Using mainly bulge red clump giants (RCG) and giants as tracers, 
a picture has emerged of the Galactic bulge consisting of a rotating 
peanut-shaped structure made up largely of old and metal-rich stars 
(~10 Gyr, [Fe/H] falling between -0.5 and +0.5 dex).  However, there 
is a more metal-poor population of stars present in the bulge, 
a scarcer, lesser explored population of stars.  I will present 
results from our spectroscopic survey of bulge RR Lyrae variables, 
tracers of possibly the oldest and most metal-poor stars in the bulge 
([Fe/H] peaking at -1.0 dex).  To date, we have obtained spectra of 
~1000 OGLE bulge RR Lyrae stars in four 2 degree windows for which 
NIR-photometry from the VVV surveys exists. Therefore, our RR Lyrae 
stars have accurate (3%) distances based on near infrared light curves.  
Our results indicate that the RR Lyrae stars exhibit hot kinematics and 
null or negligible rotation and are therefore members of a separate 
population from the bar/pseudobulge that currently dominates the mass 
and luminosity of the inner Galaxy.  Our RR Lyrae stars predate these 
structures, and have metallicities, kinematics, and spatial distribution 
that are consistent with a "classical" bulge, although we cannot yet 
completely rule out the possibility that they are the metal-poor tail 
of a more metal rich ([Fe/H] ~ -1 dex) halo-bulge population.