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The flux calibration of the LWS instrument is based on observations of Uranus, a point source in the LWS aperture. The telescope is diffraction limited at about 110 µm, beyond which a fraction of the flux of an on-axis point source may be diffracted out of the standard aperture. Significant diffraction loss does not occur in sources that appear extended in the LWS beam. Therefore, an extended source correction must be applied to put these fluxes on a point source calibration scale. In order to apply this correction, the LWS beam of each detector and the telescope PSF must be well known. The extended source correction also assumes that the source is infinitely extended and uniformly bright. None of these galaxies are either, so applying the correction requires great caution. From tests done by the LWS instrument team, the extended source correction works well for sources larger than 3'-4' (Gry et al. 2003) when compared to IRAS at 100 µm.

The fluxes quoted in Tables 2, 4, and 5 are those which have been measured according to the point source flux calibration. The current understanding of the LWS beam is still not complete, and the extended source correction may change in the future as more work is done. Therefore, the extended source correction has not been applied to the line fluxes listed in this paper, but those galaxies that may require an extended source correction have been noted in Tables 2, 4, and 5. The most up-to-date effective apertures and corrections are listed in Table 7, taken from the ISO LWS Handbook Volume III (Gry et al. 2003).

Table 7. Extended Source Aperture Corrections

Detector Aperture Radius Correction

SW1 39 0.88
SW2 42 0.88
SW3 43 0.84
SW4 41 0.73
SW5 40 0.70
LW1 38 0.69
LW2 39 0.69
LW3 35 0.62
LW4 34 0.55
LW5 33 0.48

The fluxes listed in Tables 3 and 4 for extended sources are based on a point source calibration. The multiplicative correction listed here may need to be applied to these fluxes.

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