Object |
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Adopted
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(AU) | (AU) | (AU) | (AU) | |
AA Tau |
![]() |
![]() |
... | 200-400 |
CI Tau | ... | ![]() |
... | 150-250 |
CW Tau | ... | ... | ... | 100-300 |
CX Tau | ... | ... | ... | 100-300 |
CY Tau | ![]() |
... | 230 | 230-330 |
DE Tau | ... | ... | ... | 100-300 |
DL Tau |
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... | 150-250 |
DM Tau | ![]() |
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160 | 160-260 |
DN Tau |
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125 | 125-225 |
DO Tau | ![]() |
... | ... | 100-200 |
DR Tau |
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90 | 90-190 |
DS Tau | ... | ... | ... | 100-300 |
FM Tau | ... | ... | ... | 100-300 |
FZ Tau | ... | ... | ... | 100-300 |
GM Aur |
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270 | 270-370 |
GO Tau | ... |
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160 | 160-260 |
HO Tau | ... | ... | ... | 100-300 |
IQ Tau |
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... | ... | 250-400 |
RY Tau | ![]() |
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115 | 115-215 |
SU Aur | ... | ... | ... | 100-300 |
UZ Tau E | ... | ... | 160 | 160-260 |
Notes. (a)
listed here results from image fitting using a truncated power-law for the surface density profile. K02: Kitamura et al. (2002); AW07: Andrews & Williams (2007). (b)
is the radius within which the 95% of the flux is observed, after
fitting the visibility of the source with a Gaussian; we used this
value, when available, as a lower limit for our adopted
-interval. I09: Isella et al. (2009).
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