Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/28667
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Cahill, Eoin | en_US |
dc.contributor.author | Whelan, Emma T. | en_US |
dc.contributor.author | Huélamo, Nuria | en_US |
dc.contributor.author | ALCALA', JUAN MANUEL | en_US |
dc.date.accessioned | 2020-12-03T16:25:35Z | - |
dc.date.available | 2020-12-03T16:25:35Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28667 | - |
dc.description.abstract | Although advances in exoplanet detection techniques have seen an increase in discoveries, observing a planet in the earliest stages of formation still remains a difficult task. Here four epochs of spectra of the transitional disc object T Chamaeleontis are analysed to determine whether spectro-astrometry can be used to detect a signal from its proposed protoplanet, T Cha b. The unique properties of T Cha are also further constrained. Hα and [O I] λ 6300, the most prominent lines, were analysed using spectro-astrometry. Hα being a direct accretion tracer is the target for the T Cha b detection, while [O I] λ 6300 is considered to be an indirect tracer of accretion. [O I] λ 6300 is classified as a broad low-velocity component (BC LVC). \dot{M}_acc was derived for all epochs using new [O I] λ 6300 LVC relationships and the Hα line luminosity. It is shown that a wind is the likely origin of the [O I] λ 6300 line and that the [O I] λ 6300 line serves as a better accretion tracer than Hα in this case. From the comparison between \dot{M}_acc({[O I]}) and \dot{M}_acc(Hα) it is concluded that T Cha is not an intrinsically weak accretor but rather that a significant proportion of the Hα emission tracing accretion is obscured. T Cha b is not detected in the spectro-astrometric analysis yet a detection limit of 0.5 mas is derived. The analysis in this case was hampered by spectro-astrometric artefacts and by the unique properties of T Cha. While it seems that spectro-astrometry as a means of detecting exoplanets in TDs can be challenging, it can be used to put a limit on the strength of the Hα emission from accreting planetary companions, and thus can have an important input into the planning of high-angular resolution observations. | en_US |
dc.language.iso | eng | en_US |
dc.title | UVES spectroscopy of T Chamaeleontis: line variability, mass accretion rate, and spectro-astrometric analysis | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stz280 | en_US |
dc.identifier.scopus | 2-s2.0-85093886341 | en_US |
dc.identifier.isi | 000462410300105 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/484/3/4315/5303749 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 484 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 4315 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | ESP | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2019MNRAS.484.4315C | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering | en_US |
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. Capodimonte | - |
crisitem.author.orcid | 0000-0001-8657-095X | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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stz280.pdf | PDF editoriale | 2.68 MB | Adobe PDF | View/Open |
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