Star            Name                Spectral    Apparent    Absolute    Distance

alpha CMa A     Sirius              A1 V*       -1.46       1.4            8.6
alpha Car       Canopus             F0 II       -0.72      -3.1           74 
alpha Cen       Rigil Kentaurus     G2 V+K1 V   -0.01       4.4            4.3
alpha Boo       Arcturus            K2 IIIb     -0.04      -0.3           34
alpha Lyr       Vega                A0 V         0.03       0.5           25.3
alpha Aur       Capella             G8           0.08      -0.6           41
beta  Ori       Rigel               B8 I*        0.12      -7.1          815
alpha CMi       Procyon             F5 IV        0.38       2.7           11.4
alpha Eri       Archenar            B3 Vpe       0.46      -2.3           69
alpha Ori       Betelgeuse          M2 I         0.50      -5.6          650
beta  Cen       Hadar               B1 III       0.61      -5.2          320
alpha Aql       Altair              A7 V         0.77                     16.8
213468                              A0 V         0.77
alpha Tau       Aldebaran           K5 III       0.85      -0.7           60
alpha Vir       Spica               B1 III+B2 V  0.98      -3.3          220 
alpha Sco       Antares             M1.5 I*      0.96      -5.1          425
beta Gem        Pollux              K0 III       1.14       1.0           40
alpha PsA       Fomalhaut           A3 Va        1.16       2.0           22
alpha Cyg       Deneb               A2 Iae       1.25      -7.1         1630 

1. The sources for this table are SEDS (Students Explore the Universe) and Se-605. The only numbers from Se-605 are the absolute magnitudes: they are somewhat out of date, but no matter here.

2. There is such a thing as luminosity class indicated by a Roman numeral after spectral type. Main sequence stars are luminosity class V. Only main sequence stars For other special symbols accompanying spectral type consult SEDS.

3. You can see that stars are bright because they have either high luminosity (i.e., low absolute magnitude) or because they are close. Star density in space decreases with increasing luminosity, and so, in fact, stars both very luminous and close are rare. Depending on how you count these things, Canopus may be the only such star. One can see that apparent brightness is NOT a good guide to relative distance.