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Astron. Astrophys. 319, 360-360 (1997)

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IRAS sources beyond the solar circle

VI. Analysis of the FIR, H2 O, and CO emission

J.G.A. Wouterloot 1, K. Fiegle 1, J. Brand 2 and G. Winnewisser 1

1 I. Physikalisches Institut, Zülpicher Strasse 77, D-50937 Köln, Germany
2 Istituto di Radioastronomia, CNR, Via Gobetti 101, I-40129 Bologna, Italy

Astron. Astrophys. 301, 236-260 (1995)

The last sentence of Sect. 3.3 on page 245 should read: Wouterloot & Walmsley (1986) distinguished between 'group 1' and 'group 2' sources; the latter (former) have


In the upper part of Table 4, the columns 2 and 4, and the columns 3 and 5 were erroneously interchanged. The correct Table 4 is included below.

In Sect. 4 (page 255), the scaling for the case that each source contains a star cluster with an IMF of Miller & Scalo (1979) was wrong. In our new calculations the clusters have a most massive star with mass M in the interval [FORMULA] - [FORMULA] with M = ([FORMULA] + [FORMULA])/2.0. For the scaling we assumed that the clusters also contain one star in the interval [FORMULA] - 60  [FORMULA], which is however not included in the cluster luminosities. The results following this approach are given in the new version of Table 5c, and Fig. 25c. Our conclusions are not affected in the sense that if the sources contain star clusters with M [FORMULA] 10 [FORMULA] the derived slopes of the IMF are steeper than in the case of single stars.


Table 1. Average CO parameters as a function of [FORMULA]


Table 2. Mass distribution of IRAS sources, assuming that the luminosity of each IRAS source is due to a star cluster.

[FIGURE] Fig. 25c. The IMF for these sources assuming that each FIR source contains a cluster with a Miller & Scalo (1979) mass distribution
© European Southern Observatory (ESO) 1997

Online publication: July 3, 1998