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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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