The Luminosity Function, φ(Mv) [10-3 stars pc-3 per unit absolute magnitude interval]
Derived from a list of the 100 nearest stars in Allen's Astrophysical Quantities.  Completeness is assumed for r < 6.45 pc.
Absorption has been ignored.  Spectroscopic binaries have been counted as single stars.
Mv φ(Mv)   Mv φ(Mv)   Mv φ(Mv)
< 1.0 < 0.9   7.0 3.6   13.5 9.8
1.0 0.9   7.5 3.1   14.0 4.0
1.5 0.9   8.0 2.7   14.5 5.3
2.0 0.9   8.5 5.3   15.0 7.5
2.5 1.8   9.0 7.1   15.5 7.1
3.0 0.9   9.5 4.4   16.0 4.0
3.5 0.9   10.0 8.0   16.5 1.3
4.0 1.8   10.5 12.4   17.0 0.9
4.5 3.6   11.0 11.6   17.5 0.9
5.0 3.6   11.5 11.6   18.0 0.9
5.5 5.3   12.0 8.9   18.5 0.9
6.0 7.1   12.5 10.2   19.0 0.9
6.5 4.0   13.0 13.8   > 19.0 < 0.9

        Notable Conclusions from the above Table   
    (1) φ(Mv) peaks between Mv = 10 and Mv = 13.
    (2) Stars brighter than Mv » +4 are too rare to be adequately represented in the sample, i.e., little can be concluded about φ(Mv) for Mv < 4.
    (3) Stars fainter than the sun (Mv » +4.8) outnumber those brighter than the sun by a ratio of about 13:1.
    (4) The median absolute visual magnitude is about 11.0 to 11.5.
    (5) It is not clear whether the apparent scarcity of stars fainter than Mv » +16 is real or due to the difficulty in discovering such stars (sample
          incompleteness).
    (6) ò-¥ φ(Mv) dMv » + 0.09 stars pc-3.