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Astron. Astrophys. 332, 25-32 (1998)

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5. IRAS fluxes

In order to obtain the best possible IRAS 12 and 25 µm fluxes we inspected two-dimensional images and one-dimensional co-adds of IRAS scans using the GIPSY software package (Assendorp et al. 1995). The results are listed in Table 1. The error is the 1 [FORMULA] error estimate based on the fluctuation in the background flux. The fluxes from the FSC and as determined using GIPSY are compared in Fig. 3. For the brighter objects the results are essentially identical. At the fainter flux levels the scatter is somewhat larger. The most important change is in the [FORMULA] ratio. For most stars the colours as derived from GIPSY are bluer than indicated by the FSC fluxes, by on average 8%.

[FIGURE] Fig. 3. Comparison between 12, 25 and ratio of 12 to 25 µm flux-densities from the FSC and as determined using the GIPSY package. The lines indicate the one-to-one relations.
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© European Southern Observatory (ESO) 1998

Online publication: March 10, 1998
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