Sodium UV modeless laser excitation for PLGS

Moldovan, I.; Fesquet, Vincent; Marc, F.; Chatellus, Hugues Guillet de; Pique, J. P.

doi:10.1051/anphys:2008015

Cited by 3 publications

(4 citation statements)

References 1 publication

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“…4 P 3/2 Na excitation at 330 nm has also been proposed (Pique et al 2006) and tested in the laboratory (Moldovan et al 2007;Chen et al 2016), to produce an artificial star with wavelengths as shown in Fig. 1(b).…”

Section: Laser Line #2mentioning

confidence: 99%

A precise photometric ratio via laser excitation of the sodium layer – I. One-photon excitation using 342.78 nm light

Albert

Budker

Chance

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The largest uncertainty on measurements of dark energy using type Ia supernovae is presently due to systematics from photometry; specifically to the relative uncertainty on photometry as a function of wavelength in the optical spectrum. We show that a precise constraint on relative photometry between the visible and near-infrared can be achieved at upcoming survey telescopes, such as at the Vera Rubin Observatory (VRO), via a laser source tuned to the 342.78 nm vacuum excitation wavelength of neutral sodium atoms. Using a high-power laser, this excitation will produce an artificial star, which we term a “laser photometric ratio star” (LPRS) of de-excitation light in the mesosphere at wavelengths in vacuum of 589.16 nm, 589.76 nm, 818.55 nm, and 819.70 nm, with the sum of the numbers of 589.16 nm and 589.76 nm photons produced by this process equal to the sum of the numbers of 818.55 nm and 819.70 nm photons, establishing a precise calibration ratio between, for example, the VRO r and z filters. This technique can thus provide a novel mechanism for establishing a spectrophotometric calibration ratio of unprecedented precision for upcoming telescopic observations across astronomy and atmospheric physics; thus greatly improving the performance of upcoming measurements of dark energy parameters using type Ia supernovae. The second paper of this pair describes an alternative technique to achieve a similar, but brighter, LPRS than the technique described in this paper, by using two lasers near resonances at 589.16 nm and 819.71 nm, rather than the single 342.78 nm on-resonance laser technique described in this paper.

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Section: Laser Line #2mentioning

confidence: 99%

A precise photometric ratio via laser excitation of the sodium layer – I. One-photon excitation using 342.78 nm light

Albert

Budker

Chance

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…The Earth's atmospheric layer of neutral atomic sodium (Na I) (Slipher, 1929) exists between approximately 80 and 105 km above sea level, and originates from the ablation of meteors in the ionosphere (Chapman, 1939;Plane et al, 2015). The total atmospheric column density of sodium varies with time and location between about 2 × 10 9 atoms/cm 2 and 8 × 10 9 atoms/cm 2 (Mégie et al, 1978;Moussaoui et al, 2010). Current LGS typically use solid-state lasers or fiber lasers, a with typical optical output power around 10 -20 W, directed into the mesosphere to produce an artificial star at about 9 magnitude, b which is sufficient for real-time deformable mirror AO image correction at 4 m-class and larger observatories.…”

Section: Existing Related Infrastructure and The Atmospheric Sodium L...mentioning

confidence: 99%

“…PLGS utilizing a single laser tuned to the 4 P 3/2 Na excitation at 330 nm has also been proposed (Pique et al, 2006) and tested in the laboratory (Moldovan et al, 2007;Chen et al, 2016), to produce an artificial star with wavelengths as shown in Fig. 1b.…”

Section: Existing Related Infrastructure and The Atmospheric Sodium L...mentioning

confidence: 99%

A Precise Photometric Ratio via Laser Excitation of the Sodium Layer I: One-photon Excitation Using 342.78 nm Light

Albert,

Budker,

Chance

et al. 2020

Preprint

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The largest uncertainty on measurements of dark energy using type Ia supernovae is presently due to systematics from photometry; specifically to the relative uncertainty on photometry as a function of wavelength in the optical spectrum. We show that a precise constraint on relative photometry between the visible and near-infrared can be achieved at upcoming survey telescopes (such as at the Vera Rubin Observatory [VRO], currently under construction) via a mountaintop-located laser source tuned to the 342.78 nm vacuum excitation wavelength of neutral sodium atoms. Using a high-power (500 W) laser modified from laser guide star studies, this excitation will produce an artificial star (which we term a "laser photometric ratio star," or LPRS) of deexcitation light in the mesosphere that is observable from the ground at approximately 20 magnitude (i.e., well within the expected single-image magnitude limit of VRO) at wavelengths in vacuum of 589.16 nm, 589.76 nm, 818.55 nm, and 819.70 nm, with the sum of the numbers of 589.16 nm and 589.76 nm photons produced by this process equal to the sum of the numbers of 818.55 nm and 819.70 nm photons, establishing a precise calibration ratio between, for example, the VRO r and z filters. This technique can thus provide a novel mechanism for establishing a spectrophotometric calibration ratio of unprecedented precision, from above most of the Earth's atmosphere, for upcoming telescopic observations across astronomy and atmospheric physics.This article is the first in a pair of articles on this topic. The second article of the pair describes an alternative technique to achieve a similar, but brighter, LPRS than the technique described in this paper, by using two mountaintop-located lasers, at optical frequencies approximately 4 GHz away from resonances at wavelengths in vacuum of 589.16 nm and 819.71 nm respectively, rather than the single 342.78 nm on-resonance laser technique described in this paper.

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“…The model shows no dependence of the line-width on the pump energy, with a value that is close to the experimental measurement. Given the hyperfine structure of 1.77 GHz and the Doppler effect of the sodium atom in the mesosphere, simulations have shown [21] that an ideal line-width is 2.8 GHz. Within the model introduced above we calculate that an etalon of equivalent free spectral range, but with a reflection coefficient of 70% on both sides, should be perfectly appropriate for LGS application.…”

Section: Spectral Propertiesmentioning

confidence: 99%

Pulsed frequency-shifted feedback laser for laser guide stars: intracavity preamplifier

2011

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Intensive use of laser guide stars with the new generation of extremely large telescopes and hypertelescopes will require the use of more efficient lasers to surmount novel limitations and aberrations. The pulsed frequency-shifted feedback (FSF) laser we have developed overcomes the saturation of sodium atoms and solves the new problems. This work presents a highly efficient solution for operating pulsed FSF lasers. For the first time, an intracavity preamplifier achieves a gain of 10(4) and more than 40 μJ per pulse, with a near-diffraction-limited beam and without amplified spontaneous emission. Endurance tests have shown that good performance is maintained over several hundred hours.

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Sodium UV modeless laser excitation for PLGS

Cited by 3 publications

References 1 publication

A precise photometric ratio via laser excitation of the sodium layer – I. One-photon excitation using 342.78 nm light

A precise photometric ratio via laser excitation of the sodium layer – I. One-photon excitation using 342.78 nm light

A Precise Photometric Ratio via Laser Excitation of the Sodium Layer I: One-photon Excitation Using 342.78 nm Light

Pulsed frequency-shifted feedback laser for laser guide stars: intracavity preamplifier

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