Volume 402, Number 1, April IV 2003
|Page(s)||183 - 187|
|Section||Interstellar and circumstellar matter|
|Published online||07 April 2003|
The 1.2 mm image of the β Pictoris disk*
Stockholm Observatory, SCFAB, Roslagstullsbacken 21, 106 91 Stockholm, Sweden e-mail: email@example.com, firstname.lastname@example.org, email@example.com
2 ESTEC/ESA, PO Box 299, 2200AG Noordwijk, The Netherlands e-mail: firstname.lastname@example.org
3 Lick Observatory, University of California Santa Cruz, CA 95064, USA e-mail: email@example.com
Corresponding author: R. Liseau, firstname.lastname@example.org
Accepted: 5 February 2003
We present millimeter imaging observations in the 1200 μm continuum of the disk around . With the 25 beam, the disk is unresolved perpendicularly to the disk plane (10), but slightly resolved in the northeast-southwest direction (26). Peak emission is observed at the stellar position. A secondary maximum is found 1000 AU along the disk plane in the southwest, which does not positionally coincide with a similar feature reported earlier at 850 μm. Arguments are presented which could be seen in support of the reality of these features. The observed submm/mm emission is consistent with thermal emission from dust grains, which are significantly larger than those generally found in the interstellar medium, including mm-size particles, and thus more reminiscent of the dust observed in protostellar disks. Modelling the observed scattered light in the visible and the emission in the submm/mm provides evidence for the particles dominating the scattering in the visible/NIR and those primarily responsible for the thermal emission at longer wavelengths belonging to different populations.
Key words: stars: individual: β Pictoris / circumstellar matter / planetary systems: formation / protoplanetary disks / ISM: dust, extinction
© ESO, 2003
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