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Table 2:

Integrated flux density, root-mean-square noise levels, and derived dust temperature, power law exponent of the opacity law, mass, and fractional dust luminosity for the 870-$\mu $m observations of main-sequence members of the BPMG.

Target
Integrated flux densitya F rms noise, $\sigma $ $T_{{\rm dust}}$b $\beta $ Dust massc, $M_{\rm dust}$ $f_{\rm dust}$
  (mJy) (mJy/beam) (K)   ( $M_{{\rm Moon}}$) (10-4)
$\beta $ Pic 63.6 $\pm$ 6.7 2.4 89 0.67 4.8 $\pm$ 0.5 17
$\beta $ Pic (incl. I) 70.6 $\pm$ 8.2   ... ... ... ...
$\beta $ Pic (only II) 15.8 $\pm$ 2.4   ... ... ... ...
HD 181327 51.7 $\pm$ 6.2 5.0 70 0.15 34 $\pm$ 4 27
HD 172555 30 $\pm$ 10 (SE)d 5.2 320+(10-20) 0.1+0.1 10-60 (SE) 10e
  40 $\pm$ 10 (NW)       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, $\beta $ Pic, and feature II in the $\beta $ Pic map, while a circle of radius  $47\hbox{$^{\prime\prime}$ }$ 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 $3\sigma $ 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 $\mu $m by Williams & Andrews (2006) who found F850=4.9 $\pm$ 1.6 mJy and derived a dust mass of 3.8  $M_{{\rm Moon}}$.
g From Rebull et al. (2008).
h From Moór et al. (2006).


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