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Table 1

Astrophysical parameters of the programme stars.

ID Name Sp. type Group log Teff log Lbol M d i PA
log [K] log [L] [M] [pc] [°] [°]

1 HD 100546 B9Vne I 4.02 1.62 2.4 ±0.1o 103y 42 ±5d 145 ±5d
2 HD 97048 A0pshe I 4.00 1.42 2.5 ±0.2o 180y 42.8a 175 ±1
3 HD 179218 B9e I 4.02 1.88 2.7 ±0.2i 240y 57 ±2u 23 ±3u
4 HD 101412 B9.5V II 4.02 1.40 2.3 ±0.2i 160g 80 ±7u 38 ±5u
5 HD 141569 B9.5e 3.98 1.10 2.00s 99y 51 ±3t 356 ±5t
6 HD 190073 A2IVpe II 3.95 1.92 2.85l 290y 23m 10m
7 HD 98922 B9Ve II 4.02 2.95 2.2 ±0.8x 540‡ y 45x
8 HD 95881 A2III/IV II 3.95 1.34n 2.0 ±0.3n 170 ±30n 55n 103n
9 R CrA A5IIev II 3.86 3.5r 130b 65q 180q
10 HD 135344B F8V 3.82 1.01 1.7 ±0.2i 140 ±2f 14 ±3e 56 ±2e
11 HD 150193 A1Ve II 3.95 1.19 2.3 ±0.2o 150y 38 ±9v 358 ±6v
12 HD 104237 A4Ve+sho II 3.92 1.53 1.96k 116y 18k
13 HD 142666 A8Ve II 3.88 1.03 1.8 ±0.3o 145 ±2f almost edge-onh

Notes. The references for the values for the effective temperature of the central star log Teff, the observed bolometric luminosity log Lbol, and the distance d can be found in Acke et al. (2005) and references therein, unless indicated otherwise.

(⋆)

Inclination in degrees from face-on.

(♣)

Derived from the PAH 8.6 μm image of Lagage et al. (2006).

(†)

We do not classify this source in group I/II (Sect. 2).

(‡)

Ambiguity about the distance exists (Blondel & Tjin A Djie 2006).

Reference.

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