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The FITS is the standard file format in astronomy, and it has been extended to agree with astronomical needs of the day. However, astronomical datasets have been inflating year by year. In case of ALMA telescope, a ~ TB scale 4-dimensional data cube may be produced for one target. Considering that typical Internet bandwidth is a few 10 MB/s at most, the original data cubes in FITS format are hosted on a VO server, and the region which a user is interested in should be cut out and transferred to the user (Eguchi et al., 2012). The system will equip a very high-speed disk array to process a TB scale data cube in a few 10 seconds, and disk I/O speed, endian conversion and data processing one will be comparable. Hence to reduce the endian conversion time is one of issues to realize our system. In this paper, I introduce a technique named just-in-time endian conversion, which delays the endian conversion for each pixel just before it is really needed, to sweep out the endian conversion time; by applying this method, the FITS processing speed increases 20% for single threading, and 40% for multi-threading compared to CFITSIO. The speed-up by the method tightly relates to modern CPU architecture to improve the efficiency of instruction pipelines due to break of causality, a programmed instruction code sequence.
This document describes a FITS convention developed by the IRAF Group (D. Tody, R. Seaman, and N. Zarate) at the National Optical Astronomical Observatory (NOAO). This convention is implemented by the fgread/fgwrite tasks in the IRAF fitsutil package
Data archiving is one of the most critical issues for modern astronomical observations. With the development of a new generation of radio telescopes, the transfer and archiving of massive remote data have become urgent problems to be solved. Herein,
Ultrahigh accuracy time synchronization technique based on the optical frequency comb and the GHZ radio frequency spiral scanning deflector is suggested to install on the Moon during the ARTEMIS mission. The comparison with the parameters of an analo
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