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Blue large-amplitude pulsators (BLAPs) make up a rare class of hot pulsatingstars with effective temperatures of $\approx$30,000 K and surface gravities of4.0 - 5.0 dex (cgs). The evolutionary origin and current status of BLAPs is notwell understood, largely based on a lack of spectroscopic observations and noavailable mass constraints. However, several theoretical models have beenproposed that reproduce their observed properties, including studies thatidentify them as pulsating helium-core pre-white dwarfs (He-core pre-WDs). Wepresent here follow-up high-speed photometry and phase-resolved spectroscopy ofone of the original 14 BLAPs, OGLE-BLAP-009, discovered during the OpticalGravitational Lensing Experiment. We aim to explore its pulsationcharacteristics and determine stellar properties such as mass and radius inorder to test the consistency of these results with He-core pre-WD models.Using the mean atmospheric parameters found using spectroscopy, we fit aspectral energy distribution to obtain a preliminary estimate of the radius,luminosity and mass by making use of the Gaia parallax. We then compare theconsistency of these results to He-core pre-WD models generated using MESA,with predicted pulsation periods implemented using GYRE. We find that our massconstraints are in agreement with a low-mass He-core pre-WD of $\approx$0.30M$_{\odot}$.

OGLE-BLAP-009 -- A Case Study for the Properties and Evolution of Blue Large-Amplitude Pulsators