  The surface content of lithium (Li) and beryllium (Be) provide insights into
the mixing and circulation mechanisms in stellar interiors. The old open
cluster, M 67, has been well-studied for Li abundances in both main-sequence
and evolved stars. The Be abundances give us a probe to a deeper level in
stars. We have taken high-resolution spectra with Keck I with HIRES to
determine Be abundances along the subgiant branch of M 67, where there are
dramatic depletions of Li. These subgiants range in mass from 1.26 to 1.32
M$_{\odot}$ and have evolved from main-sequence stars that would have occupied
the region of the Li-Be dip found in younger clusters. Lithium abundances have
been adjusted to the same scale for 103 stars in M 67 by Pace et al. The more
massive stars $-$ now the coolest and furthest-evolved from the main-sequence
$-$ show a drop in Li by a factor of 400 across the subgiant branch. Our new Be
abundances also show a decline, but by a factor of $\sim$50. The two elements
decline together with Li showing a steeper decline in these subgiants than it
does in the Li-Be dip stars. The relative decline in Be abundance compared to
Li is remarkably well fit by the models of Sills & Deliyannis, made
specifically for the subgiants in M 67. Those models include the effects of
mixing induced by stellar rotation. These M 67 subgiants show the effects of
both main-sequence depletion and post-main-sequence dilution of both Li and Be.
