Target of Interest System's Third body observation via
Transiting Exoplanet Survey Satellite database.
Kittituch Suratanachaiboonlert1, Nathan Changchit1 and Pathit
Techataweekul1
Vichien Donram2 and Supachai Awiphan3
Princess Chulabhorn Science High School Chonburi
1 Science and Mathematics Student, Princess Chulabhorn Science High School
Chonburi
2 Computer Science Teacher,
3 Researcher,
Princess Chulabhorn Science High School Chonburi
National Astronomical Research Institute of Thailand
Abstract
Due to Limited Astronomical resources, as a result, the process
of identifying planet status became improbable. This article
aims to determine 5000 targets of interest (TOIs) objects to find
the existence of a third body in each TOI system that the
Transiting Exoplanet Survey Satellite (TESS) telescope was
unable to detect due to the Low Inclination of the planet.
Moreover, the number of systems exists a third body and ETC.
Lastly, serve as a data reference to support TESS Information
integrity. By Utilizing the Lightkurve module to find the
fluctuation in light by capturing photons in each image pixel.
Furthermore, form a graph for planet parameters, and test the
information
accuracy by comparing various databases
constructing an O-C diagram of reference data and research
data for percentage data discrepancy and calibration.
Converting the O-C diagram in the form of a parabolic function
examines the graph for determining the possibility of a third
body in the TOI system. The study found that the efficiency
comparison between Transitfit and NASA pipeline parameter
value has a minuscule average difference. Furthermore, from
the O-C graph of all targets of interest, there are hundreds of
systems, and the third body exists.
Key words: Third body, TESS, Lightkurve, Transitfit and O-C
diagram
Introduction
There are many systems out there in the universe, much so
that the astronomical resource we currently have is not enough
to discover all of them. As a result, the ability to ascertain the
uncertainty of information in the system outside of the solar
system became improbable but with the new technological
advantage of integrating modules and software to detect
elements in the system. With this, one can achieve faster
results with higher accuracy. The module utilized in this project
is called Lightkurve, it detects the amount of luminosity of the
target by capturing the amount of luminosity from pixels of star
images collected by NASA Kepler and TESS planet-hunting
telescopes and Transitfit module to help in the analysis of the
data. with this in mind, this article aims to determine the
existence of a third body of 5000 targets of interest that
transiting exoplanet survey satellites cannot detect.
Objectives
1.
To determine the existence of a third body in a target of
interest system
2.
The article shall serve as reference data for those who
wish to implement further the
project or shortcut for finding the Third body target of
interest code from 5000 TOIs
on the database.
3.
To construct an instrument for observation of celestial
objects.
4.
To serve as inspiration for future students and youth who
take an interest in the field
of Astronomy and Astrophysics.
Experimental Method
Download all necessary data from EXOFOP, which is t0,
a, inc, rp, teff, z, and logg in case of error. If there is no data
calling function, error % = error mode in the frequency
distribution
Lightkurve module: calling in Lightkurve module to
access image database which the necessary info needed to
input are planet’s name, mission, and sector. The mission
section input “TESS,” and the other info can be found in
Lightkurve. All left is to loop all the data from start to finish.
Furthermore, calibrate the error that occurs.
Transitfit module: overlapping the output from Lightkurve
in Transitfit using Markov Chain Monte Carlo and Nested
sampling method to solve limb darkening solution problem
which can cause elliptical integral, the output will exist in the
form of graph and parameter which is t0, a, inc, and rp.
Compare the accuracy of data to the database for efficiency
checkup.
Third body detection: open allow TTV mode in Transitfit
and code the program to receive pkl file for O-C diagram
specifying the difference of t0 value between observation and
post-processed data. Lastly, Write Generalized Lomb-Scargle
Periodogram (GLS) for constructing the sine graph to find the
possibility of the third body, by calculating the mass from transit
data discrepancy approximation for first resonance system j:
j+1 in Agol et al. (2005)
Result and Discussion
As a result of incorporating Lightkurve and Transitfit
modules into calculating 5000 TESS datasets and three million
light curves in 3 weeks, the parameter value Markov Chain
Monte Carlo has fitted with constant proportion compared with
the initial value is as follows.
Ratio Stellar Radii
Ratio Planet
Ratio Inclination
Radius
Value
Error
Value
Error
Value
Error
1.00974 0.00109 1.00505 0.00122 1.01067 0.00237
When compared with the database, the difference in data
will indicate the efficiency of the image and Transitfit. In the
observation of the existence of a third body, 200 planets meet
the requirement and are ready to use, with a long span of
process. Currently, 27 planets have been processed from the
data. We found that there is one system that exists a third body
which is in TOI 193.01 with a period of 0.79206924 days based
on Agol et al. (2005) calculation, we can conclude that the third
body mass is equal to 39.39 earth mass.
Aperture from TOI 193.01
Lightcurve
from TOI 193.01
Instance of TOI TTV Signal
Conclusion
Lightkurve and Transitfit modules provide outstanding
assistance in calculating and sorting information. In which the
ratio between the initial parameter and best fit parameter of
stellar radii, planet radius, and inclination is 1.00974 ± 0.00109,
1.00505 ± 0.00122 and 1.01067 ± 0.00237 respectively,
indicating
the
efficiency
of
data
sets
and
modules.
Furthermore, from observing third body existence from
preliminary 27 planets, we found an interesting candidate
which is in TOI 193.01 with a period of 0.79206924 days with
a mass of 39.39 times Earth's mass that meets the planet
requirement.
Reference
Joshua Hayes and collaborators Detrending TransitFit,
10 July 2021,
https://transitfit.readthedocs.io/en/latest/detrending.html
Lightkurve developers What’s new in Lightkurve 2?,
Lightkurve v2.2 6 June 2022
https://docs.lightkurve.org/whats-new-v2.html
NExScI ExoFOP, 2020, https://exofop.ipac.caltech.edu/tess/
Jason Steffen, Re'em Sari, Will Clarkson, On detecting
terrestrial planets with timing of giant planet transits, Oxford
Academy, 2 May 2005,
https://academic.oup.com/mnras/article/359/2/567/987335?lo
gin=false&fbclid=IwAR2bPbORi977wJC1nFnhd0bey8mW47E
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