Nd:YAG lasers at 1064 nm with 1-Hz linewidth

Jiang, Yanyi; Fang, Shun; Bi, Zhiyi; Xu, Xiaojun; Ma, Lei

doi:10.1007/s00340-009-3735-1

Cited by 25 publications

(14 citation statements)

References 32 publications

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“…If the OSETI laser lines are narrow ( 0.01 nm), the wavelength should be chosen by ETI so that they do not occur exactly at a noise peak ( Figure 6). Nd:YAG laser lines can be extremely narrow (< 1 Hz, Uehara & Ueda 1993;Webster et al 2004;Jiang et al 2009). Then, other factors set an observational limit (e.g., for filters at the receiver), such as Earth's rotation and motion around the Sun (∆λ 0.1 nm), and the time-bandwidth limit from the Heisenberg (1927) uncertainty principle, ∆f ∆t 1.…”

Section: Atmospheric Noisementioning

confidence: 99%

Interstellar communication: The colors of optical SETI

Hippke

2018

J Astrophys Astron

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It has recently been argued from a laser engineering point of view that there are only a few magic colors for optical SETI. These are primarily the Nd:YAG line at 1,064 nm and its second harmonic (532.1 nm). Next best choices would be the sum frequency and/or second harmonic generation of Nd:YAG and Nd:YLF laser lines, 393.8 nm (near Fraunhofer CaK), 656.5 nm (Hα) and 589.1 nm (NaD2). In this paper, we examine the interstellar extinction, atmospheric transparency and scintillation, as well as noise conditions for these laser lines. For strong signals, we find that optical wavelengths are optimal for distances d kpc. Nd:YAG at λ = 1,064 nm is a similarly good choice, within a factor of two, under most conditions and out to d 3 kpc. For weaker transmitters, where the signal-to-noise ratio with respect to the blended host star is relevant, the optimal wavelength depends on the background source, such as the stellar type. Fraunhofer spectral lines, while providing lower stellar background noise, are irrelevant in most use cases, as they are overpowered by other factors. Laser-pushed spaceflight concepts, such as "Breakthrough Starshot", would produce brighter and tighter beams than ever assumed for OSETI. Such beamers would appear as naked eye stars out to kpc distances. If laser physics has already matured and converged on the most efficient technology, the laser line of choice for a given scenario (e.g., Nd:YAG for strong signals) can be observed with a narrow filter to dramatically reduce background noise, allowing for large field-of-view observations in fast surveys.

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Section: Atmospheric Noisementioning

confidence: 99%

Interstellar communication: The colors of optical SETI

Hippke

2018

J Astrophys Astron

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“…By using the Pound-Drever-Hall (PDH) technique [9] to stabilize a laser frequency to the resonance of an ultrastable optical Fabry-Perot (FP) reference cavity, frequency noise of a laser can be largely reduced, and their original linewidth of several kilohertz or even megahertz can be narrowed to the hertz level or even lower [5,6,[10][11][12][13][14][15][16][17]. In our previous work [16], two 1 Hz-linewidth Nd:YAG lasers at 1064 nm have been realized by stabilizing them independently to two separately located, vertically mounted ultrastable reference cavities.…”

Section: Introductionmentioning

confidence: 99%

“…In our previous work [16], two 1 Hz-linewidth Nd:YAG lasers at 1064 nm have been realized by stabilizing them independently to two separately located, vertically mounted ultrastable reference cavities. In this work, improvements on the two laser systems have been made to further optimize their performance: (1) homemade acoustic isolation chambers with temperature stabilizations;…”

Section: Introductionmentioning

confidence: 99%

Frequency stabilization of Nd:YAG lasers with a most probable linewidth of 06 Hz

et al. 2013

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Two Nd:YAG lasers at 1064 nm are independently frequency-stabilized to two separately located, vertically mounted ultrastable Fabry-Perot reference cavities. Measurements show that each laser system has achieved a most probable linewidth of 0.6 Hz and fractional frequency instability of ∼1.2 × 10 −15 between 1 and 40 s averaging time. Systematic evaluation shows that the performance of each laser system is limited by thermal noise of the reference cavity.

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“…In a cavity-stabilized laser system, the power of light incident onto a cavity is stabilized since the power fluctuation of cavity resonant light induces temperature fluctuation and thus the cavity length fluctuation is due to thermal expansion (TE) and the thermo-refractive (TR) effect. Fractional power instability of 1 × 10 −4 can be achieved after stabilization [12] . Usually, the power-dependent frequency shift of a cavity-stabilized laser is measured to be a few tens of hertz/microwatt (Hz/μW) [12] , corresponding to a cavity length sensitivity at the 10 −14 m∕μW level.…”

mentioning

confidence: 99%

“…Fractional power instability of 1 × 10 −4 can be achieved after stabilization [12] . Usually, the power-dependent frequency shift of a cavity-stabilized laser is measured to be a few tens of hertz/microwatt (Hz/μW) [12] , corresponding to a cavity length sensitivity at the 10 −14 m∕μW level. For a 10-cm-long cavity made of ultra-low expansion (ULE) glass, the light power fluctuation-induced fractional length instability is nearly 10 −16 , while the thermal-noiselimited length instability of the cavity at room temperature is approximately 8 × 10 −16 .…”

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confidence: 99%

Study on the sensitivity of optical cavity length to light power fluctuation

Jiang

et al. 2016

中国光学快报

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The length stability of optical cavities is vital in ultra-stable, cavity-stabilized laser systems. Using finite element analysis, we study the length deviation of optical cavities due to thermal expansion and thermo-refractive effects when the incident light power is changed. The simulated fractional length sensitivity of a 7.75-cm-long football cavity to the power fluctuation of incident light is 5 × 10 −14 ∕μW, which is in agreement with the experimental results found by measuring the frequency change of a cavity-stabilized laser when the incident light power is changed. Based on the simulation, the cavity sensitivity to light power fluctuation is found to depend on the cavity size and material.

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Nd:YAG lasers at 1064 nm with 1-Hz linewidth

Cited by 25 publications

References 32 publications

Interstellar communication: The colors of optical SETI

Interstellar communication: The colors of optical SETI

Frequency stabilization of Nd:YAG lasers with a most probable linewidth of 06 Hz

Study on the sensitivity of optical cavity length to light power fluctuation

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