The detection and investigation of exoplanets with MASTER Global network telescopes

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Abstract

The paper presents the method for detecting exoplanets in the archive of images obtained on telescopes of the MASTER Global Network since 2002. The unique archive represents homogeneous photometric data obtained during over 20 years for the northern (MASTER-Amur, MASTER-Tunka, MASTER-Kislovodsk, MASTER-Tavrida, MASTER-IAC, MASTER-OAGH) and for 11 years for the southern sky (MASTER-OAFA, MASTER-SAAO). Algorithm of gamma-ray burst error box observation on the MASTER wide-field telescopes make it possible to detect transit phenomena and find exoplanets in archival data. The article presents the results of a photometric analysis of the TESS exoplanet candidate TOI–3570.01.

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About the authors

V. M. Lipunov

Lomonosov Moscow State University; Lomonosov Moscow State University, Sternberg Astronomical Institute

Author for correspondence.
Email: lipunov@sai.msu.ru

Physics Department

Russian Federation, Moscow; Moscow

A. N. Tarasenkov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Russian Federation, Moscow

A. S. Kuznetsov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Russian Federation, Moscow

P. V. Balanutsa

Lomonosov Moscow State University, Sternberg Astronomical Institute; Research Center Kurchatov Institute

Email: lipunov@sai.msu.ru
Russian Federation, Moscow; Moscow

G. A. Antipov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Russian Federation, Moscow

Ya. Yu. Kechin

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Russian Federation, Moscow

N. V. Tyurina

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Russian Federation, Moscow

E. S. Gorbovskoy

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Russian Federation, Moscow

D. Buckley

South African Astronomical Observatory (SAAO)

Email: lipunov@sai.msu.ru
South Africa, Cape Town

C. Francile

Observatorio Astronomico Felix Aguilar (OAFA), National University of San Juan

Email: lipunov@sai.msu.ru
Argentina

F. Podesta

Observatorio Astronomico Felix Aguilar (OAFA), National University of San Juan

Email: lipunov@sai.msu.ru
Argentina

A. G. Tlatov

Kislovodsk Mountain Astronomical Station, Main Astronomical Observatory of RAS

Email: lipunov@sai.msu.ru
Russian Federation, Kislovodsk

R. Rebolo Lopez

Instituto de Astrofisica de Canarias (IAC)

Email: lipunov@sai.msu.ru
Spain, La Laguna (Tenerife)

N. M. Budnev

Irkutsk State University, Institute of Applied Physics

Email: lipunov@sai.msu.ru
Russian Federation, Irkutsk

O. A. Gress

Irkutsk State University, Institute of Applied Physics

Email: lipunov@sai.msu.ru
Russian Federation, Irkutsk

V. V. Yurkov

Blagoveshchensk State Pedagogical University

Email: lipunov@sai.msu.ru
Russian Federation, Blagoveshchensk

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Supplementary files

Supplementary Files
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2. Fig. 1. The P-band light curve of TOI–3570.01 on June 29, 2015, obtained with the MASTER-IAC telescope. The exposure duration is 180 s, averaging over two exposures (i.e. 360 s). The green dots are the photometry results corrected for atmospheric absorption, the green curve shows the transit model constructed by the AstroimageJ program. The colored dots at the bottom, approximated by straight lines, represent the photometry of the comparison stars. The gray vertical lines indicate the actual beginning and end of the transit, and the red ones are the ephemerides calculated by the Tapir package. The characteristics of the planet obtained from the model are shown at the top of the figure.

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3. Fig. 2. The light curve of TOI-3661.01 in the V and R bands on December 29, 2023, obtained with the MASTER-Kislovodsk telescope (western (V) and eastern (R) channels). The exposure duration is 60 s, averaging over 2 points in the V band and 3 points in the R band. Green dots are the photometry results corrected for atmospheric absorption, the green curve shows the transit model constructed by the AstroimageJ program. The colored dots at the bottom, approximated by straight lines, represent the photometry of the comparison stars. The gray vertical lines indicate the actual beginning and end of the transit, and the red ones are the ephemerides calculated by the Tapir package. The characteristics of the planet obtained from the model are shown at the top of the figure.

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4. Supplement
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