Number of filters defined = 9 NF Wavelngth Freq. Width HPBW 1 2000 146.0 39.0 33.8 2 1300 221.0 60.0 22.3 3 1100 264.0 60.0 18.7 4 850 350.0 30.0 14.0 5 750 407.0 30.0 12.1 6 600 483.0 51.0 10.2 7 450 677.0 30.0 7.3 8 350 866.0 30.0 5.7 9 200 1490.0 72.0 5.7 10 0.0 0.0 0.0 11 0.0 0.0 0.0 12 0.0 0.0 0.0 13 0.0 0.0 0.0 14 0.0 0.0 0.0 15 0.0 0.0 0.0 Planetary temperatures and errors: Mars Jupiter Saturn Uranus Neptune 2000 0.0 0.0 173.3 1.5 140.0 5.0 110.3 1.7 105.7 2.0 1300 0.0 0.0 170.0 5.0 133.0 5.0 96.4 1.7 91.7 2.0 1100 0.0 0.0 170.0 5.0 126.0 5.0 92.7 1.7 88.0 2.0 850 0.0 0.0 163.8 4.0 124.3 5.0 85.9 1.7 81.3 2.0 750 0.0 0.0 160.3 4.0 123.4 5.0 81.8 1.7 77.3 2.0 600 0.0 0.0 140.0 10.0 110.0 10.0 79.0 1.7 74.6 2.0 450 0.0 0.0 148.5 5.0 111.0 5.0 69.9 1.7 66.2 2.0 350 0.0 0.0 143.2 1.9 105.0 5.0 64.0 1.7 60.9 2.0 200 0.0 0.0 130.0 0.0 103.0 0.0 60.0 0.0 58.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 Notes (these are revised numbers as of 7 Aug 1992): The planetary brightness temperatures used are obtained from the measurements of Griffin et al. (1986, Icarus 65, 244), Orton et al. (1986, Icarus 67, 289), and Griffin & Orton (1993, Icarus, 105, 537). The errors in brightness tempera- tures are the rms internal errors of the observations. For MJD's between 46040 through 50000 the Martian temperatures are derived from the model developed by Wright (1976, Ap.J., 210, 250). Outside these MJD's (i.e., in particular after 10 October 1995) a simplified model of a rotating cratered asteroid is used (Wright, 1995; private communication to H.E. Matthews). Since the results for Mars are derived from models no errors are quoted; however the Martian bright- ness temperatures are probably uncertain at the 5% level and this uncertainty must be added to obtain the absolute errors. Over the interval for which both the original Wright model and the simplified model are valid, the differences in brightness temperatures have an rms error of 0.13 K (i.e. negligible). The flux densities for Saturn are for the planetary disk only; an additional flux is expected when the rings present an open aspect, and at such times Saturn should not be used as a calibration object. Individuals using these data in published works should reference the appropriate papers as noted above. The filter frequencies are the effective frequencies for 1mm of water vapour. These are the SCUBA filters (effective from 23-May-1996). Version 27-October-1995 (HEM) SCUBA Version 25-July-1996 (WSH) 23-July-2003 (TJ) - Add THUMPER 18-March-2005 (TJ) - Add THUMPER properly