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Warm dust resolved in the cold disk around T Chamaeleontis with VLTI/AMBER

Olofsson, J. and Benisty, Myriam and Augereau, J.-C. and Pinte, C. and Ménard, F. and Tatulli, E. and Berger, J.-P. and Malbet, F. and Merín, B. and van Dishoeck, E. F. and Lacour, S. and Pontoppidan, K. M. and Monin, J.-L. and Brown, J. M. and Blake, G. A. (2011) Warm dust resolved in the cold disk around T Chamaeleontis with VLTI/AMBER. Astronomy and Astrophysics, 528 . Art. No. L6. ISSN 0004-6361.

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Context. The transition between massive Class II circumstellar disks and Class III debris disks, with dust residuals, has not yet been clearly understood. Disks are expected to dissipate with time, and dust clearing in the inner regions can be the consequence of several mechanisms. Planetary formation is one of them that will possibly open a gap inside the disk. Aims. According to recent models based on photometric observations, T Cha is expected to present a large gap within its disk, meaning that an inner dusty disk is supposed to have survived close to the star. We investigate this scenario with new near-infrared interferometric observations. Methods. We observed T Cha in the H and K bands using the AMBER instrument at VLTI and used the MCFOST radiative transfer code to model the SED of T Cha and the interferometric observations simultaneously and to test the scenario of an inner dusty structure. We also used a toy model of a binary to check that a companion close to the star can reproduce our observations. Results. The scenario of a close (few mas) companion cannot satisfactorily reproduce the visibilities and SED, while a disk model with a large gap and an inner ring producing the bulk of the emission (in H and K-bands) close to 0.1 AU is able to account for all the observations. Conclusions. With this study, the presence of an optically thick inner dusty disk close to the star and dominating the H and K-bands emission is confirmed. According to our model, the large gap extends up to ~7.5 AU. This points toward a companion (located at several AU) gap-opening scenario to explain the morphology of T Cha.

Item Type:Article
Related URLs:
URLURL TypeDescription
Benisty, Myriam0000-0002-7695-7605
Pinte, C.0000-0001-5907-5179
Berger, J.-P.0000-0001-5025-0428
van Dishoeck, E. F.0000-0001-7591-1907
Lacour, S.0000-0002-6948-0263
Pontoppidan, K. M.0000-0001-7552-1562
Blake, G. A.0000-0003-0787-1610
Additional Information:© 2011 ESO. Article published by EDP Sciences. Received 4 November 2010; Accepted 4 January 2011. Published online 24 February 2011. Based on AMBER observations collected at the VLTI (European Southern Observatory, Paranal, Chile) with open time programs 083.C-0295(A,B). The authors thank the anonymous referee for the constructive and useful comments provided. They also thank the Max Planck Society, the Programme National de Physique Stellaire (PNPS) and ANR (contract ANR-07-BLAN-0221) for supporting part of this research. C. Pinte acknowledges funding from the European Commission’s 7th Framework Program (contracts PIEFGA-2008-220891 and PERG06-GA-2009-256513). CNRS is acknowledged for having supported this work with allocation of 0.3 night in guaranteed time observations.
Funding AgencyGrant Number
Max Planck SocietyUNSPECIFIED
Programme National de Physique Stellaire (PNPS)UNSPECIFIED
Agence Nationale pour la Recherche (ANR)ANR-07-BLAN-0221
Marie Curie FellowshipPIEFGA-2008-220891
Marie Curie FellowshipPERG06-GA-2009-256513
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Subject Keywords:stars: pre-main sequence; stars: evolution; protoplanetary disks; circumstellar matter; infrared: stars; techniques: interferometric
Record Number:CaltechAUTHORS:20110414-105139377
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Official Citation:Warm dust resolved in the cold disk around T Chamaeleontis with VLTI/AMBER J. Olofsson, M. Benisty, J.-C. Augereau, C. Pinte, F. Ménard, E. Tatulli, J.-P. Berger, F. Malbet, B. Merín, E. F. van Dishoeck, S. Lacour, K. M. Pontoppidan, J.-L. Monin, J. M. Brown and G. A. Blake A&A 528 L6 (2011) DOI: 10.1051/0004-6361/201016074
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:23336
Deposited By: Jason Perez
Deposited On:14 Apr 2011 21:15
Last Modified:01 Nov 2019 17:03

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