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The Vega debris disc: A view from Herschel

B. Sibthorpe ; B. Vandenbussche ; J. S. Greaves ; E. Pantin ; G. Olofsson ; B. Acke ; M. J. Barlow ; Jadl Blommaert ; J. Bouwman ; A. Brandeker ; M. Cohen ; W. De Meester ; W. R. F. Dent ; J. Di Francesco ; C. Dominik ; M. Fridlund ; W. K. Gear ; A. M. Glauser ; H. L. Gomez ; P. C. Hargrave ; P. M. Harvey ; T. Henning ; A. M. Heras ; M. R. Hogerheijde ; W. S. Holland ; R. J. Ivison ; S. J. Leeks ; T. L. Lim ; René Liseau (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; B. C. Matthews ; D. A. Naylor ; G. L. Pilbratt ; E. T. Polehampton ; S. Regibo ; P. Royer ; A. Sicilia-Aguilar ; B. M. Swinyard ; C. Waelkens ; H. J. Walker ; R. Wesson
Astronomy & Astrophysics (0004-6361). Vol. 518 (2010), Article Number: L130,
[Artikel, refereegranskad vetenskaplig]

We present five band imaging of the Vega debris disc obtained using the Herschel Space Observatory. These data span a wavelength range of 70-500 mu m with full-width half-maximum angular resolutions of 5.6-36.9 ''. The disc is well resolved in all bands, with the ring structure visible at 70 and 160 mu m. Radial profiles of the disc surface brightness are produced, and a disc radius of 11 '' (similar to 85AU) is determined. The disc is seen to have a smooth structure thoughout the entire wavelength range, suggesting that the disc is in a steady state, rather than being an ephemeral structure caused by the recent collision of two large planetesimals.

Nyckelord: stars: individual: Vega, instrumentation: photometers, methods:, observational, dust, evolution, mission, spitzer, images, stars



Denna post skapades 2010-12-08. Senast ändrad 2011-03-30.
CPL Pubid: 130349

 

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