**Table 4:** Basic results of SMA observations at 1.4 mm. For comparison, the SEST 1.3 mm single-dish fluxes from Nürnberger et al. (1997) are shown.
Source name	Continuum flux^a		rms^b	Gaussian size	RA^a	Dec^a	Effective frequency	SEST 1.3 mm^c
	(mJy)		(mJy/beam)	(arcsec)	(J2000)	(J2000)	(GHz)	Flux	rms
	(P)	(G)						(mJy)	(mJy)
HT Lup	73	77	4.0	$1.01 \pm 0.66$	15 45 12.9	-34 17 30.1	221.3	135	15
GW Lup	64	70	3.7	$1.22 \pm 0.48$	15 46 44.8	-34 30 35.7	221.3	106	18
IM Lup	188	214	4.3	$1.33 \pm 0.20$	15 56 09.2	-37 56 06.5	221.3	260	9
RU Lup	148	158	4.5	$1.02 \pm 0.32$	15 56 42.3	-37 49 15.9	221.3	197	7
HK Lup	89	101	3.9	$1.43 \pm 0.38$	16 08 22.5	-39 04 47.5	221.3	84	17

NOTE. Source name in boldface indicates that the source is resolved at 1.4 mm with the SMA, see Sect. 3.2. ^a Continuum flux and position are taken from fits in the (u, v) plane. Both the point-source flux (P) and the integrated flux for a Gaussian (G) are shown. ^b Calculated from the cleaned image. ^c Nürnberger et al. (1997). The SEST fluxes are in general higher than the SMA fluxes, partly due to the slightly shorter effective wavelength, 1.3 mm (SEST) vs. 1.4 mm (SMA).

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