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C.A. Grady (NOAO/STIS, GSFC), E. Polomski (U. Minn. and U. Florida), Th. Henning (AIU, Jena, Germany), B. Stecklum (Thuringer Landessternwarte Tautenberg, Germany), B. Woodgate (LASP, NASA's GSFC), C. Telesco, R. Pina (U. Florida), P. Plait (ACC, GSFC), T. Gull (LASP, NASA's GSFC), A. Boggess (CUA), C. Bowers (LASP, NASA's GSFC), F.C. Bruhweiler (CUA), M. Clampin (STScI), A. Danks (Raytheon PSC, GSFC), R.F. Green (NOAO), S.R. Heap (LASP, NASA's GSFC), J.B. Hutchings (DAO), E. Jenkins (Princeton University Observatory), M. Kaiser (JHU), R. Kimble (LASP, NASA's GSFC), S. Kraemer (CUA), D. Lindler (ACC, GSFC), J.L. Linsky (JILA, U. Colorado and NIST), S.P. Maran (NASA's GSFC), H.W. Moos (JHU), F. Roesler (U. Wisconsin), J.G. Timothy (Nightsen, Inc.), D. Weistrop (UNLV)
We present coronagraphic imaging of the nearest Herbig Be star with the Space Telescope Imaging Spectrograph on board HST, K-short imaging with ADONIS from the 3.6m telescope at La Silla, and mid-IR imaging with OSCIR using the 4m telescope at CTIO. We confirm the disk detection reported by Pantin et al. (2000). The brightest material associated with the disk is located within 3.5" (365 AU) of the star, but disk material can be traced to 5" (515 AU) based on the surface brightness distribution. Spiral dark lanes are seen beyond 200 AU. HD 100546 is accompanied by a diffuse envelope which is more highly flared than the disk and which extends 10" (1000 AU) from the star. Far from the star, a band of nebulosity running from NNW to SSE is seen, compatible with the orientation of filaments in DC 292.6-7.9 (Vieira et al. 1999). Closer to the star, the bands are bowed out to the W and WSW, in the direction of HD 100546's proper motion. The OSCIR images show that the source is slightly extended at 11.7 microns, but unresolved at 10 and 18 microns. The mid-IR color temperatures are consistent with central clearing of the disk, supporting the inference of Pantin et al. (2000).
This study is based on observations made with HST, and at ESO and CTIO. Funding was provided by NASA GTO funding to the STIS Science Team in response to NASA A/O OSSA -4-84 through the HST Project at GSFC, and through interagency transfer of funds to NOAO.
The author(s) of this abstract have provided an email address for comments about the abstract: cgrady@echelle.gsfc.nasa.gov