Astron. Astrophys. 361, 555-580 (2000)

Footnotes

1. although recent studies suggest d  120-140 pc - see Knude & Hog (1998) and de Zeeuw et al. (1999).

2. Since the intensity in Column 7 includes the contribution of the zodiacal light emission, the contrast in Column 9 is not truly representative of the actual core absorption strength.

3. `CIA' is a joint development by the ESA Astrophysics Division and the ISOCAM Consortium. The ISOCAM Consortium is led by the ISOCAM PI, C. Cesarsky.

4. At the observed mid-IR wavelengths, the scattering component of should be more than ten times smaller than the absorption component for a dust composition following Preibisch et al. (1993) and can thus be neglected (e.g. Bohren & Huffman 1983).

5. For Oph D, the Eastern profile does not stretch far enough to enable an analysis at large radii ( 200"). For L328, the Eastern profile is disturbed by the presence of additional absorption features. For L310, L1709A, L1544 and GF5, the profile we kept was the longest one not affected by the presence of supplementary absorption features (or by flatfield noise as in L1544).

6. The results of this comparison would remain unchanged if we used T=12.5 K, the dust temperature adopted for our pre-stellar cores - see Sect. 3.3.1.

7. According to CM95 (see also McKee 1989), UV ionization exceeds cosmic ray ionization for A_v 4, which means that the UV field can influence cloud support up to A_v 4, while it excites UIB carriers only up to A_v  1 (see Sect. 3.3).

8. When evaluated for the CM95 and Ciolek & Basu (2000) models, the cutoff wavelength below which Alfvén waves cannot propagate in the neutrals (e.g. Eqs. [1a] and [2a] of Mouschovias 1991) is  0.08-0.14 pc, i.e., comparable to in Table 3. This suggests that hydromagnetic turbulence may indeed play a role near or beyond but quickly decays on smaller scales.

9. Since protostellar outflows are believed to be directly powered by accretion (e.g. Königl & Pudritz 2000), the outflow momentum rate may be used as a surrogate tracer of the accretion rate.

© European Southern Observatory (ESO) 2000

Online publication: October 2, 2000
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