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Astron. Astrophys. 342, 313-336 (1999)

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8. Conclusion

The PRETI method for faint source detection with ISOCAM has been successfully applied to the observation of the HDF and flanking fields. Faint fluxes are reached with a good reliability. Moreover, our simulations allow us to test the completeness and photometric accuracy of our results. On the ISO-HDF, the method gives a 99.9% completeness at 200 µJy in LW3 when detecting above five times the noise level in wavelet space. The same completeness is obtained at 65 µJy in LW2. Using PRETI, we detected 49 sources in our main source list, plus 51 in a less secure supplementary list. Most of the sources are detected at 15 µm, 11 are detected at 6.7 µm only. Our results for the brightest sources are in good agreement with those of Désert et al. (1998) in both filters, as well as with those of Rowan-Robinson et al. (1997) at 15 µm, but not at 6.75µm. The number counts derived for the LW3 filter show a clear excess of sources with respect to the predictions of a no evolution model (Franceschini et al. 1997). A forthcoming paper (Elbaz et al. in prep) will refine these results with a source by source study and discuss extinction and star formation rates.

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© European Southern Observatory (ESO) 1999

Online publication: February 22, 1999
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