Target | Integrated flux densitya F | rms noise, ![]() |
![]() |
![]() |
Dust massc,
![]() |
![]() |
(mJy) | (mJy/beam) | (K) | (
![]() |
(10-4) | ||
![]() |
63.6 ![]() |
2.4 | 89 | 0.67 | 4.8 ![]() |
17 |
![]() |
70.6 ![]() |
... | ... | ... | ... | |
![]() |
15.8 ![]() |
... | ... | ... | ... | |
HD 181327 | 51.7 ![]() |
5.0 | 70 | 0.15 | 34 ![]() |
27 |
HD 172555 | 30 ![]() |
5.2 | 320+(10-20) | 0.1+0.1 | 10-60 (SE) | 10e |
40 ![]() |
20-70 (NW) | |||||
HD 15115 | ... | 5.1 | 62 | 0.73f | <2.9 | 5.8f |
HD 164249 | ... | 4.0 | 70 | ... | <2.2 | 5.9g |
HD 181296 | ... | 4.8 | 150 | ... | <1.3 | 2.4g |
HD 191089 | ... | 6.0 | 95 | ... | <3.2 | 19h |
a The integrated flux density was calculated by fitting a Gaussian peak for HD 181327, Pic, and feature II in the
Pic map, while a circle of radius
was used when including feature I. For HD 172555 the flux was measured within the boxes in Fig. 1c,
as described in the text. Estimated errors come from rms noise
calculation in the specific integration region, together with an
absolute calibration error of 10% (Siringo et al. 2009).
b For detected sources we use the dust temperature
derived from the best fit of the spectral energy distribution. For
HD 15115 the best-fit temperature from Williams & Andrews (2006) is employed, while temperatures from IR excess measured with IRAS (Rhee et al. 2007) is used for the other objects.
c Upper
limit on the dust mass for undetected sources.
d South-east and north-west feature of HD 172555 calculated separately.
e For a 15 K disk.
f From detection at 850 m by Williams & Andrews (2006) who found
F850=4.9
1.6 mJy and derived a dust mass of 3.8
.
g From Rebull et al. (2008).
h From Moór et al. (2006).
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