Table 2:

Integrated flux density, root-mean-square noise levels, and derived dust temperature, power-law exponent of the opacity law, mass, fractional dust luminosity, and characteristic radial dust distances for the 22 stars observed at 870-m.

Object ID	Integrated flux sensity, F	RMS noise,	a		Dust massb,
	(mJy)	(mJy/beam)	(K)		( )	(10-4)	(AU)
DETECTIONS (>)
HD 21997	17.6  8.0	4.6	52	0.7	33  15	4.9	240
HD 95086	41.3  18.4	10.4	150+(15-45)c	...	>76d	6.4-14	16+(250-1500)
HD 98800	33.6  8.4	3.9	155e	0.1	8.5	470	2.4
HD 109573	21.5  6.6	3.1	88f	0.7	19.5  6.0	38	77
HD 131835	8.5  4.4	3.0	89	0.1	21  11	25	47
HD 141569	12.6  4.6	2.3	80g	0.8	27  10	73	110
HD 152404	42.9  9.8	3.7	...h	...	...	...	...
HD 161868	12.8  5.2	2.5	73	0.5	2.6  1.1	0.90	120
HD 170773	18.0  5.4	2.6	43	0.7	9.7  2.9	4.5	170
HD 207129	5.1  2.7	2.1	38	0.7	0.6  0.3	0.94	130
MARGINAL DETECTIONS (>)
HD 105	10.7  5.9	3.7	40	0.6	7.7  4.2	2.6	110
HD 30447	6.9  5.0	4.5	61	0.3	12.3  8.9	9.3	56
HD 195627	13.0  7.1	4.1	57	0.3	3.1  1.7	1.0	74
NON-DETECTIONS
HD 17390	...	6.8	55i	...	<13.4	1.9j	...
HD 25457	...	3.3	70k	...	<0.9	1.0k	...
HD 31392	...	4.7	49k	...	<3.4	1.6k	...
HD 32297	...	6.5	30l	...	<150	33j	...
HD 61005	...	6.0	58k	...	<6.6	25k	...
HD 78702	...	4.2	36m	2.0m	<39	2.6m	...
HD 139664	...	3.5	78n	...	<0.7	1.2n	...
HD 164249	...	3.5	78	...	<5.3	5.9o	...
HD 193307p	...	3.8	...	...	...	...	...

Notes. ^(a) For detected and marginally detected sources we use the dust temperature derived from the best fit to the spectral energy distribution. ^(b) Upper limit on the dust mass for undetected sources. ^(c) In order not to be resolved the second dust belt should be at <1500 AU, which would mean >15 K, while a temperature >45 K would not be compatible with far-IR data. ^(d) Calculated for upper limit on dust temperature. ^(e) Ambiguous fit (see discussion in Sect. 5.2). ^(f) Source appears spatially resolved (see discussion in Appendix A). See also more detailed modelling by Augereau et al. (1999b) and SCUBA measurement by Sheret et al. (2004). ^(g) Source appears spatially resolved (see discussion in Appendix A). See also modelling by Sheret et al. (2004). ^(h) No simple debris disk model can be fitted (see Section 5.2). ⁽ⁱ⁾ From Rhee et al. (2007). ^(j) From Moór et al. (2006). ^(k) From Hillenbrand et al. (2008). ^(l) From Maness et al. (2008). ^(m) From Williams & Andrews (2006). ⁽ⁿ⁾ From Beichman et al. (2006a). ^(o) From Rebull et al. (2008). ^(p) Not enough photometry data for reliable SED fit.