Novel method of optical image registration in wide wavelength range using matrix of piezoelectric crystals

2018 ◽  
Author(s):  
Aleksey Pigarev ◽  
Vladimir Fedorov ◽  
Oleg A. Ryabushkin ◽  
Timur Bazarov
Keyword(s):  
Image Registration ◽  
Wavelength Range ◽  
Optical Image ◽  
Piezoelectric Crystals ◽  
Wide Wavelength Range ◽  
Novel Method

scholarly journals HOLBP: Remote Sensing Image Registration Based on Histogram of Oriented Local Binary Pattern Descriptor

2021 ◽  
Vol 13 (12) ◽  
pp. 2328
Author(s):  
Yameng Hong ◽  
Chengcai Leng ◽  
Xinyue Zhang ◽  
Zhao Pei ◽  
Irene Cheng ◽  
...  
Keyword(s):  
Image Registration ◽  
Local Binary Pattern ◽  
Computational Time ◽  
Rotation Invariant ◽  
Edge Information ◽  
Important Research Topic ◽  
New Construction ◽  
Novel Method ◽  
Direction Information ◽  
Angle Calculation

Image registration has always been an important research topic. This paper proposes a novel method of constructing descriptors called the histogram of oriented local binary pattern descriptor (HOLBP) for fast and robust matching. There are three new components in our algorithm. First, we redefined the gradient and angle calculation template to make it more sensitive to edge information. Second, we proposed a new construction method of the HOLBP descriptor and improved the traditional local binary pattern (LBP) computation template. Third, the principle of uniform rotation-invariant LBP was applied to add 10-dimensional gradient direction information to form a 138-dimension HOLBP descriptor vector. The experimental results showed that our method is very stable in terms of accuracy and computational time for different test images.

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.

Sign in / Sign up

Export Citation Format

Share Document