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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



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ID: 448235.0, MPI für Astronomie / Publikationen_mpia
Edge-on disk around the T Tauri star [MR81] Hα 17 NE in Corona Australis
Authors:Neuhäuser, R.; Krämer, S.; Mugrauer, M.; Köhler, R.; Schmidt, T. O. B.; Ammler-von Eiff, M.; Alves, J.; Fiedler, S.; Vogt, N.
Language:English
Date of Publication (YYYY-MM-DD):2009
Title of Journal:Astronomy and Astrophysics
Journal Abbrev.:A & A
Volume:496
Start Page:777
End Page:786
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:Aims. Using the speckle camera SHARP at the 3.5 m ESO NTT, Köhler and collaborators found an object Ëœ 3.5 mag fainter in K only 1.3'' north-east of the T Tauri star [MR81] Halpha 17 in the Corona Australis (CrA) star-forming region, which could be either a brown dwarf or a T Tauri star with an edge-on disk. We attempt to study this faint object in detail. Methods: We acquired deep VLT NACO near-infrared images at three epochs to determine, whether [MR81] Halpha 17 and the nearby faint object are comoving and to measure the infrared colors of both objects. We obtained optical and infrared spectra of both objects with the VLT using FORS and ISAAC, respectively, to determine spectral types and temperatures as well as ages and masses. Results: The T Tauri star [MR81] Halpha 17 and the faint nearby object have a projected separation of 1369.58 mas, i.e. 178 AU at 130 pc. They share the same proper motion (~ 5 sigma), so that they most certainly form a bound binary pair. The apparently fainter component [MR81] Halpha 17 NE has a spectral type of M2e, while the apparently brighter component [MR81] Halpha 17 SW, the previously known T Tauri star, has a spectral type of M4-5e. We can identify a nearly edge-on disk around [MR81] Halpha 17 NE by visual inspection, which has a diameter of at least 30 to 50 AU. We are able to detect strong emission lines in [MR81] Halpha 17 NE, which are almost certainly due to ongoing accretion. The NE object is detectable only by means of its scattered light. Conclusions: If both objects are co-eval (2-3 Myr) and located at the same distance (Ëœ 130 pc as CrA), then the apparently fainter [MR81] Halpha 17
Free Keywords:astrometry; stars: binaries: visual; stars: formation; stars: pre-main sequence
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/abs/2009A%26A...496..777... [ID No:1]
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