The Vega debris disc: A view from Herschel

B. Sibthorpe*, B. Vandenbussche, J. S. Greaves, E. Pantin, G. Olofsson, B. Acke, M. J. Barlow, J. A. D. L. 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. HargraveP. M. Harvey, Th. Henning, A. M. Heras, M. R. Hogerheijde, W. S. Holland, R. J. Ivison, S. J. Leeks, T. L. Lim, R. Liseau, 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

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

39 Citations (Scopus)


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.

Original languageEnglish
Article numberL130
Number of pages5
JournalAstronomy & Astrophysics
Publication statusPublished - Jul 2010


  • stars: individual: Vega
  • instrumentation: photometers
  • methods: observational
  • DUST


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