Table 1.
Candidate stars examined in this work.
Star | Spec. | mK | mL | mM | mN2 | |
---|---|---|---|---|---|---|
Sirius | A1V (1) | −1.35 (2) | −1.38 | −1.34 | −1.31 | |
Altair | A7V (1) | 0.24 (2) | 0.21 | 0.24 | 0.27 | |
Procyon | F5IV-V (3) | −0.65 (2) | −0.68 | −0.65 | −0.63 | |
α Cen A | G2V (4) | −1.49 (2) | −1.52 | −1.47 | −1.48 | |
e Eri | G6V (6) | 2.53 (2) | 2.50 | 2.56 | 2.54 | |
del Pav | G8IV (5) | 2.04 (2) | 2.01 | 2.07 | 2.05 | |
τ Ceti | G8V (6) | 1.68 (2) | 1.65 | 1.71 | 1.69 | |
Omi02 Eri | K0V (6) | 2.41 (2) | 2.38 | 2.44 | 2.42 | |
70 Oph | K0V (6) | 1.79 (2) | 1.76 | 1.82 | 1.80 | |
α Cen B | K1V (4) | −0.60 (2) | −0.63 | −0.57 | −0.59 | |
36 Oph A | K2V (4) | 2.95 (4), ( * ) | 2.92 | 2.99 | 2.95 | |
36 Oph B | K2V (4) | 1.84 (7), ( * ) | 1.84 | 1.91 | 1.88 | |
ϵ Eri | K2V (6) | 1.67 (2) | 1.64 | 1.71 | 1.68 | |
HD 191408 | K2.5V (5) | 3.05 (8), ( * ) | 3.01 | 3.09 | 3.05 | |
70 Oph B | K4V (9) | 3.34 (7), ( * ) | 3.30 | 3.37 | 3.33 | |
HD 131977 | K4V (6) | 3.10 (2) | 3.06 | 3.13 | 3.09 | |
ϵ Indi | K5V (4) | 2.24 (10) | 2.20 | 2.27 | 2.22 | |
V2215 Oph | K5V (4) | 3.47 (10) | 3.42 | 3.50 | 3.45 | |
η Cas | F9V (11) | 1.99 (2) | 1.96 | 2.00 | 2.00 | |
σ Dra | K0V (6) | 2.83 (12) | 2.80 | 2.86 | 2.84 | |
HD 219134 | K3V (6) | 3.25 (2) | 3.22 | 3.29 | 3.25 | |
61 Cyg A | K5V (6) | 2.68 (12) | 2.64 | 2.71 | 2.67 |
Notes. The list of the 18 ELT candidates with spectral type, apparent K magnitude, and calculated magnitudes. L, M, and N2 magnitudes are calculated from the given K magnitude and spectral type following the work of Pecaut & Mamajek (2013). The top four new candidates for a theoretical northern hemisphere survey at a Hawaii or La Palma site are also given (see Sect. 2.3 for details) following the dividing line. σ Draconis is only visible from La Palma site. Both northern sites can also see Procyon and Altair but only the Hawaii site can see Sirius. ( * )Converted from a V band magnitude from the given source.
References. (1) Gray et al. (2003); (2) Ducati (2002); (3) Skiff (2013); (4) Torres et al. (2006); (5) Gray et al. (2006); (6) Keenan & McNeil (1989); (7) Fabricius et al. (2002); (8) Zacharias et al. (2012); (9) Cowley et al. (1967); (10) Cutri et al. (2003); (11) Abt (2008); (12) van Belle & von Braun (2009).
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