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HST/ACS Multiband Coronagraphic Imaging of the Debris Disk around Beta Pictoris | | D. A. Golimowski
; D. R. Ardila
; J. E. Krist
; M. Clampin
; H. C. Ford
; G. D. Illingworth
; F. Bartko
; N. Benitez
; J. P. Blakeslee
; R. J. Bouwens
; L. D. Bradley
; T. J. Broadhurst
; R. A. Brown
; C. J. Burrows
; E. S. Cheng
; N. J. G. Cross
; R. Demarco
; P. D. Feldman
; M. Franx
; T. Goto
; C. Gronwall
; G. F. Hartig
; B. P. Holden
; N. L. Homeier
; L. Infante
; M. J. Jee
; R. A. Kimble
; M. P. Lesser
; A. R. Martel
; S. Mei
; F. Menanteau
; G. R. Meurer
; G. K. Miley
; V. Motta
; M. Postman
; P. Rosati
; M. Sirianni
; W. B. Sparks
; H. D. Tran
; Z. I. Tsvetanov
; R. L. White
; W. Zheng
; A. W. Zirm
; | | Date: |
14 Feb 2006 | | Abstract: | (Abridged.) We present F435W (B), F606W (Broad V), and F814W (Broad I) coronagraphic images of the debris disk around Beta Pictoris obtained with HST’s Advanced Camera for Surveys. We confirm that the previously reported warp in the inner disk is a distinct secondary disk inclined by ~5 deg from the main disk. The main disk’s northeast extension is linear from 80 to 250 AU, but the southwest extension is distinctly bowed with an amplitude of ~1 AU over the same region. Both extensions of the secondary disk appear linear, but not collinear, from 80 to 150 AU. Within ~120 AU of the star, the main disk is ~50% thinner than previously reported. The surface-brightness profiles along the spine of the main disk are fitted with four distinct radial power laws between 40 and 250 AU, while those of the secondary disk between 80 and 150 AU are fitted with single power laws. These discrepancies suggest that the two disks have different grain compositions or size distributions. The F606W/F435W and F814W/F435W flux ratios of the composite disk are nonuniform and asymmetric about both projected axes of the disk. Within ~120 AU, the m_F435W-m_F606W and m_F435W-m_F814W colors along the spine of the main disk are ~10% and ~20% redder, respectively, than those of Beta Pic. These colors increasingly redden beyond ~120 AU, becoming 25% and 40% redder, respectively, than the star at 250 AU. We compare the observed red colors within ~120 AU with the simulated colors of non-icy grains having a radial number density ~r^-3 and different compositions, porosities, and minimum grain sizes. The observed colors are consistent with those of compact or moderately porous grains of astronomical silicate and/or graphite with sizes >0.15-0.20 um, but the colors are inconsistent with the blue colors expected from grains with porosities >90%. | | Source: | arXiv, astro-ph/0602292 | | Services: | Forum | Review | PDF | Favorites | |
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