Carbon- and Oxygen-rich Asymptotic Giant Branch (AGB) stars in the Bulge
  Asymmetries and Dynamical Evolution (BAaDE) survey
  Detections of SiO masers from the Bulge Asymmetries and Dynamical Evolution
(BAaDE) survey more tightly define the region where Oxygen-rich (O) Asymptotic
Giant Branch (AGB) stars reside in multiple infrared (IR) color-color diagrams.
Using MSX and 2MASS data along with radio spectra from the BAaDE survey we find
that three main populations were observed in the BAaDE survey: O-rich AGB stars
of which about $73\%$ host SiO masers, Carbon-rich (C) AGB stars which do not
host these masers, and a small contaminating set of possible Young Stellar
Objects (YSOs). The distinction between YSOs and AGB stars can be drawn using
only MSX data, specifically the $[D]-[E]$ color, while the shorter wavelengths
provided by 2MASS are necessary to divide potential C- and O-rich AGB stars.
Divisions similar to these have been seen in multiple earlier IR-studies, but
BAaDE currently provides a sample of $\sim$ 15000 sources which far exceeds
previous studies in sample size, and therefore provides much more distinct
divisions. With these IR distinctions in place, we discuss the sources which
are exceptions in either their molecular detections or IR colors, as well as
the distribution of the three populations in Galactic coordinates.
