{I, up}}^{2}}{{I_{0, up}}^{2}}$	Time^a	Θ(deg)	$\frac{{σ_{I, star (0.2 m)}}^{2}}{{I_{0, star (0.2 m)}}^{2}}$	$\frac{{σ_{I, star (1.5 m)}}^{2}}{{I_{0, star (1.5 m)}}^{2}}$
1995 March 1	19:27	37	1.46	21:33	53	0.132	0.0136
October 21	2:33	41	0.647	1:36	40	0.320	0.000523
November 2	1:49	41	0.999	0:30	23	0.0728	0.00152
November 5	1:44	40	0.905	1:10	23	0.0287	0.00230
December 1	24:25	37	1.15	23:12	53	0.149	0.00124
December 4	24:15	37	1.41	23:08	53	0.0989	0.00957
December 25	23:33	31	2.05	26:42	53	0.389	0.0348
1996 January 9	23:16	31	2.78	25:30	53	0.281	0.0416
January 12	22:55	32	1.35	25:15	53	0.0875	0.00466
January 24	21:17	35	1.97	24:30	53	0.169	0.0428
January 27	21:26	34	0.751	24:46	53	0.0595	0.00386

Component	Characteristics
Transmitting part
Laser	AlGaAs–LD
Wavelength	0.83 µm
Transmitting power	4.1 mW
Beam diameter	7.5 cm
Divergence (full width)	30 µrad
Polarization	Circular
Receiving part
Telescope type	Galilean
Telescope aperture diameter	7.5 cm
Optical detector	Si–APD
Field of view	± 100 µrad
Optical efficiency (at 0.514 µm)	0.098
Minimum detecting power	0.1 nW
Electrical circuit 3 dB Frequency bandwidth	dc −0.4 kHz
Data sampling interval	2 ms

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Applied Optics