WASP-52b: Insights into the exoplanet’s parameters from combining new photometric ground observations and TESS observation with SOPHIE, COR, and HARPS data for multifilter photometric and spectroscopic radial velocity

This paper is done in three steps, (A) exoplanet photometric Observation, (B) photometric, radial velocity, and transmission transit analysis by the RAW data with different software and open-source platforms, and (C) combines new photometric data (our observations and TESS data) with radial velocities data to bring insights into this planet, to compare our transit observations results with previously published and reanalyzed results. All these results test the ability of exoplanet observations using a small telescope aperture hosted in Sharjah Astronomical Observatory (SAO- M47) with a 431 mm diameter.

For that, we made eight new light curves for the WASP-52b exoplanet. The observations were obtained from the Sharjah Astronomical Observatory (M47, 0.431 m) during 2019 and 2023 using different filters R, V, and L. Using multiple software, we estimated the planet transit’s physical and orbital parameters from individual and folded light curves analysis and apply transit results with radial velocity observation by EXOFAST tool for generate the full parameters of the exoplanet depend on filters. First, we analyzed light curve transits in two ways, individually with different photometrical software and codes like Muniwin and Hops Master, for folded light curves we applied the TransitFit code. By photometric results, we have determined the radius of the planet (R), semi-major axis (a), inclination (i), and period of transit time (P) for comparison with previous studies. For folded our observations, where we folded three observations by the L filter, three observations by the R filter, and two observations by the V filter. Also, for comparing exoplanet orbit parameters we relied upon different radial velocity observations collected from multi-source and public data archives we reexamined, merged, and utilized (RV) observation data by collecting open-source observations from many observatories archives like the Haute-Provence Observatory spectrograph (SOPHIE) new release data starting from 2010 to 2022, HARPS from HARPS RVBank archive and CORALIE (COR) spectrograph installed at The Swiss 1.2-metre Leonhard Euler Telescope at La Silla. Using the platform DACE we recalculate and reanalyze the Mass (M${}_j$), Period (P), and semi-major axis(a) of the exoplanet after combining the data and compare them with our photometric results generated by both software ( HOPS and TransitFit) results. Moreover, we reanalyzed the transmission transit observation data for the WASP-52b exoplanet taken in 2017 to comprehend the difference in transit depth between multifilter observation results. For that, we employed the PLanetary Atmospheric Transmission for Observer Noobs (PLATON) code to estimate the planet’s size with multi-filter observations for characterizing the atmospheric features that would affect the planetary transit depth and plot all previous transmission data listed in the NASA Exoplanet Archive/ Atmospheric Spectroscopy platform. In late November 2024, the TESS archive released data for 14 new transits of WASP-52b. These transits were utilized to re-evaluate the exoplanet parameters by comparing them to previously published results and the authors’ prior findings. The analysis included investigating the transit-timing variation (TTV) of WASP-52b to explore the possibility of the planet being influenced by an unseen companion. Furthermore, these tests were conducted to assess the capability of a small-aperture 431 mm telescope to produce reliable and accurate measurements for an exoplanet with similar properties. By using folded P results in this study, We try to determine the orbit model by following a linear or quadratic model. We use the equations of both models to calculate the fit period for the new Epochs we observed for all 2023 transits. The results from both equations were compared, showing a closer match with the linear model and confirming the stability of the planet’s rotational period. Our analysis found that Rp/R* = 0.15415, 0.16366, and 0.164985 for the L, V, and R filters respectively. To better understand the difference between the results of the L filter and to identify the reason for the variance in the depth of the crossing between the filters, it became apparent that the amount of light passing through the range of the L filter is greater than what is indicated by the decrease in the size of the planet in wide band photometric observations. This is illustrated by comparing the filters in the Figure 4. Finally, the period results from photometric and spectroscopic are shown as follows P of filter L= 1.7497788, P of filter V= 1.7497807, P of filter R= 1.7497782 respectively, in the same order a/R*= 7.363, 7.408, 7.521 respectively. All analyses of the data from SAO and TESS were performed under the assumption of free eccentricity to determine whether any ellipticity is present in the planet’s orbit.