Speaker
Description
V1223 Sagittarii is an intermediate polar (IP), a subclass of magnetic cataclysmic variables containing an accreting white dwarf(WD) with a magnetic fields ranging between(0.5-8) MG. Optical and x-ray observations have established an orbital period of approximately 3.366 hr and a WD spin period of approximately 12.4 min. Additionally, a 13.2 min beat period, arising from the interaction between the spin and orbital frequencies, has been detected and is often the more dominant optical period. V1223 Sagittarii have been investigated as a source for non thermal emission and high-energy particle acceleration, with theoretical evidence for high-energy emission.Recent exploratory searches for $\gamma$-ray emission from highly magnetised white dwarfs using approximately 15 years of Fermi-LAT data, resulted in indications of probable transient pulsed emissions. V1223 Sagittarii were among the sources looked at and showed signs of transient emission but no dedicated periodicity search were done for this source. In this study we conducted a follow up analysis using a longer base line of about 18 years of Fermi-LAT data in conjunction with 3(120s resolution), and 1(20s resolution) observations sections of TESS data. Analysis techniques used with Fermi-data includes unbinned light curves and TS-Gating. Periodicity search were done using Rayleigh and H-test algorithm using previously published ephemeris. Timing analysis of TESS data were done using the \textit{lightkurve} module in python utilizing the Lomb-Scargle Periodogram.Prelimanary results shows pulsed emission from V1223 Sagittarii in the Fermi data and also confirmed in TESS data, ongoing analysis will be to better constrain the ephemeris used for Periodity search using a extended dataset which includes BOOTES6 and 7 data.