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Table 5

Continuum fluxes obtained at 2.6 and 1.3 mm from the interferometric data.

Source Continuum fluxes IRAS fluxes
at 2.6 mm (mJy) at 1.3 mm (mJy) f12 (Jy) f25 (Jy) f60 (Jy) f100 (Jy)

WX Psc 4.8 ± 1.6  ± 6 1155 968 215 72
IK Tau 9 ± 1 28 ± 2 4634 2377 332 103
TX Cam 10.1 ± 0.6 24.5 ± 0.9 1640 635 134 39
RX Boo 7 ± 1 20 ± 3 846 419 69 26
X Her 2.8 ± 0.4 13.5 ± 0.6 484 241 39 18
CRL 2362  ± 0.3  ± 0.6 112 137 31 8
χ Cyg 15.8 ± 0.7 65 ± 3 1690 459 81 18
V Cyg 7.2 ± 0.5 17.0 ± 0.9 665 234 49 17
S Cep 4.6 ± 0.7* 11.3 ± 1.4* 383 133 29 13
OH 104.9+2.4  ± 0.6  ± 1.4 123 229 91 35
R Cas 13.0 ± 0.7 45 ± 2 1340 555 103 39
IRAS 19475+3119  ± 0.4  ± 0.6 0.5 38 56 15
IRAS 20028+3910 5.0 ± 0.5* 24 ± 2* 42 211 143 47
IRAS 21282+5050 2.9 ± 0.6 5.4 ± 1.2 51 74 33 15
IRAS 23321+6545  ± 0.4 4.0 ± 0.7 14 86 64 19
CRL 2477 1.3 ± 0.4 4.4 ± 0.6 75 109 47 14

Notes. The continuum fluxes (shown in Cols. 2 and 3) were obtained, after line emission subtraction, by fitting the data in the uv − plane with a point-like source model, but for χ Cyg, for which an elliptical Gaussian source (0″̣9  ×  0″̣7 size) model was fitted. (*) Means that the continuum obtained at 2.6 mm is found to be displaced with respect to that at 1.3 mm. In Cols. 4−7 IRAS fluxes (from SIMBAD) are shown for comparison. We think however that a large part of the CSE continuum emission is filtered out in the data, by comparison with the results obtained by Groenewegen et al. (1997).

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