Object name |
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(AU) | (AU) | (
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(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
SR 4 | ... | 100-300 | 2.5 | 0.7 |
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GSS 26 | ... | 100-300 | 1.9 | 0.0 |
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... | ... |
EL 20 | ... | 100-300 | 2.5 | 0.8 |
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DoAr 25 | 200 | 100-300 | 2.3 | 0.5 |
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... |
EL 24 | 175 | 75-275 | 2.2 | 0.4 |
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... |
EL 27 | 275 | 175-375 | 2.2 | 0.5 |
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SR 21 | 600 | 500-700 | 2.9 | 1.1 |
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IRS 41 | ... | 100-300 | 2.1 | 0.3 |
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YLW 16c | ... | 100-300 | 2.4 | 0.0 |
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IRS 49 | ... | 100-300 | 1.8 | 0.0 |
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... | ... |
DoAr 33 | ... | 100-300 | 2.2 | 0.4 |
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WSB 52 | ... | 100-300 | 1.8 | 0.0 |
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WSB 60 | 350 | 250-450 | 1.9 | 0.3 |
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DoAr 44 | ... | 100-300 | 2.2 | 0.4 |
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RNO 90 | ... | 100-300 | 2.3 | 0.4 |
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Wa Oph 6 | 275 | 175-375 | 2.4 | 0.7 |
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AS 209 | 200 | 100-300 | 2.4 | 0.7 |
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Notes. (1) Underlined objects are those which have not been
mapped to date through high-angular resolution imaging. The objects
which have been mapped but do not have an estimate for the outer disk
radius as reported in Col. (2) have been spatially resolve by
Andrews et al. (2009). Contrary to Andrews & Williams (2007a),
they modeled the disk surface brightness by using a self-similar
profile instead of a truncated power-law. For this reason no estimate
for
could be extracted for these sources (see footnote in Sect. 4.1).
(2) Best-fit estimate of the disk outer radius by fitting the
observed visibilities at sub-millimeter wavelengths using a truncated
power-law for the surface density profile. AW07: Andrews &
Williams (2007a).
(3) Interval of the disk outer radius adopted for our analysis.
(4) Best-fit estimate of the spectral index of the SED
between 1 and 3 mm derived by considering for the outer disk
radius the central value of the interval reported in Col. 3, and
for the power-law index of the surface density profile p=1. (5) Best-fit estimate of the spectral index of the dust opacity
between 1 and 3 mm. (6) Product between the dust mass and the
dust opacity at 1 mm from the best-fit two-layer disk model.
(7) Dust mass obtained with a power-law index for the grain size
distribution q=2.5. (8) Like Col. (7) but with q=3. The sources without an estimate of the dust mass have a
-value (reported in Col. (6)) which cannot be reproduced with q=3. (9) Like Col. (8) but with q=3.5.
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