Cross-talk analysis for optical backplane using two-dimensional beam array from VCSEL and microlens array

Author(s):  
Gicherl Kim ◽  
Ray T. Chen
Author(s):  
Tong Zhou ◽  
Qiang Du ◽  
Tyler Sano ◽  
Russell Wilcox ◽  
Wim Leemans

2013 ◽  
Vol 88 (1) ◽  
Author(s):  
M. J. Piotrowicz ◽  
M. Lichtman ◽  
K. Maller ◽  
G. Li ◽  
S. Zhang ◽  
...  

2010 ◽  
Vol 18 (23) ◽  
pp. 23900 ◽  
Author(s):  
Zhenfu Wang ◽  
Yongqiang Ning ◽  
Yan Zhang ◽  
Jingjing Shi ◽  
Xing Zhang ◽  
...  

Langmuir ◽  
2006 ◽  
Vol 22 (17) ◽  
pp. 7358-7363 ◽  
Author(s):  
Hye Jin Nam ◽  
Duk-Young Jung ◽  
Gi-Ra Yi ◽  
Hyun Choi

1966 ◽  
Vol 24 ◽  
pp. 118-119
Author(s):  
Th. Schmidt-Kaler

I should like to give you a very condensed progress report on some spectrophotometric measurements of objective-prism spectra made in collaboration with H. Leicher at Bonn. The procedure used is almost completely automatic. The measurements are made with the help of a semi-automatic fully digitized registering microphotometer constructed by Hög-Hamburg. The reductions are carried out with the aid of a number of interconnected programmes written for the computer IBM 7090, beginning with the output of the photometer in the form of punched cards and ending with the printing-out of the final two-dimensional classifications.


1966 ◽  
Vol 24 ◽  
pp. 3-5
Author(s):  
W. W. Morgan

1. The definition of “normal” stars in spectral classification changes with time; at the time of the publication of theYerkes Spectral Atlasthe term “normal” was applied to stars whose spectra could be fitted smoothly into a two-dimensional array. Thus, at that time, weak-lined spectra (RR Lyrae and HD 140283) would have been considered peculiar. At the present time we would tend to classify such spectra as “normal”—in a more complicated classification scheme which would have a parameter varying with metallic-line intensity within a specific spectral subdivision.


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