EDP Sciences
Free access
Volume 496, Number 1, March II 2009
Page(s) 133 - 137
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:200810403
Published online 14 January 2009
A&A 496, 133-137 (2009)
DOI: 10.1051/0004-6361:200810403

Research Note

Revisiting the optical interferometry observations of HR 4049

J.-L. Menut1, O. Chesneau2, E. Bakker3, B. Lopez2, G. Perrin4, C. Leinert5, and A. Quirrenbach6

1  Observatoire de la Côte d'Azur, Dpt. Gemini-CNRS-UMR 6203, BP 4229, 06304 Nice, France
    e-mail: menut@obs-azur.fr
2  Observatoire de la Côte d'Azur, Dpt. Gemini-CNRS-UMR 6203, Avenue Copernic, 06130 Grasse, France
    e-mail: Olivier.Chesneau@obs-azur.fr
3  Observatoire de Paris – Section de Meudon, 5 Place Jules Janssen, 92195 Meudon, France
4  Magdalena Ridge Observatory, New Mexico Tech, 801 Leroy Place, Socorro, NM 87801, USA
5  Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
6  Zentrum für Astronomie, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany

Received 17 June 2008 / Accepted 10 November 2008

Aims. We present high spatial resolution observations in the mid-infrared of the dusty core of the binary system HR 4049.
Methods. We used the mid-infrared interferometer MIDI/VLTI with 40 m projected baselines. These observations provided two spectrally dispersed visibility curves at a spatial resolution of ~10 mas. Acquisition images and spectra are in addition obtained with a single telescope spatial resolution of ~250 mas.
Results. The MIDI spectra show features due to emission lines (7.9, 8.6 and 11.3 micron) attributed to PAHs. The comparison between ISO and MIDI spectra and dispersed visibility curves allows us to investigate the budget of continuum and PAH emission from distant regions to the inner regions of the compact dusty structure. The flux balance between these different PAH features is different to the one seen in the large beam ISO spectrum, suggesting different contributions at varying locations from the central star for the different PAH species. These features are over-resolved (i.e. their correlated flux is close to zero), placing the bulk of their line forming region at least at 50-70 mas from the central star. The continuum extension is estimated to range between 23 and 27 mas using a Gaussian model, and is very close to the K-band sizes measured with VINCI/VLTI, implying that the emitting regions of the near and mid-IR are similar. The visibilities from the two different baselines do not allow us to constrain the shape of the continuum emitting region but noticeable differences between them suggest that the N band dusty environment is flattened in a direction that coincides with the one suggested by previous polarimetric observations.

Key words: techniques: interferometric -- techniques: high angular resolution -- stars: AGB and post-AGB -- stars: mass-loss -- stars: circumstellar matter

© ESO 2009