Astron. Astrophys. 348, 768-782 (1999)

Footnotes

1. Based on observations collected at the European Southern Observatory, La Silla, Chile, using the IRAC2B camera with the ESO-MPG 2.2m telescope.

2. In the following we refer to as observed and as dereddened flux density.

3. ISO is an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands and the United Kingdom) with the participation of ISAS and NASA.

4. We use the relation between flux density and K band magnitude .

5. The central , according to Genzel et al. (1997), encloses a total mass of , of which are associated with a central Black Hole, leaving a total mass of of stars.

6. We estimate a detection limit of Jy and a completeness limit of our source counts for Jy.

7. Note for the following discussion of the KLF that Jy), with defined by Eq. (4) if both flux densities refer to the same area and Jy is the detection limit.

8. For the sake of simplicity we use here this IMF although being aware that it overestimates the number of stars at both the high- and low-mass end (Scalo, 1986)

9. M ap O n-Off P ointing S kydip I mage

© European Southern Observatory (ESO) 1999

Online publication: August 13, 199
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