AMBER-NACO aperture-synthesis imaging of the half-obscured central star and the edge-on disk of the red giant L2 Puppis

被引:8
作者
Ohnaka, K. [1 ,2 ]
Schertl, D. [2 ]
Hofmann, K. -H. [2 ]
Weigelt, G. [2 ]
机构
[1] Univ Catolica Norte, Inst Astron, Antofagasta, Chile
[2] Max Planck Inst Radioastron, D-53121 Bonn, Germany
关键词
infrared: stars; techniques: interferometric; stars: imaging; stars: AGB and post-AGB; stars: individual: L2 Pup; circumstellar matter; 1ST OVERTONE LINES; SPECKLE-MASKING; DYNAMICAL ATMOSPHERE; AGB STARS; CIRCUMSTELLAR ENVELOPES; SUPERGIANT ANTARES; PLANETARY-NEBULAE; DUST DISK; MASS-LOSS; MU-M;
D O I
10.1051/0004-6361/201526338
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Aims. The red giant L-2 Pup started a dimming event in 1994, which is considered to be caused by the ejection of dust clouds. We present near-IR aperture-synthesis imaging of L-2 Pup achieved by combining data from VLT/NACO and the AMBER instrument of the Very Large Telescope Interferometer (VLTI). Our aim is to spatially resolve the innermost region of the circumstellar environment. Methods. We carried out speckle interferometric observations at 2.27 mu m with VLT/NACO and long-baseline interferometric observations with VLTI/AMBER at 2.2-2.35 mu m with baselines of 15-81 m. We also extracted an 8.7 mu m image from the mid-IR VLTI instrument MIDI. Results. The diffraction-limited image obtained by bispectrum speckle interferometry with NACO with a spatial resolution of 57 mas shows an elongated component. The aperture-synthesis imaging combining the NACO speckle data and AMBER data with a spatial resolution of 5.6 x 7.3 mas further resolves not only this elongated component, but also the central star. The reconstructed image reveals that the elongated component is a nearly edge-on disk with a size of similar to 180 x 50 mas lying in the E-W direction, and furthermore, that the southern hemisphere of the central star is severely obscured by the equatorial dust lane of the disk. The angular size of the disk is consistent with the distance that the dust clouds that were ejected at the onset of the dimming event should have traveled by the time of our observations, if we assume that the dust clouds moved radially. This implies that the formation of the disk may be responsible for the dimming event. The 8.7 mu m image with a spatial resolution of 220 mas extracted from the MIDI data taken in 2004 (seven years before the AMBER and NACO observations) shows an approximately spherical envelope without a signature of the disk. This suggests that the mass loss before the dimming event may have been spherical.
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