  Low mass ratio systems (LMR) are a very interesting class of contact
eclipsing binaries challenging the theoretical models of stability. These
systems are also considered possible progenitors of the rare low-mass optical
transients called red novae. In this study, we present the identification of 7
new totally eclipsing LMR systems from Catalina Sky Surveys (CSS) and 77 LMR
candidates from the All Sky Automated Survey (ASAS$-$3). Using the available
CSS light curves and new multiband observations for CSS$\_$J210228.3$-$031048
and CSS$\_$J231513.$+$345335 with the 2.3 m Aristarchos telescope at Helmos
Observatory, we estimate their physical and absolute parameters and investigate
their stability and their progenitors. The light curves are analyzed by
performing a 2$-$dimension scan on the mass ratio $-$ inclination plane with
Phoebe$-$0.31 scripter while the errors are estimated using Monte-Carlo
simulations and heuristic scanning of the parameter space. Our analysis
revealed that all 9 CSS systems have extreme mass ratios from 0.09 to 0.16. Our
statistical analysis of well$-$studied LMR contact binaries shows that LMR
systems tend to have warmer and more massive primaries. The investigation of
the progenitors of both low and higher-mass ratio systems reveals a trend for
the former to originate from higher-mass ancestors. Finally, we investigate the
stability condition by calculating the ratio of spin angular momentum to
orbital angular momentum and other stability indicators in the context of the
reliability of the solutions.
