Parallelizing Compiler Framework and API for Power Reduction and Software Productivity of Real-Time Heterogeneous Multicores

Author(s):  
Akihiro Hayashi ◽  
Yasutaka Wada ◽  
Takeshi Watanabe ◽  
Takeshi Sekiguchi ◽  
Masayoshi Mase ◽  
...  
2020 ◽  
Vol 17 (5) ◽  
pp. 1735-1754
Author(s):  
Guilherme Paim ◽  
Gustavo M. Santana ◽  
Brunno A. Abreu ◽  
Leandro M. G. Rocha ◽  
Mateus Grellert ◽  
...  

2010 ◽  
Vol 46 (2) ◽  
pp. 251-300 ◽  
Author(s):  
Heiko Falk ◽  
Paul Lokuciejewski

Abstract The current practice to design software for real-time systems is tedious. There is almost no tool support that assists the designer in automatically deriving safe bounds of the worst-case execution time (WCET) of a system during code generation and in systematically optimizing code to reduce WCET. This article presents concepts and infrastructures for WCET-aware code generation and optimization techniques for WCET reduction. All together, they help to obtain code explicitly optimized for its worst-case timing, to automate large parts of the real-time software design flow, and to reduce costs of a real-time system by allowing to use tailored hardware.


Author(s):  
Jason J. Brown ◽  
Danny Z. Chen ◽  
Garrison W. Greenwood ◽  
Xiaobo Hu ◽  
Richard W. Taylor

2020 ◽  
Vol 17 (6) ◽  
pp. 1991-2004
Author(s):  
Sunil Jacob ◽  
Varun G. Menon ◽  
Saira Joseph ◽  
Paramjit Sehdev

1979 ◽  
Vol 44 ◽  
pp. 41-47
Author(s):  
Donald A. Landman

This paper describes some recent results of our quiescent prominence spectrometry program at the Mees Solar Observatory on Haleakala. The observations were made with the 25 cm coronagraph/coudé spectrograph system using a silicon vidicon detector. This detector consists of 500 contiguous channels covering approximately 6 or 80 Å, depending on the grating used. The instrument is interfaced to the Observatory’s PDP 11/45 computer system, and has the important advantages of wide spectral response, linearity and signal-averaging with real-time display. Its principal drawback is the relatively small target size. For the present work, the aperture was about 3″ × 5″. Absolute intensity calibrations were made by measuring quiet regions near sun center.


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