ISOCAM Interactive Analysis User's Manual Version 5.0 - ISO - ESA

246 CHAPTER 20. ADVANCED DATA CALIBRATION
psf dir has to point to a local directory, containing the theoretical PSFs (see Section 15.4.1).
The output of the program is:
• sort wave: wavelength, sorted in ascending order.
• flux: The flux of the point source (one per executed CVF step).
• est flux: The flux of the point source (one per observed wavelength). In case a wavelength
was observed twice, est flux is the mean of both observations.
• est flux error: The error of the point source flux (one per observed wavelength). This
error is computed on the fly by Monte-Carlo simulations.
20.7 Analysis of solar-system-objects
Basic data reduction steps are performed as in chapter 5.2. The exposures of the general
PDScreated with get sscdstruct are dark-corrected, deglitched, transient corrected and also
flat-fielded:
CIA> corr_flat, sso_pds, /cube
As next step, you have to get the ISO centred ephemerids of the solar system object:
CIA> jd = convert_time(sso_pds.utk, ’UTK’, ’MJD’) + 2400000l
CIA> print, min(jd), max(jd), format=(’(d13.4)’)
2450849.0361 2450849.0380 jd contains the time in Julian Date when these data were taken.
Then you have to access the ”HORIZONS On-Line Ephemeris System”
>telnet ssd.jpl.nasa.gov 6775
JPL Horizons, vers SUN-v3.0
Type ‘?’ for brief intro, ‘?!’ for more details
System news updated Jan 15, 2002
Horizons> tempel-tuttle;
>EXACT< name search [SPACE sensitive]:
NAME = TEMPEL-TUTTLE;
Continue [ =yes, n=no, ? ] : y
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JPL/DASTCOM3 Small-body Index Search Results 2002-Feb-26 08:44:47
Comet & asteroid index search:
NAME = TEMPEL-TUTTLE;
Matching small-bodies: