CCD PHOTOMETRY, PERIOD ANALYSIS, AND LIGHT CURVE DECONVOLUTION OF THE SHORT PERIOD PULSATING VARIABLE STAR TYC 3603-1124-1

"CCD derived B- and V-magnitudes were determined for Tyc_3603-1124-1, a short period pulsating variable classified as a High Amplitude δ Scuti (HADS) star. Some of these data were acquired during September and October of 2021, and the remainder was recorded in September 2023. Period phased plots of the data showed a slow rise to maximum light but a more rapid drop to minimum brightness. This is somewhat unusual for a HADS star. B-V color indices from 2021 and 2023 were slightly different indicating a possible temperature drop during that period. Additional time-of-maximum data obtained from the SuperWASP extra-solar planet detection program and from the Transiting Exoplanet Survey Satellite (TESS) were combined with Stonecrest Observatory data (SO) in order to perform a predicted time difference (PTD) analysis and obtain an updated linear ephemeris. Fourier analysis of the SuperWASP data yielded only four frequencies with signal-to-noise ratios over SNR=6, but the combined TESS data produced six significantly different frequencies. Regardless of the data source, the first frequencies, F1 ≈ 7.35 and F2 ≈ 14.7 cycles per day, were essentially the same, as was the next frequency, F3 < 0.03 per day. These lower frequencies provided some insight into the noisy appearance of the B and V photometric magnitudes. Stellar parameters for Tyc 3603-1124-1 were not inconsistent with those expected for a HADS variable. Stellar tracks from PARSEC models gave some insight into the evolutionary status of the star.