Table 3.
Candidates for which we have detected an IR excess.
| Object | SpT (Ref.) | d | G | AG | Teff, GDR2 | Teff, S11 | AV,SED | Teff, SED | Teff,SED 96% CL | log g | χ2 | SW4 | S24 | Binary | New |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (pc) | (mag) | (mag) | (K) | (K) | (mag) | (K) | (K) | ||||||||
| HD 161261 | B9 (1) | 356 ± 17 | 8.26 | 0.62 | 9132 | 8842 | 0.6 | 12 000 | 11 250–13 000 | 4.5 | 10.0 | 32.8 | ? | Y | |
| HD 161733 | B7(2)–B8 (1) | 322 ± 13 | 7.96 | 0.43 | 9124 | 8740 | 0.65 | 15 000 | 14 000–16 914 | 5.0 | 5.2 | 2.3 | 12.6 | ? | N |
| HD 161621 | A0 (1) | 314 ± 11 | 9.45 | 0.61 | 7886 | 0.4 | 8250 | 7250–11 000 | 4.0 | 9.0 | Y | Y( * ) | |||
| TYC 428-1938-1 | A (3) | 338 ± 15 | 11.01 | 0.77 | 6197 | 7840 | 0.7 | 7500 | 6031–8 463 | 4.5 | 0.9 | 47.4 | N | N | |
| TYC 428-980-1 | A2 (3) | 340 ± 11 | 10.36 | 7310 | 0.35 | 7750 | 6750–10 250 | 4.0 | 0.6 | 25.0 | 417.1 | N | Y | ||
| 2MASS J17462472+0517213 | G2–G3 (4) | 336 ± 10 | 12.67 | 0.78 | 5155 | 5459 | 0.65 | 5750 | 5000–6500 | 5.0 | 3.8 | 20.8 | N | N | |
| HD 161734 | B8 (5)–A0 (1) | 447 ± 20 | 8.82 | 0.75 | 8478 | 8420 | 0.9 | 13 000 | 10 705–14 000 | 4.5 | 5.9 | 150.0 | 320.3 | ? | N |
Notes. Columns indicate: (1) Object ID; (2) spectral type; (3) Bayesian distance; (4–5) Gaia DR2 G-band magnitude and extinction; (6–7) photometric effective temperature from Gaia DR2 and Smith et al. (2011); (8–12) extinction, effective temperature and the 96% confidence level, log g, and reduced χ2 parameter of the best fit SED; (13–14) significance of the W4 and 24 μm excess defined as 
; (15) binary flag (from literature); (16) new candidate to host a debris disc.
( * )We note that eventually we reject the source HD 161621 as a candidate (see text).
References. (1) Cannon & Pickering (1993); (2) Kraicheva et al. (1980); (3) Giampapa et al. (1998); (4) Allain et al. (1996); (5) Gray & Corbally (2002).
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