First detection of variable radio emission originating from the infant planetary system V1298 Tau

Context. V1298 Tau is a very young and magnetically active K1V star that hosts a benchmark multi-planetary system to study planet formation and evolutionary history at the earliest stages. Thanks to the high interest, it has been the target of a multi-wavelength follow-up.

Detalles Bibliográficos
Autores: Damasso, M., Morata, Óscar, Kaur, S., Viganò, Daniele, Melis, A., Murgia, M., Pilia, Maura, Lanza, A., Del Sordo, Fabio, Antonietti, N., Kansabanik, Devojyoti, Molinari, E., Pérez-Torres, Miguel A., Sánchez-Monge, Álvaro, Maggio, A., Girart, Josep Miquel
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2025
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/389560
Acceso en línea:http://hdl.handle.net/10261/389560
Access Level:acceso abierto
Palabra clave:Planet-star interactions
Planetary systems
Stars: individual: V1298Tau
Radio continuum: planetary systems
Radio continuum: stars
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dc.title.none.fl_str_mv First detection of variable radio emission originating from the infant planetary system V1298 Tau
title First detection of variable radio emission originating from the infant planetary system V1298 Tau
spellingShingle First detection of variable radio emission originating from the infant planetary system V1298 Tau
Damasso, M.
Planet-star interactions
Planetary systems
Stars: individual: V1298Tau
Radio continuum: planetary systems
Radio continuum: stars
title_short First detection of variable radio emission originating from the infant planetary system V1298 Tau
title_full First detection of variable radio emission originating from the infant planetary system V1298 Tau
title_fullStr First detection of variable radio emission originating from the infant planetary system V1298 Tau
title_full_unstemmed First detection of variable radio emission originating from the infant planetary system V1298 Tau
title_sort First detection of variable radio emission originating from the infant planetary system V1298 Tau
dc.creator.none.fl_str_mv Damasso, M.
Morata, Óscar
Kaur, S.
Viganò, Daniele
Melis, A.
Murgia, M.
Pilia, Maura
Lanza, A.
Del Sordo, Fabio
Antonietti, N.
Kansabanik, Devojyoti
Molinari, E.
Pérez-Torres, Miguel A.
Sánchez-Monge, Álvaro
Maggio, A.
Girart, Josep Miquel
author Damasso, M.
author_facet Damasso, M.
Morata, Óscar
Kaur, S.
Viganò, Daniele
Melis, A.
Murgia, M.
Pilia, Maura
Lanza, A.
Del Sordo, Fabio
Antonietti, N.
Kansabanik, Devojyoti
Molinari, E.
Pérez-Torres, Miguel A.
Sánchez-Monge, Álvaro
Maggio, A.
Girart, Josep Miquel
author_role author
author2 Morata, Óscar
Kaur, S.
Viganò, Daniele
Melis, A.
Murgia, M.
Pilia, Maura
Lanza, A.
Del Sordo, Fabio
Antonietti, N.
Kansabanik, Devojyoti
Molinari, E.
Pérez-Torres, Miguel A.
Sánchez-Monge, Álvaro
Maggio, A.
Girart, Josep Miquel
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Istituto Nazionale di Astrofisica
European Research Council
European Commission
Agencia Estatal de Investigación (España)
Ministerio de Ciencia e Innovación (España)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Planet-star interactions
Planetary systems
Stars: individual: V1298Tau
Radio continuum: planetary systems
Radio continuum: stars
topic Planet-star interactions
Planetary systems
Stars: individual: V1298Tau
Radio continuum: planetary systems
Radio continuum: stars
description Context. V1298 Tau is a very young and magnetically active K1V star that hosts a benchmark multi-planetary system to study planet formation and evolutionary history at the earliest stages. Thanks to the high interest, it has been the target of a multi-wavelength follow-up.
publishDate 2025
dc.date.none.fl_str_mv 2025
2025
2025
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dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/389560
url http://hdl.handle.net/10261/389560
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http://dx.doi.org/10.1051/0004-6361/202553884
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spelling First detection of variable radio emission originating from the infant planetary system V1298 TauDamasso, M.Morata, ÓscarKaur, S.Viganò, DanieleMelis, A.Murgia, M.Pilia, MauraLanza, A.Del Sordo, FabioAntonietti, N.Kansabanik, DevojyotiMolinari, E.Pérez-Torres, Miguel A.Sánchez-Monge, ÁlvaroMaggio, A.Girart, Josep MiquelPlanet-star interactionsPlanetary systemsStars: individual: V1298TauRadio continuum: planetary systemsRadio continuum: starsContext. V1298 Tau is a very young and magnetically active K1V star that hosts a benchmark multi-planetary system to study planet formation and evolutionary history at the earliest stages. Thanks to the high interest, it has been the target of a multi-wavelength follow-up.Aims. We selected V1298 Tau for a first targeted follow-up at radio frequencies with the Karl G. Jansky Very Large Telescope (JVLA), the upgraded Giant Metrewave Radio Telescope (uGMRT), and the Sardinia Radio Telescope (SRT) to search for emission in the overall frequency range 0.55–7.2 GHz. Detecting radio emission from such a very active star is key to characterising its magnetosphere, allowing us in principle to probe the strength of the coronal magnetic field and plasma density.Methods. Observations were carried out between October 2023 and September 2024: three epochs (total of ∼180 min on-source) with uGMRT band-4 (0.55–0.75 GHz), 12 epochs (total of ∼427 min on-source) with the JVLA using L (1–2 GHz) and C (4.5–6.5 GHz) bands, and three epochs (total of ∼56 min on-source) with SRT using C-high band (6–7.2 GHz).Results. We report the first detection of radio emission from V1298 Tau at different epochs using the JVLA. The emission has maximum peak flux densities of 91±10 and 177±6 µJy/beam in the L- and C-band, respectively. From a comparison with contemporary optical photometry, we found that the detected emission with the highest fluxes are located around a phase of minimum of the photospheric light curve. Although the uGMRT and SRT observations could not detect the source, we measured 3σ flux density upper limits in the range ∼41–56 µJy/beam using uGMRT, while with SRT we reached upper limits down to 13 mJy. The lack of a significant fraction of circular polarisation indicates that the observed flux is not due to electron cyclotron maser emission from star-planet interaction, and it is likely produced by gyrosynchroton and/or cyclotron emission from the corona triggered by stellar magnetic activity, although we cannot exclude thermal emission, due to a lack of constraints on the brightness temperature. © The Authors 2025We thank the anonymous referee for helpful comments on the paper. M.D. acknowledges financial support through INAF mini-grant fundamental research funding for the year 2022. S.K. carried out this work within the framework of the doctoral program in Physics of the Universitat Autònoma de Barcelona. O.M., S.K., and D.V. are supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (ERC Starting Grant “IMAGINE” No. 948582). F.D.S. acknowledges support from a Marie Curie Action of the European Union (Grant agreement 101030103). We acknowledge the “María de Maeztu” award from the Spanish Science and Innovation Ministry to the Institut de Ciències de l’Espai (CEX2020-001058-M). M.P.T. acknowledges financial support from the Severo Ochoa grant CEX2021-001131-S and from the Spanish grant PID2023-147883NB-C21, funded by MCIU/AEI/10.13039/501100011033, as well as support through ERDF/EU. A.S.-M. acknowledges support from the RyC2021-032892-I grant funded by MCIN/AEI/10.13039/501100011033 and by the European Union ‘Next GenerationEU’/PRTR, as well as the program Unidad de Excelencia María de Maeztu CEX2020-001058-M, and support from the PID2023-146675NB-I00 (MCI-AEI-FEDER, UE). J.M.G. acknowledges financial support through the grant PID2023-146675NB-I00. The Sardinia Radio Telescope is funded by the Ministry of Education, University and Research (MIUR), Italian Space Agency (ASI), the Autonomous Region of Sardinia (RAS) and INAF itself and is operated as a National Facility by the National Institute for Astrophysics (INAF). We thank A. Miotello and C. Manara for useful discussions.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2020-001058-M).Peer reviewedEDP SciencesIstituto Nazionale di AstrofisicaEuropean Research CouncilEuropean CommissionAgencia Estatal de Investigación (España)Ministerio de Ciencia e Innovación (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/389560reponame:DIGITAL.CSIC. 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