The detection and investigation of exoplanets with MASTER Global network telescopes

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Resumo

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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Sobre autores

V. Lipunov

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

Autor responsável pela correspondência
Email: lipunov@sai.msu.ru

Physics Department

Rússia, Moscow; Moscow

A. Tarasenkov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Rússia, Moscow

A. Kuznetsov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Rússia, Moscow

P. Balanutsa

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

Email: lipunov@sai.msu.ru
Rússia, Moscow; Moscow

G. Antipov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Rússia, Moscow

Ya. Kechin

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Rússia, Moscow

N. Tyurina

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Rússia, Moscow

E. Gorbovskoy

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lipunov@sai.msu.ru
Rússia, Moscow

D. Buckley

South African Astronomical Observatory (SAAO)

Email: lipunov@sai.msu.ru
República da África do Sul, 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. Tlatov

Kislovodsk Mountain Astronomical Station, Main Astronomical Observatory of RAS

Email: lipunov@sai.msu.ru
Rússia, Kislovodsk

R. Rebolo Lopez

Instituto de Astrofisica de Canarias (IAC)

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

N. Budnev

Irkutsk State University, Institute of Applied Physics

Email: lipunov@sai.msu.ru
Rússia, Irkutsk

O. Gress

Irkutsk State University, Institute of Applied Physics

Email: lipunov@sai.msu.ru
Rússia, Irkutsk

V. Yurkov

Blagoveshchensk State Pedagogical University

Email: lipunov@sai.msu.ru
Rússia, Blagoveshchensk

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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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Declaração de direitos autorais © The Russian Academy of Sciences, 2024