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Title:
Hubble Space Telescope Advanced Camera for Surveys Coronagraphic Imaging of the AU Microscopii Debris Disk
Authors:
Krist, John E.; Ardila, D. R.; Golimowski, D. A.; Clampin, M.; Ford, H. C.; Illingworth, G. D.; Hartig, G. F.; Bartko, F.; Benítez, N.; Blakeslee, J. P.; Bouwens, R. J.; Bradley, L. D.; Broadhurst, T. J.; Brown, R. A.; Burrows, C. J.; Cheng, E. S.; Cross, N. J. G.; Demarco, R.; Feldman, P. D.; Franx, M.; Goto, T.; Gronwall, C.; Holden, B.; Homeier, N.; Infante, L.; Kimble, R. A.; Lesser, M. P.; Martel, A. R.; Mei, S.; Menanteau, F.; Meurer, G. R.; Miley, G. K.; Motta, V.; Postman, M.; Rosati, P.; Sirianni, M.; Sparks, W. B.; Tran, H. D.; Tsvetanov, Z. I.; White, R. L.; Zheng, W.
Affiliation:
AA(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AB(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AC(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AD(NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771.), AE(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AF(UCO/Lick Observatory, University of California, Santa Cruz, CA 95064.), AG(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AH(Bartko Science and Technology, 14520 Akron Street, Brighton, CO 80602.), AI(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AJ(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AK(UCO/Lick Observatory, University of California, Santa Cruz, CA 95064.), AL(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AM(Racah Institute of Physics, Hebrew University, Jerusalem 91904, Israel.), AN(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AO(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AP(Conceptual Analytics, LLC, 8209 Woburn Abbey Road, Glenn Dale, MD 20769.), AQ(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AR(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AS(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AT(Leiden Observatory, Postbus 9513, NL-2300 RA Leiden, Netherlands.), AU(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AV(Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802.), AW(UCO/Lick Observatory, University of California, Santa Cruz, CA 95064.), AX(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), AY(Departmento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile.), AZ(NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771.), BA(Steward Observatory, University of Arizona, Tucson, AZ 85721.), BB(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BC(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BD(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BE(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BF(Leiden Observatory, Postbus 9513, NL-2300 RA Leiden, Netherlands.), BG(Departmento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile.), BH(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), BI(European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany.), BJ(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BK(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), BL(W. M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, HI 96743.), BM(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.), BN(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), BO(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218.)
Publication:
The Astronomical Journal, Volume 129, Issue 2, pp. 1008-1017. (AJ Homepage)
Publication Date:
02/2005
Origin:
UCP
AJ Keywords:
Stars: Circumstellar Matter, Stars: Individual: Constellation Name: AU Microscopii
DOI:
10.1086/426755
Bibliographic Code:
2005AJ....129.1008K

Abstract

We present Hubble Space Telescope Advanced Camera for Surveys multicolor coronagraphic images of the recently discovered edge-on debris disk around the nearby (~10 pc) M dwarf AU Microscopii. The disk is seen between r=0.75" and 15" (7.5-150 AU) from the star. It has a thin midplane with a projected FWHM thickness of 2.5-3.5 AU within r<50 AU of the star that increases to 6.5-9 AU at r~75 AU. The disk's radial brightness profile is generally flat for r<15 AU, then decreases gradually (I~r-1.8) out to r~43 AU, beyond which it falls rapidly (I~r-4.7). Within 50 AU the midplane is straight and aligned with the star, and beyond that it deviates by ~3°, resulting in a bowed appearance that was also seen in ground-based images. Three-dimensional modeling of the disk shows that the inner region (r<50 AU) is inclined to the line of sight by less than 1° and the outer disk by ~3°. The inclination of the outer disk and moderate forward scattering (g~0.4) can explain the apparent bow. The intrinsic, deprojected FWHM thickness is 1.5-10 AU, increasing with radius. The models indicate that the disk is clear of dust within ~12 AU of the star, in general agreement with the previous prediction of 17 AU based on the infrared spectral energy distribution. The disk is blue, being 60% brighter at B than I relative to the star. One possible explanation for this is that there is a surplus of very small grains compared with other imaged debris disks that have more neutral or red colors. This may be due to the low radiation pressure exerted by the late-type star. Observations at two epochs show that an extended source seen along the midplane is a background galaxy.
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