Growth of high‐quality GaxIn1−xAsyP1−yby chemical beam epitaxy

1987 ◽  
Vol 51 (10) ◽  
pp. 761-763 ◽  
Author(s):  
W. T. Tsang ◽  
E. F. Schubert ◽  
T. H. Chiu ◽  
J. E. Cunningham ◽  
E. G. Burkhardt ◽  
...  
1993 ◽  
Vol 62 (14) ◽  
pp. 1653-1655 ◽  
Author(s):  
Y. R. Xing ◽  
Z. Jamal ◽  
T. B. Joyce ◽  
T. J. Bullough ◽  
C. J. Kiely ◽  
...  

1996 ◽  
Vol 164 (1-4) ◽  
pp. 202-207 ◽  
Author(s):  
W. Tong ◽  
B.K. Wagner ◽  
T.K. Tran ◽  
W. Ogle ◽  
W. Park ◽  
...  

1992 ◽  
Vol 120 (1-4) ◽  
pp. 130-134 ◽  
Author(s):  
H. Rothfritz ◽  
G. Tränkle ◽  
R. Müller ◽  
G. Weimann

1987 ◽  
Vol 102 ◽  
Author(s):  
T. H. Chiu ◽  
E. F. Schubert ◽  
J. E. Cunningham ◽  
W. T. Tsang ◽  
B. Tell

ABSTRACTHigh quality GaAs layers have been grown by chemical beam epitaxy using triethylgallium and arsine. Undoped GaAs epilayer with net acceptor concentration NA - ND = 3}10 14cm-3 has been obtained at a low growth temperature of 500°C. Si dopant diffusion at such low temperature during growth is negligible. Using monolayer doping technique epilayers with Si impurities localized in a 2-dimensional plane were prepared. Capacitance-voltage profiling showed a high sheet electron concentration of lx1013cm-2 and peak widths of 22Å and 18Å at 300K and 77K, respectively, which are the narrowest ever reported. For samples grown or annealed at higher temperatures, significant impurity diffusion was observed.


1997 ◽  
Vol 15 (1) ◽  
pp. 29-33 ◽  
Author(s):  
R. T. H. Rongen ◽  
M. R. Leys ◽  
P. J. van Hall ◽  
H. Vonk ◽  
J. H. Wolter

2011 ◽  
Vol 11 (5) ◽  
pp. 1896-1900 ◽  
Author(s):  
Alexander T. Vogel ◽  
Johannes de Boor ◽  
Joerg V. Wittemann ◽  
Samuel L. Mensah ◽  
Peter Werner ◽  
...  

1966 ◽  
Vol 24 ◽  
pp. 51-52
Author(s):  
E. K. Kharadze ◽  
R. A. Bartaya

The unique 70-cm meniscus-type telescope of the Abastumani Astrophysical Observatory supplied with two objective prisms and the seeing conditions characteristic at Mount Kanobili (Abastumani) permit us to obtain stellar spectra of a high quality. No additional design to improve the “climate” immediately around the telescope itself is being applied. The dispersions and photographic magnitude limits are 160 and 660Å/mm, and 12–13, respectively. The short-wave end of spectra reaches 3500–3400Å.


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