Table 4
Result of the interferometric model fitting.
| Index | IRAS |
Θ
|
F
tot
|
ρ
sub
|
|
F
tot
|
τ
eff
|
hlr
|
Bayes factor B10 | Resolved? |
| (mas) | (Jy) | (mas) | (Jy) | (mas) | ||||||
|
|
||||||||||
| 1 | 04440+2605 | 13.9 |
11.8 |
2.3 |
1.11 |
12 |
0.27 |
4.3 |
1014 | y |
| 2 | 07008+1050 | 37 |
3.9 |
2.2 |
0.69 |
3.7 |
0.02 |
10 |
~16 | y |
| 3 | 07284-0940 (max) | 50.0 |
125 |
7.0 |
0.87 |
157 |
0.196 |
18.4 |
10233 | y |
| 07284-0940 (min) | 41.2 |
75 |
7.0 |
0.97 |
90 |
0.15 |
15.6 |
1099 | y | |
| 4 | 08011-3627 | 63 |
121 |
1.7 |
0.507 |
121 |
0.25 |
25 |
1052 | y |
| 5 | 08544-4431 | 46 |
153 |
6.2 |
0.90 |
171 |
0.32 |
14.8 |
10271 | y |
| 6 | 09256-6324 | 38 |
102 |
3.8 |
0.86 |
103 |
0.42 |
10.3 |
108 | y |
| 7 | 10158-2844 | 42 |
23.4 |
6.6 |
1.09 |
23.9 |
0.062 |
12.5 |
1020 | y |
| 8 | 10174-5704 | 140 |
53 |
3.0 |
0.457 |
54 |
0.018 |
75 |
10160 | y |
| 9 | 10456-5712 | 58 |
163 |
7.4 |
0.92 |
170 |
0.23 |
18 |
1019 | y |
| 10 | 11385-5517 | 27.9 |
80 |
4.0 |
1.00 |
81 |
0.45 |
8.5 |
10101 | y |
| 11 | 12185-4856 | <27 | 5.3 |
1.4 |
>0.75 | 5.2 |
>0.1 | <5.2 | ~0.1 | n |
| 12 | 12222-4652 | 28 |
31.9 |
1.9 |
0.72 |
33 |
0.29 |
7.7 |
1033 | y |
| 13 | 15469-5311 | 36 |
40 |
2.9 |
0.77 |
40 |
0.20 |
10 |
1011 | y |
| 14 | 17038-4815 (max) | 19.8 |
14.5 |
1.2 |
0.68 |
14.6 |
0.25 |
5.8 |
1018 | y |
| 17038-4815 (min) | 17 |
9.1 |
1.2 |
0.72 |
9.1 |
0.20 |
5.0 |
105 | y | |
| 15 | 17243-4348 | 14.7 |
10.3 |
0.9 |
0.70 |
10.5 |
0.35 |
4.0 |
1010 | y |
| 16 | 17534+2603 | 22.2 |
79 |
5.4 |
1.9 |
79 |
0.90 |
7.0 |
1051 | y |
| 17534+2603 (alt)a | 3.9 |
1.12 |
83 |
0.65 |
7.2 |
|||||
| 17 | 18281+2149 | 65.7 |
42 |
3.3 |
0.537 |
41 |
0.030 |
38 |
10101 | y |
| 18 | 19125+0343 | 20.0 |
25 |
1.6 |
0.74 |
25 |
0.33 |
6.1 |
1042 | y |
| 19 | 22327-1731 | <20 | 5.3 |
1.3 |
>0.67 | 4.9 |
>0.08 | <6.5 | ~1 | n |
Notes. The mid-IR variable sources identified in Sect. 3.3 have two entries, one for a minimum and a maximum pulsation phase. For unresolved sources we give 3σ upper or lower limits on the determined size parameters, otherwise the uncertainties are at the 1σ level. We define τeff as the scale factor (τeff = (1−exp−τ). For small τ, the effective scale factor reduces to τ.
The results of the fit when assuming the stellar parameters of Hillen et al. (2013), i.e., Teff = 6250 K and θ⋆ = 0.45 mas.
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