Is this project an undergraduate, graduate, or faculty project?
Undergraduate
individual
What campus are you from?
Daytona Beach
Authors' Class Standing
Senior
Lead Presenter's Name
Divyeshwari P. Vansadia
Faculty Mentor Name
Dr. Stephen Gillam
Abstract
We present our analysis of the rotational period and principal frequency of the rapidly oscillating Ap star KIC 7582608 using TESS data. To separate the flux of the target star from that of contaminating neighbors, our processing pipeline carries out multiple point spread function fitting on the TESS Full Frame Images (FFIs). TGLC package was used to extract the decontaminated light curves of the star measured in TESS sectors 14, 26, 40, 41, 53, and 74, we estimated the star's pulsation frequencies and its rotation period. Higher temporal resolution data, such as the Target Pixel Files (TPFs) with a cadence of less than 200 seconds, is evidently essential to detect the star’s principal frequency. Pywhiten's Lomb-Scargle frequency analysis was used to calculate the principal frequency and rotation period, which were then compared to the findings utilizing Period 04 and ground-based data. A main frequency of 2.10335 ± 2.33E-08 mHz was found for the 200 sec Sector 74 data. Meanwhile, based on sectors 26 (1800 sec) and 40 (600 sec), rotation periods between 18.99417805 ± 3.47 days and 20.52826489 ± 4.05 days were determined for our star. Our findings suggest that the FFI data is sensitive to the star's rotation period; however, to determine the principal frequency of the star, we need high cadence data (such as sector 74).
Keywords: TESS data, principal frequency detection, rotational period, Lomb-Scargle frequency analysis, point spread function, Period 04, TGLC, PyWhiten, Full Frame Images.
Did this research project receive funding support from the Office of Undergraduate Research.
No
Analysis of TESS Data for Pulsating Star - KIC7582608
We present our analysis of the rotational period and principal frequency of the rapidly oscillating Ap star KIC 7582608 using TESS data. To separate the flux of the target star from that of contaminating neighbors, our processing pipeline carries out multiple point spread function fitting on the TESS Full Frame Images (FFIs). TGLC package was used to extract the decontaminated light curves of the star measured in TESS sectors 14, 26, 40, 41, 53, and 74, we estimated the star's pulsation frequencies and its rotation period. Higher temporal resolution data, such as the Target Pixel Files (TPFs) with a cadence of less than 200 seconds, is evidently essential to detect the star’s principal frequency. Pywhiten's Lomb-Scargle frequency analysis was used to calculate the principal frequency and rotation period, which were then compared to the findings utilizing Period 04 and ground-based data. A main frequency of 2.10335 ± 2.33E-08 mHz was found for the 200 sec Sector 74 data. Meanwhile, based on sectors 26 (1800 sec) and 40 (600 sec), rotation periods between 18.99417805 ± 3.47 days and 20.52826489 ± 4.05 days were determined for our star. Our findings suggest that the FFI data is sensitive to the star's rotation period; however, to determine the principal frequency of the star, we need high cadence data (such as sector 74).
Keywords: TESS data, principal frequency detection, rotational period, Lomb-Scargle frequency analysis, point spread function, Period 04, TGLC, PyWhiten, Full Frame Images.