Large grains in discs around young stars: ATCA observations of WW Chamaeleontis, RU Lupi, and CS Chamaeleontis

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Volume 495 / No 3 (March I 2009)

A&A, 495 3 (2009) 869-879

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Table 6:

Overview of the results for CS Cha.
Obs. date	Wavelength	Flux^a	rms^a	Beam size^b
	(mm)	(mJy)	(mJy/beam)	(arcsec)
26 April 2008	7.0	$1.00\pm0.28$	0.129	$2.4 \times 1.4$
26 April 2008	7.3	$0.92\pm0.25$	0.114	$2.4 \times 1.5$
5 July 2008	6.7	<0.82	0.273	$10.8 \times 0.6$
5 July 2008	7.0	<0.71	0.238	$11.3 \times 0.6$
6 July 2008	6.7	<1.11	0.371	$4.3 \times 0.6$
6 July 2008	7.0	$1.38\pm0.26$	0.218	$4.5 \times 0.6$

^a Continuum fluxes are from point-source fits in the (u, v) plane, where 3 $\sigma$ upper limits are quoted in the case of non-detections. rms calculated from the cleaned image. CS Cha is located at 11:02:25.1, -77:33:35.95 (J2000); ^b restored beam, using natural weighting. Note that the exact beam size depends on frequency and location of the source in the sky, as well as on the time of the observations, over which time range the data were taken, and exactly which data/baselines were included.

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