The detection and investigation of exoplanets with MASTER Global network telescopes

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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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作者简介

V. Lipunov

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

编辑信件的主要联系方式.
Email: lipunov@sai.msu.ru

Physics Department

俄罗斯联邦, Moscow; Moscow

A. Tarasenkov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
俄罗斯联邦, Moscow

A. Kuznetsov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
俄罗斯联邦, Moscow

P. Balanutsa

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

Email: lipunov@sai.msu.ru
俄罗斯联邦, Moscow; Moscow

G. Antipov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
俄罗斯联邦, Moscow

Ya. Kechin

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
俄罗斯联邦, Moscow

N. Tyurina

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
俄罗斯联邦, Moscow

E. Gorbovskoy

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
俄罗斯联邦, Moscow

D. Buckley

South African Astronomical Observatory (SAAO)

Email: lipunov@sai.msu.ru
南非, Cape Town

C. Francile

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

Email: lipunov@sai.msu.ru
阿根廷

F. Podesta

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

Email: lipunov@sai.msu.ru
阿根廷

A. Tlatov

Kislovodsk Mountain Astronomical Station, Main Astronomical Observatory of RAS

Email: lipunov@sai.msu.ru
俄罗斯联邦, Kislovodsk

R. Rebolo Lopez

Instituto de Astrofisica de Canarias (IAC)

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

N. Budnev

Irkutsk State University, Institute of Applied Physics

Email: lipunov@sai.msu.ru
俄罗斯联邦, Irkutsk

O. Gress

Irkutsk State University, Institute of Applied Physics

Email: lipunov@sai.msu.ru
俄罗斯联邦, Irkutsk

V. Yurkov

Blagoveshchensk State Pedagogical University

Email: lipunov@sai.msu.ru
俄罗斯联邦, Blagoveshchensk

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补充文件

附件文件
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1. JATS XML
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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