Ultracompact and large-scale power splitters on silicon-based two-dimensional photonic crystals at near-infrared wavelengths

2006 ◽  
Vol 45 (2) ◽  
pp. 024601 ◽  
Author(s):  
Yuzhou Zhao
MRS Bulletin ◽  
2001 ◽  
Vol 26 (8) ◽  
pp. 637-641 ◽  
Author(s):  
Vicki L. Colvin

Over a decade ago, theorists predicted that photonic crystals active at visible and near-infrared wavelengths would possess a variety of exciting optical properties. Only in the last several years, however, have experimentalists begun to build materials that realize this potential in the laboratory. This lag between experiment and theory is primarily due to the to the challenges associated with fabricating these unique materials. As the term “crystal” suggests, these samples must consist of highly perfect ordered arrays of solids. However, unlike conventional crystals, which exhibit order on the angstrom length scale, photonic crystals must have order on the submicrometer length scale. In addition, many of the most valuable properties of photonic crystals are only realized when samples possess a “full” photonic bandgap. For such systems, large dielectric contrasts and particular crystal symmetries create a range of frequencies over which light cannot propagate. Realizing the nanoscopic architectures required to form such systems is a challenge for experimentalists. As a result, fabrication schemes that rely on lithographic techniques or spontaneous assembly have been a focus in the development of the field.


2021 ◽  
Vol 2021 (12) ◽  
pp. 009
Author(s):  
Roy Maartens ◽  
José Fonseca ◽  
Stefano Camera ◽  
Sheean Jolicoeur ◽  
Jan-Albert Viljoen ◽  
...  

Abstract Measurements of galaxy clustering in upcoming surveys such as those planned for the Euclid and Roman satellites, and the SKA Observatory, will be sensitive to distortions from lensing magnification and Doppler effects, beyond the standard redshift-space distortions. The amplitude of these contributions depends sensitively on magnification bias and evolution bias in the galaxy number density. Magnification bias quantifies the change in the observed number of galaxies gained or lost by lensing magnification, while evolution bias quantifies the physical change in the galaxy number density relative to the conserved case. These biases are given by derivatives of the number density, and consequently are very sensitive to the form of the luminosity function. We give a careful derivation of the magnification and evolution biases, clarifying a number of results in the literature. We then examine the biases for a variety of surveys, encompassing galaxy surveys and line intensity mapping at radio and optical/near-infrared wavelengths.


2006 ◽  
Vol 12 (10-11) ◽  
pp. 919-922 ◽  
Author(s):  
Jian Zhu ◽  
Yong Zhang ◽  
Bailing Zhou ◽  
Jianfeng Gao ◽  
Shixing Jia

2017 ◽  
Vol 25 (21) ◽  
pp. 25071 ◽  
Author(s):  
Jinyoung Hwang ◽  
Jong Wook Roh

1999 ◽  
Vol 74 (11) ◽  
pp. 1522-1524 ◽  
Author(s):  
R. K. Lee ◽  
O. J. Painter ◽  
B. D’Urso ◽  
A. Scherer ◽  
A. Yariv

Sign in / Sign up

Export Citation Format

Share Document