a  Unless otherwise marked, the parallax for the primary (or for the combined system) is used for all components of the system.
b  Proxima Centauri is the third member of the {alpha} Centauri system. The error bar quoted here for the parallax is the updated one used in Jao et al. (2005AJ....129.1954J).
c  The spectral type is a joint type including all objects in the system.
d  These spectral types are estimates based on the MV values for the B and C components as measured by Delfosse et al. (1999A&A...350L..39D) and translated into spectral type using Table 3 of Kirkpatrick & McCarthy (1994AJ....107..333K).
e  This object is sometimes referred to as van Maanen 2, although in the original discovery paper (van Maanen 1917PASP...29..258V) it is neither named nor numbered.
f  We estimate a distance by averaging the 7.1pc estimate of Reid et al. (2007, Cat. J/AJ/133/2825) and the 6pc estimate of Riaz et al. (2006, Cat. J/AJ/132/866).
g  According to Luyten (1979, Cat. I/98), Innes discovered this object. However, Innes did not number his discoveries, so the discovery name is noted here simply as "Innes (unnumbered)."
h  This is a composite type for G 208-44 AB (GJ 1245 AC).
i  McCarthy et al. (1988ApJ...333..943M) give delta(V)~2.0mag for the G 208-44 AB pair, so we estimate the spectral type of G 208-44 B to be approximately one subclass later than G 208-44 A (assumed to have a type identical to the composite spectral type of M5.5 V).
j  We estimate a distance by averaging the 6.9pc estimate of Scholz et al. (2005, Cat. J/A+A/442/211) and the 6.2pc estimate of Reid et al. (2002, Cat. J/AJ/123/2822).
k  We estimate a distance by averaging the 7.3pc estimate of Scholz et al. (2005, Cat. J/A+A/442/211) and the 6.7pc estimate of Reid et al. (2002, Cat. J/AJ/123/2822).
l  We estimate a distance by averaging the 7.2pc estimate of Reid et al. (2004, Cat. J/AJ/128/463) and the 8.7pc estimate of Scholz et al. (2005, Cat. J/A+A/442/211).
m  This spectral type is a composite type for the Lalande 27173 BC pair.
n  This spectral type is estimated from the absolute J, H, K values measured by Forveille et al. (1999A&A...351..619F) and the absolute magnitudes vs. spectral type relation given in Table 3 of Kirkpatrick & McCarthy (1994AJ....107..333K).
o  The parallax for 36 Oph A is assumed for 36 Oph C; an independent Hipparcos parallax for 36 Oph C is 167.49+/-0.60mas (van Leeuwen 2007, Cat. I/311).
p  2MASS J18450079-1409036 and 2MASS J18450097-1409053 appear to be a common proper motion pair based on Digitized Sky Survey R-band images taken in 1951 and again in 1988 (see http://irsa.ipac.caltech.edu/applications/FinderChart/).
q  Hawley et al. (1997AJ....113.1458H) say this is an M3 III but Luyten (1979, Cat. I/98) lists this pair as a common proper motion binary so the giant luminosity classification must be an error.
r  Reid et al. (2004, Cat. J/AJ/128/463) state that they believe this parallax measurement may be in error because the result suggests a location on the H-R diagram significantly below the main sequence despite the fact that this M dwarf's spectrum shows no evidence of the low metallicity expected for such a location.
s  Identification taken from van de Kamp (1930PA.....38...17V).
t  This spectral type is the composite type for Wolf 630 ABaBb. 
u  The spectral type is estimated from the measured mass of this component (Segransan et al. 2000, Cat. J/A+A/364/665) and a mapping of mass into spectral type using other objects in this table and their masses as measured in Henry & McCarthy (1993, Cat. J/AJ/106/773).
v  Costa et al. (2005AJ....130..337C) measure an independent parallax of 155.43+/-1.33mas for van Biesbroeck 8.
w  van Leeuwen (2007, Cat. I/311) measures a parallax value of 148.92+/-4.00mas; an independent Yale parallax gives 169.84+/-6.6mas (van Altena et al. 1995, Cat. I/238).
x  This spectral type is based on delta J, H, K values measured by Henry & McCarthy (1993, Cat. J/AJ/106/773) and using the absolute magnitude vs. spectral types tabulate in Table 3 of Kirkpatrick & McCarthy (1994AJ....107..333K).
y  Given that the mass ratio is ~1 (Delfosse et al. 1999A&A...350L..39D), we assume equal spectral types for both components.
z  SCR J1546-5534 has J-Ks=1.10mag from 2MASS; WISE photometry is corrupted by a brighter source immediately to the northwest (the Galactic latitude of this source is -0.8deg) so we can only say that J-W2<3.65 and H-W2<2.99. The overall photometry from both 2MASS and WISE is consistent with a late-M dwarf.
aa Given that Delfosse et al. (1999A&A...350L..39D) find nearly equal masses for components A and B and that component C is ~0.5mag fainter than the joint AB pair in adaptive optics imaging, we assume all components are roughly the same spectral type.
bb Identification taken from Hertzsprung (1922BAN.....1...21H); Kapteyn's Star is also referred to as Cordoba 5h243 (van Maanen 1943ASPL....4..199V).
cc The object LP 771-95 shares common proper motion with LP 771-96 AB. The parallax measured for LP 771-95 is assumed for LP 771-96 AB.
dd This is the composite spectral type for LP 771-96 AB.
ee This spectral type is estimated from the delta V, R, I values measured in Henry et al. (2006AJ....132.2360H), the measured composite type for LP 771-96 AB, and spectral type vs. absolute magnitude relations given in Table 3 of Kirkpatrick & McCarthy (1994AJ....107..333K).
ff Rodgers & Eggen (1974PASP...86..742R) note peculiarities in the blue spectrum of this object.
gg These two objects share common proper motion.
hh Kuiper (1943ApJ....97..275K) types this object one spectral subclass later than L 369-44; as Kuiper was probably typing on the Mt. Wilson system, we assign this object a type one subclass later than the type assigned for L 369-44 by Riaz et al. (2006, Cat. J/AJ/132/866).
ii BD+61 2068 is noted as a spectroscopic binary by Herbst & Layden (1987AJ.....94..150H) (see also Heintz 1981ApJS...46..247H). No other info is given, so an M spectral type is assumed for the secondary. 
jj The spectral type is an estimate based on measured broadband colors.
kk The object LP 229-17 lies near on the sky and in distance to Vega.
ll Montagnier et al. (2006A&A...460L..19M) show that this is a near equal-magnitude binary, so we estimate a spectral type identical to the joint spectrum.
mm GJ 2005 D, a fourth component reported elsewhere, may not exist according to Seifahrt et al. (2008A&A...484..429S).
nn This object is believed to be a white dwarf.
oo This spectral type is an estimate based on the measured absolute V magnitude.
pp Fomalhaut has common proper motion with LTT 9283 (Gl 879).
qq The object LTT 9283 has common proper motion with Fomalhaut but may lie slightly closer to the Sun than Fomalhaut itself.
rr Marsh et al. (2013ApJ...762..119M) report a parallax of 0.087"+/-0.054" for this object, whereas Kirkpatrick et al. (2011, Cat. J/ApJS/197/19) report 0.351"+/-0.108". Given the discrepancies in this measurements, we instead use our spectrophotometric distance estimate from Table 8.