Skip navigation
  • INAF logo
  • Home
  • Communities
    & Collections
  • Research outputs
  • Researchers
  • Organization units
  • Projects
  • Explore by
    • Research outputs
    • Researchers
    • Organization units
    • Projects
  • Login:
    • My DSpace
    • Receive email
      updates
    • Edit Account details
  • Italian
  • English

  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/28667
Title: UVES spectroscopy of T Chamaeleontis: line variability, mass accretion rate, and spectro-astrometric analysis
Authors: Cahill, Eoin
Whelan, Emma T.
Huélamo, Nuria
ALCALA', JUAN MANUEL 
Issue Date: 2019
Journal: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 
Number: 484
Issue: 3
First Page: 4315
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.
URI: http://hdl.handle.net/20.500.12386/28667
URL: https://academic.oup.com/mnras/article/484/3/4315/5303749
ISSN: 0035-8711
DOI: 10.1093/mnras/stz280
Bibcode ADS: 2019MNRAS.484.4315C
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

Files in This Item:
File Description SizeFormat 
stz280.pdfPDF editoriale2.68 MBAdobe PDFView/Open
Show full item record

Page view(s)

7
checked on Jan 26, 2021

Download(s)

2
checked on Jan 26, 2021

Google ScholarTM

Check

Altmetric


Items in DSpace are published in Open Access, unless otherwise indicated.


Explore by
  • Communities
    & Collections
  • Research outputs
  • Researchers
  • Organization units
  • Projects

Informazioni e guide per autori

https://openaccess-info.inaf.it: tutte le informazioni sull'accesso aperto in INAF

Come si inserisce un prodotto: le guide a OA@INAF

La Policy INAF sull'accesso aperto

Documenti e modelli scaricabili

Feedback
Built with DSpace-CRIS - Extension maintained and optimized by Logo 4SCIENCE