Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/34875
DC Field | Value | Language |
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dc.contributor.author | PINO, Lorenzo | en_US |
dc.contributor.author | Brogi, M. | en_US |
dc.contributor.author | Désert, J.M. | en_US |
dc.contributor.author | NASCIMBENI, VALERIO | en_US |
dc.contributor.author | BONOMO, ALDO STEFANO | en_US |
dc.contributor.author | Rauscher, E. | en_US |
dc.contributor.author | Basilicata, M. | en_US |
dc.contributor.author | BIAZZO, Katia | en_US |
dc.contributor.author | BIGNAMINI, ANDREA | en_US |
dc.contributor.author | BORSA, Francesco | en_US |
dc.contributor.author | CLAUDI, Riccardo | en_US |
dc.contributor.author | COVINO, Elvira | en_US |
dc.contributor.author | Di Mauro, M.P. | en_US |
dc.contributor.author | Guilluy, G. | en_US |
dc.contributor.author | MAGGIO, Antonio | en_US |
dc.contributor.author | Malavolta, L. | en_US |
dc.contributor.author | MICELA, Giuseppina | en_US |
dc.contributor.author | MOLINARI, Emilio Carlo | en_US |
dc.contributor.author | MOLINARO, Marco | en_US |
dc.contributor.author | Montalto, M. | en_US |
dc.contributor.author | Nardiello, D. | en_US |
dc.contributor.author | Pedani, M. | en_US |
dc.contributor.author | Piotto, G. | en_US |
dc.contributor.author | PORETTI, Ennio | en_US |
dc.contributor.author | RAINER, Monica | en_US |
dc.contributor.author | SCANDARIATO, GAETANO | en_US |
dc.contributor.author | SICILIA, Daniela | en_US |
dc.contributor.author | SOZZETTI, Alessandro | en_US |
dc.date.accessioned | 2024-03-05T15:15:04Z | - |
dc.date.available | 2024-03-05T15:15:04Z | - |
dc.date.issued | 2022 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/34875 | - |
dc.description.abstract | Aims. We present a novel method for studying the thermal emission of exoplanets as a function of orbital phase at very high spectral resolution, and use it to investigate the climate of the ultra-hot Jupiter KELT-9b. Methods. We combine three nights of HARPS-N and two nights of CARMENES optical spectra, covering orbital phases between quadratures (0.25 < φ < 0.75), when the planet shows its day-side hemisphere with different geometries. We co-add the signal of thousands of Fea I lines through cross-correlation, which we map to a likelihood function. We investigate the phase-dependence of two separate observable quantities, namely (i) the line depths of Fea I and (ii) their Doppler shifts, introducing a new method that exploits the very high spectral resolution of our observations. Results. We confirm a previous detection of Fea I emission, and demonstrate a precision of 0.5 km s-1 on the orbital properties of KELT-9b when combining all nights of observations. By studying the phase-resolved Doppler shift of Fea I lines, we detect an anomaly in the planet's orbital radial velocity well-fitted with a slightly eccentric orbital solution (e = 0.016 ± 0.003, ω = 150-11+13, 5σ preference). However, we argue that this anomaly is caused by atmospheric circulation patterns, and can be explained if neutral iron gas is advected by day-to-night atmospheric wind flows of the order of a few km s-1. We additionally show that the Fea I emission line depths are symmetric around the substellar point within 10 (2σ), possibly indicating the lack of a large hot-spot offset at the altitude probed by neutral iron emission lines. Finally, we do not obtain a significant preference for models with a strong phase-dependence of the Fea I emission line strength. We show that these results are qualitatively compatible with predictions from general circulation models (GCMs) for ultra-hot Jupiter planets. Conclusions. Very high-resolution spectroscopy phase curves are of sufficient sensitivity to reveal a phase dependence in both the line depths and their Doppler shifts throughout the orbit. They constitute an under-exploited treasure trove of information that is highly complementary to space-based phase curves obtained with HST and JWST, and open a new window onto the still poorly understood climate and atmospheric structure of the hottest planets known to date. | en_US |
dc.language.iso | eng | en_US |
dc.title | The GAPS Programme at TNG: XLI. The climate of KELT-9b revealed with a new approach to high-spectral-resolution phase curves | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/202244593 | en_US |
dc.identifier.scopus | 2-s2.0-85145437622 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2022/12/aa44593-22/aa44593-22.html | en_US |
dc.identifier.url | http://www.scopus.com/inward/record.url?eid=2-s2.0-85145437622&partnerID=MN8TOARS | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 668 | en_US |
dc.relation.firstpage | A176 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | 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. Arcetri | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.orcid | 0000-0002-1321-8856 | - |
crisitem.author.orcid | 0000-0001-9770-1214 | - |
crisitem.author.orcid | 0000-0002-6177-198X | - |
crisitem.author.orcid | 0000-0002-1892-2180 | - |
crisitem.author.orcid | 0000-0002-5606-6354 | - |
crisitem.author.orcid | 0000-0003-4830-0590 | - |
crisitem.author.orcid | 0000-0001-7707-5105 | - |
crisitem.author.orcid | 0000-0002-6187-6685 | - |
crisitem.author.orcid | 0000-0001-5154-6108 | - |
crisitem.author.orcid | 0000-0002-6492-2085 | - |
crisitem.author.orcid | 0000-0002-9900-4751 | - |
crisitem.author.orcid | 0000-0002-1742-7735 | - |
crisitem.author.orcid | 0000-0001-5028-6041 | - |
crisitem.author.orcid | 0000-0003-1200-0473 | - |
crisitem.author.orcid | 0000-0002-8786-2572 | - |
crisitem.author.orcid | 0000-0003-2029-0626 | - |
crisitem.author.orcid | 0000-0002-7504-365X | - |
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 | |
---|---|---|---|---|
aa44593-22.pdf | Pdf editoriale | 2.99 MB | Adobe PDF | View/Open |
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