Table 1
Name, equatorial coordinates α and δ (J2000), effective temperature Teff, surface gravity log g and metallicity [Fe/H] of our Galactic sample stars.
| N° | Name | α (J2000) | δ (J2000) | T eff | log g | [Fe/H] | P orbit | E(B − V)tot | LIR/L∗ | d | Prog. ID |
| (h m s) | (° ) |
(K) | (cgs) | (days) | (%) | (kpc) | |||||
|
|
|||||||||||
| 1 | EP Lyr | 19 18 17.5 | + 27 50 38 | 7000 | 2.0 | –1.5 | 0.52 ± 0.01 | 3 ± 0 | 4.1 ± 0.8 | 3274 | |
| 2 | HD 131356 | 14 57 00.7 | −68 50 23 | 6000 | 1.0 | –0.5 | 1490 | 0.20 ± 0.01 | 50 ± 2 | 3.0 ± 0.6 | 3274 |
| 3 | HD 213985 | 22 35 27.5 | −17 15 27 | 8250 | 1.5 | –1.0 | 259 | 0.27 ± 0.01 | 24 ± 1 | 3.1 ± 0.6 | 3274 |
| 4 | HD 52961 | 07 03 39.6 | + 10 46 13 | 6000 | 0.5 | –4.8 | 1310 | 0.06 ± 0.01 | 12 ± 1 | 2.1 ± 0.4 | 3274 |
| 5 | IRAS 05208−2035 | 05 22 59.4 | −20 32 53 | 4000 | 0.5 | 0.0 | 236 | 0.00 ± 0.00 | 38 ± 2 | 3.9 ± 0.8 | 3274 |
| 6 | IRAS 06034 + 1354 | 06 06 12.3 | + 13 53 09 | 6000 | 1.5 | –2.0 | 0.97 ± 0.02 | 48 ± 3 | 3.4 ± 0.7 | 50092 | |
| 7 | IRAS 06072 + 0953 | 06 09 57.4 | + 09 52 35 | 5500 | 1.0 | –2.0 | 0.20 ± 0.01 | 54 ± 3 | 5.9 ± 1.2 | 50092 | |
| 8 | IRAS 06338 + 5333 | 06 37 52.4 | + 53 31 02 | 6250 | 1.0 | –1.5 | 0.16 ± 0.02 | 3 ± 0 | 3.9 ± 0.8 | 50092 | |
| 9 | IRAS 09060−2807 | 09 08 10.1 | −28 19 10 | 6500 | 1.5 | –0.5 | 371 | 0.57 ± 0.02 | 63 ± 3 | 5.4 ± 1.1 | 3274 |
| 10 | IRAS 09144−4933 | 09 16 09.1 | −49 46 06 | 5750 | 0.5 | –0.5 | 1770 | 1.99 ± 0.05 | 53 ± 5 | 2.7 ± 0.6 | 3274 |
| 11 | IRAS 09538−7622 | 09 53 58.5 | −76 36 53 | 5500 | 1.0 | –0.5 | 0.35 ± 0.02 | 64 ± 5 | 7.8 ± 1.6 | 50092 | |
| 12 | IRAS 10174−5704 | 10 19 18.1 | −57 19 36 | G8IaO | 323 | 3274 | |||||
| 13 | IRAS 11000−6153 | 11 02 04.3 | −62 09 43 | 7600 | 2.0 | 0.1 | 0.63 ± 0.01 | 42 ± 2 | 1.9 ± 0.4 | 50092 | |
| 14 | IRAS 13258−8103* | 13 31 07.1 | −81 18 30 | F4Ib-G0Ib | 50092 | ||||||
| 15 | IRAS 15556−5444 | 15 59 32.1 | −54 53 18 | F8 | 50092 | ||||||
| 16 | IRAS 16230−3410 | 16 26 20.3 | −34 17 12 | 6250 | 1.0 | –0.5 | 0.56 ± 0.02 | 60 ± 3 | 6.1 ± 1.2 | 3274 | |
| 17 | IRAS 17038−4815 | 17 07 36.3 | −48 19 08 | 4750 | 0.5 | –1.5 | 1381 | 0.22 ± 0.02 | 69 ± 5 | 4.5 ± 1.0 | 3274 |
| 18 | IRAS 17233−4330* | 17 26 57.7 | −43 33 13 | 6250 | 1.5 | –1.0 | 0.53 ± 0.02 | 548 ± 32 | 9.2 ± 2.0 | 50092 | |
| 19 | IRAS 17243−4348 | 17 27 56.1 | −43 50 48 | 6250 | 0.5 | 0.0 | 484 | 0.59 ± 0.02 | 68 ± 4 | 3.8 ± 0.8 | 3274 |
| 20 | IRAS 17530−3348 | 17 56 18.5 | −33 48 47 | 5000 | 0.0 | 0.0 | 0.38 ± 0.02 | 57 ± 4 | 2.6 ± 0.5 | 50092 | |
| 21 | IRAS 18123 + 0511 | 18 14 49.4 | + 05 12 55 | 5000 | 0.5 | 0.0 | 0.24 ± 0.02 | 89 ± 6 | 4.9 ± 1.0 | 50092 | |
| 22 | IRAS 18158−3445 | 18 19 13.6 | −34 44 32 | 6500 | 1.5 | 0.0 | 0.78 ± 0.03 | 13 ± 9 | 10 ± 2.3 | 50092 | |
| 23 | IRAS 19125 + 0343 | 19 15 00.8 | + 03 48 41 | 7750 | 1.0 | –0.5 | 517 | 1.08 ± 0.02 | 52 ± 3 | 1.8 ± 0.4 | 3274 |
| 24 | IRAS 19157−0247 | 19 18 22.5 | −02 42 09 | 7750 | 1.0 | 0.0 | 120.5 | 0.68 ± 0.01 | 63 ± 2 | 4.2 ± 0.9 | 3274 |
| 25 | IRAS 20056 + 1834* | 20 07 54.8 | + 18 42 57 | 5850 | 0.7 | –0.4 | 0.51 ± 0.02 | 905 ± 42 | 10.9 ± 2.3 | 3274 | |
| 26 | RU Cen | 12 09 23.7 | −45 25 35 | 6000 | 1.5 | –2.0 | 1489 | 0.55 ± 0.01 | 13 ± 1 | 2.3 ± 0.5 | 3274 |
| 27 | SAO 173329 | 07 16 08.3 | −23 27 02 | 7000 | 1.5 | –0.8 | 115.9 | 0.39 ± 0.01 | 36 ± 1 | 6.5 ± 1.3 | 3274 |
| 28 | ST Pup | 06 48 56.4 | −37 16 33 | 5750 | 0.5 | –1.5 | 410 | 0.00 ± 0.00 | 55 ± 1 | 5.7 ± 1.2 | 3274 |
| 29 | SU Gem* | 06 14 00.8 | + 27 42 12 | 5750 | 1.125 | –0.7 | 0.58 ± 0.02 | 111 ± 7 | 4.8 ± 1.0 | 3274 | |
| 30 | SX Cen | 12 21 12.6 | −49 12 41 | 6000 | 1.0 | –1.0 | 600 | 0.32 ± 0.02 | 34 ± 2 | 3.8 ± 0.7 | 3274 |
| 31 | TW Cam | 04 20 48.1 | + 57 26 26 | 4800 | 0.0 | –0.5 | 0.40 ± 0.02 | 42 ± 3 | 3.2 ± 0.6 | 3274 | |
| 32 | UY Ara* | 17 29 28.9 | −59 54 02 | 5500 | 0.5 | –1.0 | 0.00 ± 0.00 | 72 ± 3 | 12 ± 2.5 | 50092 | |
| 33 | UY CMa* | 06 18 16.4 | −17 02 35 | 5500 | 1.0 | 0.0 | 0.00 ± 0.00 | 89 ± 3 | 9.6 ± 2.0 | 3274 | |
Notes. For the model parameters we refer to De Ruyter et al. (2006). Also given is the orbital period (see references in De Ruyter et al. 2006; Gielen et al. 2007; Van Winckel et al. 2009). The total reddening E(B − V)tot, the energy ratio LIR/L∗ and the calculated distance, assuming a luminosity of L∗ = 5000 ± 2000 L⊙. Stars marked with * are seen in reflection only, resulting in unreliable E(B − V)tot values and luminosity ratios, and upper limits for the distances. The last column lists whether the spectra are part of the SAGE-Spec catalogue, Spitzer programme 3274 or 50092.
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