  Rotational transitions in vibrationally excited AlO and TiO -- two possible
precursors of dust -- were observed in the 300 GHz range (1 mm wavelength)
towards the oxygen rich AGB stars R Dor and IK Tau with ALMA, and vibrationally
excited AlO was observed towards the red supergiant VY CMa with the SMA. The
$J=11 \to 10$ transition of TiO in the $v=1~{\rm{and}}~2$ levels, and the $N =
9 \to 8$ transition in the $v=2$ level of AlO were identified towards R Dor;
the $J=11 \to 10$ line of TiO was identified in the $v=1$ level towards IK Tau;
and two transitions in the $v=1~{\rm{and}}~2$ levels of AlO were identified
towards VY CMa. The newly-derived high vibrational temperature of TiO and AlO
in R Dor of $1800 \pm 200$ K, and prior measurements of the angular extent
confirm that the majority of the emission is from a region within
$\lesssim2R_{\star}$ of the central star. A full radiative transfer analysis of
AlO in R Dor yielded a fractional abundance of $\sim$3% of the solar abundance
of Al. From a similar analysis of TiO a fractional abundance of $\sim78$% of
the solar abundance of Ti was found. The observations provide indirect evidence
that TiO is present in a rotating disk close to the star. Further observations
in the ground and excited vibrational levels are needed to determine whether
AlO, TiO, and TiO$_2$ are seeds of the Al$_2$O$_3$ dust in R Dor, and perhaps
in the gravitationally bound dust shells in other AGB stars with low mass loss
rates.
