  I present the results of a search for new low-mass stars and brown dwarfs in
the Eta Cha and Eps Cha young associations. Within radii of 1.5 and 0.5 deg
surrounding Eta Cha and Eps Cha, respectively, I have constructed
color-magnitude diagrams from DENIS and 2MASS photometry and have obtained
spectra of the candidate low-mass members therein. The five candidates in Eta
Cha are classified as four field M dwarfs and one carbon star. No new members
are found in this survey, which is complete for M_sun=0.015-0.15 according to
the evolutionary models of Chabrier and Baraffe. Thus, an extended population
of low-mass members is not present in Eta Cha out to four times the radius of
the known membership. Meanwhile, the three candidate members of Eps Cha are
classified as young stars, and thus likely members of the association, based on
Li absorption and gravity-sensitive absorption lines. These new sources have
spectral types of M2.25, M3.75, and M5.75, corresponding to masses of 0.45,
0.25, and 0.09 M_sun by the models of Chabrier and Baraffe. For one of these
stars, intense H(alpha) emission, forbidden line emission, and strong K-band
excess emission suggest the presence of accretion, an outflow, and a disk,
respectively. This young star is also much fainter than expected for an
association member at its spectral type, which could indicate that it is seen
in scattered light. No brown dwarfs are detected in Eps Cha down to the
completeness limit of 0.015 M_sun. The absence of brown dwarfs in these
associations is statistically consistent with the mass functions measured in
star-forming regions, which exhibit only ~2 and ~1 brown dwarfs for stellar
samples at the sizes of the Eta Cha and Eps Cha associations.
