scholarly journals High-precision and wide-wavelength range FBG demodulation method based on spectrum correction and data fusion

2021 ◽  
Author(s):  
Guozhen Yao ◽  
YiMeng YIN ◽  
Yongqian Li ◽  
Haonan Yi
Keyword(s):  
Data Fusion ◽  
High Precision ◽  
Wavelength Range ◽  
Wide Wavelength Range ◽  
Spectrum Correction ◽  
Demodulation Method

scholarly journals Diva - A Small Satellite for Global Astrometry and Photometry

1998 ◽  
Vol 11 (1) ◽  
pp. 583-583
Author(s):  
S. Röser ◽  
U. Bastian ◽  
K.S. de Boer ◽  
E. Høg ◽  
E. Schilbach ◽  
...  
Keyword(s):  
High Precision ◽  
Wavelength Range ◽  
Fizeau Interferometer ◽  
Proper Motions ◽  
Small Satellite ◽  
Short Overview ◽  
Photometric Observations ◽  
Photometric Measurements ◽  
First Time ◽  
Astronomy And Astrophysics

DIVA (Double Interferometer for Visual Astrometry) is a Fizeau interferometer on a small satellite. It will perform astrometric and photometric observations of at least 4 million stars. A launch in 2002 and a minimum mission length of 24 months are aimed at. A detailed description of the experiment can be obtained from the DIVA homepage at http://www.aip.de:8080/᷉dso/diva. An overview is given by Röser et al., 1997. The limiting magnitude of DIVA is about V = 15 for spectral types earlier than M0, but drops to about V = 17.5 for stars later than M5. Table 1 gives a short overview on DIVA’s performance. DIVA will carry out a skysurvey complete to V = 12.5. For the first time this survey will comprise precise photometry in at least 8 bands in the wavelength range from 400 to 1000 nm. DIVA will improve parallaxes by a factor of 3 compared to Hipparcos; proper motions by at least a factor of 2 and, in combination with the Hipparcos observations, by a factor of 10 for Hipparcos stars. At least 30 times asmany stars as Hipparcos will be observed, and doing this DIVA will fill the gap in observations between Hipparcos and GAIA. DIVA’s combined astrometric and photometric measurements of high precision will have important impacts on astronomy and astrophysics in the next decade.

Quarter-wave plate tunable in a wide wavelength range

1995 ◽  
Vol 25 (2) ◽  
pp. 187-190 ◽  
Author(s):  
I V Gol'tser ◽  
M Ya Darsht ◽  
Boris Ya Zel'dovich ◽  
N D Kundikova ◽  
L F Rogacheva
Keyword(s):  
Wavelength Range ◽  
Quarter Wave Plate ◽  
Wave Plate ◽  
Wide Wavelength Range ◽  
Quarter Wave

Wide-wavelength range AlGaInAs laser array achieved by selective area growth on heterogenerous InP-on-Si wafer

2021 ◽  
Author(s):  
Claire Besancon ◽  
Delphine Néel ◽  
Giancarlo Cerulo ◽  
Dalila Make ◽  
Nicolas I. Vaissiere ◽  
...  
Keyword(s):  
Wavelength Range ◽  
Selective Area Growth ◽  
Laser Array ◽  
Selective Area ◽  
Wide Wavelength Range ◽  
Area Growth ◽  
Si Wafer

scholarly journals Nanowire photonics toward wide wavelength range and subwavelength confinement [Invited]

2020 ◽  
Vol 10 (10) ◽  
pp. 2560 ◽  
Author(s):  
Masaya Notomi ◽  
Masato Takiguchi ◽  
Sylvain Sergent ◽  
Guoqiang Zhang ◽  
Hisashi Sumikura
Keyword(s):  
Wavelength Range ◽  
Wide Wavelength Range

Synergistic enhancing photoelectrochemical response of Bi10O6S9 with WO3 optical heterojunction in wide wavelength range

2020 ◽  
Vol 509 ◽  
pp. 144697 ◽  
Author(s):  
Changchang Shi ◽  
Xiaowen Zhou ◽  
Wanqing Li ◽  
Hongmei Guo ◽  
Yanjie Zhao ◽  
...  
Keyword(s):  
Wavelength Range ◽  
Photoelectrochemical Response ◽  
Wide Wavelength Range

scholarly journals Faint Galaxy Number-Counts

1996 ◽  
Vol 171 ◽  
pp. 225-228
Author(s):  
N. Metcalfe ◽  
T. Shanks ◽  
R. Fong ◽  
J. Gardner ◽  
N. Roche
Keyword(s):  
Wavelength Range ◽  
Evolutionary History ◽  
Statistical Properties ◽  
Normal Galaxies ◽  
Number Magnitude ◽  
Faint Galaxy ◽  
Wide Wavelength Range ◽  
History Of ◽  
Number Counts ◽  
Additional Constraints

Observers studying the cosmology and evolutionary history of our Universe through the statistical properties of ‘normal’ galaxies have four main tools at their disposal. (1) The number-redshift relation. Although a very powerful diagnostic, spectroscopic surveys are currently limited to B < 24m and significantly incomplete in the range, 23m< B < 24m. (2) Galaxy number-magnitude counts. Although by themselves, they cannot constrain models as tightly as spectroscopy, they can be measured ∼ 4m fainter, where cosmological effects are expected to be significant. (3) Galaxy colours over a wide wavelength range, which provide additional constraints. (4) The dependence of galaxy clustering with magnitude. ω(θ) can be measured to the limit of the counts.Here we report on the latest Durham count and clustering work.

Chiral 2D Organic Inorganic Hybrid Perovskite with Circular Dichroism Tunable Over Wide Wavelength Range

2020 ◽  
Vol 142 (9) ◽  
pp. 4206-4212 ◽  
Author(s):  
Jihoon Ahn ◽  
Sunihl Ma ◽  
Ji-Young Kim ◽  
Jihoon Kyhm ◽  
Wooseok Yang ◽  
...  
Keyword(s):  
Circular Dichroism ◽  
Wavelength Range ◽  
Inorganic Hybrid ◽  
Hybrid Perovskite ◽  
Wide Wavelength Range ◽  
Circular Dichroïsm
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