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


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 [FORMULA] as observed and [FORMULA] 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 [FORMULA].

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

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

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