(2)=AWM96; (3)=Bourke, Hyland & Robinson 1995; (4)=Benson & Myers 1989; (5)=Caselli, Myers, Thaddeus 1995; (6)=Hilton & Lahulla 1995; (7)=Keene 1981; (8)=Loren 1989; (9)=Loren et al. 1990; (10)=Leung, Kutner & Mead 1982; (11)=Parker 1988; (12)=Sandqvist & Lindroos 1976, Sandqvist 1977; (13)=Schneider & Elmegreen 1979; (14)=Tafalla et al. 1998; (15)=Ward-Thompson et al. 1994; (16)=Williams et al. 1999\
$^{\dagger}$Oph D was also mapped in the LW3, LW6 and LW9 filters (see text and Fig. \[absorption\]cd). The zodiacal intensity is 45 MJy/sr in LW3.\
$^{\ddagger}$Values of I$_{zodi}$ come from the zodiacal light model of Kelsall et al. (1998). Typical uncertainty is $\sim$ 20%.\
$^{*}$Cores belonging to Taurus molecular complex.\
$^{**}$Cores belonging to $\rho$ Ophiuchi molecular complex.\

\[sources\]

The properties of the observed cloud cores are summarized in Table \[sources\]. Column 1 lists the names of the sources as found in the dark cloud catalogues, columns 2 and 3 list the J2000 coordinates of the centre of the ISOCAM field. The image centres are sometimes shifted from their original positions as given in the dark cloud catalogues (see above). Column 4 gives the distances to the clouds. For the clouds not belonging to the $\rho$ Ophiuchi (adopted distance d = 160 pc[^4]) and Taurus (d 