Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/34909
DC Field | Value | Language |
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dc.contributor.author | DAMASSO, Mario | en_US |
dc.contributor.author | SCANDARIATO, GAETANO | en_US |
dc.contributor.author | NASCIMBENI, VALERIO | en_US |
dc.contributor.author | Nardiello, D. | en_US |
dc.contributor.author | Mancini, L. | en_US |
dc.contributor.author | Marino, G. | en_US |
dc.contributor.author | BRUNO, Giovanni | en_US |
dc.contributor.author | Brandeker, A. | en_US |
dc.contributor.author | LETO, Giuseppe | en_US |
dc.contributor.author | Marzari, F. | en_US |
dc.contributor.author | LANZA, Antonino Francesco | en_US |
dc.contributor.author | BENATTI, Serena | en_US |
dc.contributor.author | DESIDERA, Silvano | en_US |
dc.contributor.author | Béjar, V. J. S. | en_US |
dc.contributor.author | Biagini, A. | en_US |
dc.contributor.author | BORSATO, LUCA | en_US |
dc.contributor.author | Cabona, L. | en_US |
dc.contributor.author | CLAUDI, Riccardo | en_US |
dc.contributor.author | Lodieu, N. | en_US |
dc.contributor.author | MAGGIO, Antonio | en_US |
dc.contributor.author | Mallorquín, M. | en_US |
dc.contributor.author | MESSINA, Sergio | en_US |
dc.contributor.author | MICELA, Giuseppina | en_US |
dc.contributor.author | RICCI, Davide | en_US |
dc.contributor.author | SOZZETTI, Alessandro | en_US |
dc.contributor.author | Suárez Mascareño, A. | en_US |
dc.contributor.author | TURRINI, Diego | en_US |
dc.contributor.author | Zapatero Osorio, M. R. | en_US |
dc.date.accessioned | 2024-03-07T09:50:17Z | - |
dc.date.available | 2024-03-07T09:50:17Z | - |
dc.date.issued | 2023 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/34909 | - |
dc.description.abstract | Context. The 20 Myr old star V1298 Tau hosts at least four planets. Since its discovery, this system has been a target of intensive photometric and spectroscopic monitoring. To date, the characterisation of its architecture and planets' fundamental properties has been very challenging. <BR /> Aims: The determination of the orbital ephemeris of the outermost planet V1298 Tau e remains an open question. Only two transits have been detected so far by Kepler/K2 and TESS, allowing for a grid of reference periods to be tested with new observations, without excluding the possibility of transit timing variations. Observing a third transit would allow for better constraints to be set on the orbital period and would also help in determining an accurate radius for V1298 Tau e because the previous transits showed different depths. <BR /> Methods: We observed V1298 Tau with the CHaracterising ExOPlanet Satellite (CHEOPS) to search for a third transit of planet e within observing windows selected to test three of the shortest predicted orbital periods. We also collected ground-based observations to verify the result found with CHEOPS. We reanalysed Kepler/K2 and TESS light curves to test how the results derived from these data are affected by alternative photometric extraction and detrending methods. <BR /> Results: We report the CHEOPS detection of a transit-like signal that could be attributed to V1298 Tau e. If so, that result would imply that the orbital period calculated from fitting a linear ephemeris to the three available transits is close to ~45 days. Results from the ground-based follow-up marginally support this possibility. We found that i) the transit observed by CHEOPS has a longer duration compared to that of the transits observed by Kepler/K2 and TESS; and ii) the transit observed by TESS is >30% deeper than that of Kepler/K2 and CHEOPS, and it is also deeper than the measurement previously reported in the literature, according to our reanalysis. <BR /> Conclusions: If the new transit detected by CHEOPS is found to be due to V1298 Tau e, this would imply that the planet experiences TTVs of a few hours, as deduced from three transits, as well as orbital precession, which would explain the longer duration of the transit compared to the Kepler/K2 and TESS signals. Another and a priori less likely possibility is that the newly detected transit belongs to a fifth planet with a longer orbital period than that of V1298 Tau e. Planning further photometric follow-up to search for additional transits is indeed necessary to solve the conundrum, as well as to pin down the radius of V1298 Tau e.... | en_US |
dc.language.iso | eng | en_US |
dc.title | Photometric follow-up of the 20 Myr old multi-planet host star V1298 Tau with CHEOPS and ground-based telescopes | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/202346840 | en_US |
dc.identifier.scopus | 2-s2.0-85176803770 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2023/12/aa46840-23/aa46840-23.html | en_US |
dc.identifier.url | https://api.elsevier.com/content/abstract/scopus_id/85176803770 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 680 | en_US |
dc.relation.firstpage | A8 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.orcid | 0000-0001-9984-4278 | - |
crisitem.author.orcid | 0000-0003-2029-0626 | - |
crisitem.author.orcid | 0000-0001-9770-1214 | - |
crisitem.author.orcid | 0000-0002-3288-0802 | - |
crisitem.author.orcid | 0000-0002-0040-5011 | - |
crisitem.author.orcid | 0000-0001-5928-7251 | - |
crisitem.author.orcid | 0000-0002-4638-3495 | - |
crisitem.author.orcid | 0000-0001-8613-2589 | - |
crisitem.author.orcid | 0000-0003-0066-9268 | - |
crisitem.author.orcid | 0000-0001-7707-5105 | - |
crisitem.author.orcid | 0000-0001-5154-6108 | - |
crisitem.author.orcid | 0000-0002-2851-2468 | - |
crisitem.author.orcid | 0000-0002-9900-4751 | - |
crisitem.author.orcid | 0000-0002-9790-0552 | - |
crisitem.author.orcid | 0000-0002-7504-365X | - |
crisitem.author.orcid | 0000-0002-1923-7740 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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damasso.pdf | Pdf editoriale | 6.62 MB | Adobe PDF | View/Open |
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