[논문]SEARCHING FOR TRANSIT TIMING VARIATIONS AND FITTING A NEW EPHEMERIS TO TRANSITS OF TRES-1 B

Yeung, Paige; Perian, Quinn; Robertson, Peyton; Fitzgerald, Michael; Fowler, Martin; Sienkiewicz, Frank; Tock, Kalee

doi:10.5303/jkas.2022.55.4.111

SEARCHING FOR TRANSIT TIMING VARIATIONS AND FITTING A NEW EPHEMERIS TO TRANSITS OF TRES-1 B 원문보기

Journal of the Korean astronomical society = 천문학회지, v.55 no.4, 2022년, pp.111 - 121

Yeung, Paige (Massachusetts Institute of Technology) , Perian, Quinn (Massachusetts Institute of Technology) , Robertson, Peyton (Stanford University) , Fitzgerald, Michael (Las Cumbres Observatory) , Fowler, Martin , Sienkiewicz, Frank (Harvard-Smithsonian Center for Astrophysics, Smithsonian Astrophysical Observatory) , Tock, Kalee (Stanford Online High School)

Abstract ▼ AI-Helper

Based on the light an exoplanet blocks from its host star as it passes in front of it during a transit, the mid-transit time can be determined. Periodic variations in mid-transit times can indicate another planet's gravitational influence. We investigate 83 transits of TrES-1 b as observed from 6-inch telescopes in the MicroObservatory robotic telescope network. The EXOTIC data reduction pipeline is used to process these transits, fit transit models to light curves, and calculate transit midpoints. This paper details the methodology for analyzing transit timing variations (TTVs) and using transit measurements to maintain ephemerides. The application of Lomb-Scargle period analysis for studying the plausibility of TTVs is explained. The analysis of the resultant TTVs from 46 transits from MicroObservatory and 47 transits from archival data in the Exoplanet Transit Database indicated the possible existence of other planets affecting the orbit of TrES-1 and improved the precision of the ephemeris by one order of magnitude. We now estimate the ephemeris to be (2 455 489.66026 BJDTDB ± 0.00044 d) + (3.0300689 ± 0.0000007) d × epoch. This analysis also demonstrates the role of small telescopes in making precise midtransit time measurements, which can be used to help maintain ephemerides and perform TTV analysis. The maintenance of ephemerides allows for an increased ability to optimize telescope time on large ground-based telescopes and space telescope missions.

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표/그림 (10)

그림 Figure 1. Light curve fit by EXOTIC for the transit of TrES-1 b on May 25, 2011.
그림 Figure 2. Breakdown of transit outcomes by light curve and image quality.
그림 Figure 3. Top left: "good light curve" from images taken on May 25, 2011. Top right: "poor light curve" from images taken on June 25, 2020. Bottom left: “partial light curve” from images taken on March 26, 2012. Bottom right: "technical issue" from images taken on July 10, 2020.
그림 Figure 4. Star field of TrES-1 b with target labeled with "T1" and comparison stars labeled in green with their magnitudes.
그림 Figure 5. O - C plot from MicroObservatory data (plotted in red) along with archival data (plotted in blue) compared to the predicted value based on the period from the NASA Exoplanet Archive and the time of the first MicroObservatory observation.
그림 Figure 6. Graph of archival and processed transit midpoints along with the fitted linear ephemeris.
표 Table 1Transit midpoints and O - C values for Figure 5 from the MicroObservatory and the Exoplanet Transit Database
표 Table 1 Continued
그림 Figure 7. Lomb-Scargle periodogram produced from O - C values with data from 46 of the transits we reduced.
그림 Figure 8. Lomb-Scargle periodogram produced from O - C values with data from 46 of the transits we reduced and 47 transits from the Exoplanet Transit Database. The three highest peaks with frequencies of 0.00275, 0.00548, and 0.01276 cycles per day (in decreasing order of power) are highlighted in red.

참고문헌 (11)

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