Hubble Space Telescope Advanced Camera for Surveys coronagraphic imaging of the AU Microscopii debris disk

John E. Krist, D. R. Ardila, D. A. Golimowski, M. Clampin, H. C. Ford, G. D. Illingworth, G. F. Hartig, F. Bartko, N. Benítez, 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 & 21 others T. Goto, C. Gronwall, B. Holden, N. Homeier, L. Infante, 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, Zlatan Tsvetanov, R. L. White, W. Zheng

Research output: Contribution to journalArticle

103 Citations (Scopus)

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.

Original languageEnglish
Pages (from-to)1008-1017
Number of pages10
JournalAstronomical Journal
Volume129
Issue number2
DOIs
Publication statusPublished - Feb 2005
Externally publishedYes

Fingerprint

Hubble Space Telescope
debris
cameras
three-dimensional modeling
stars
scattering
dust
prediction
energy
radiation pressure
forward scattering
bows
spectral energy distribution
line of sight
inclination
brightness
low pressure
time measurement
galaxies
color

Keywords

  • Circumstellar matter
  • Stars: individual (AU Microscopii)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Krist, J. E., Ardila, D. R., Golimowski, D. A., Clampin, M., Ford, H. C., Illingworth, G. D., ... Zheng, W. (2005). Hubble Space Telescope Advanced Camera for Surveys coronagraphic imaging of the AU Microscopii debris disk. Astronomical Journal, 129(2), 1008-1017. https://doi.org/10.1086/426755

Hubble Space Telescope Advanced Camera for Surveys coronagraphic imaging of the AU Microscopii debris disk. / 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, Zlatan; White, R. L.; Zheng, W.

In: Astronomical Journal, Vol. 129, No. 2, 02.2005, p. 1008-1017.

Research output: Contribution to journalArticle

Krist, JE, Ardila, DR, Golimowski, DA, Clampin, M, Ford, HC, Illingworth, GD, Hartig, GF, Bartko, F, Benítez, N, Blakeslee, JP, Bouwens, RJ, Bradley, LD, Broadhurst, TJ, Brown, RA, Burrows, CJ, Cheng, ES, Cross, NJG, Demarco, R, Feldman, PD, Franx, M, Goto, T, Gronwall, C, Holden, B, Homeier, N, Infante, L, Kimble, RA, Lesser, MP, Martel, AR, Mei, S, Menanteau, F, Meurer, GR, Miley, GK, Motta, V, Postman, M, Rosati, P, Sirianni, M, Sparks, WB, Tran, HD, Tsvetanov, Z, White, RL & Zheng, W 2005, 'Hubble Space Telescope Advanced Camera for Surveys coronagraphic imaging of the AU Microscopii debris disk', Astronomical Journal, vol. 129, no. 2, pp. 1008-1017. https://doi.org/10.1086/426755
Krist JE, Ardila DR, Golimowski DA, Clampin M, Ford HC, Illingworth GD et al. Hubble Space Telescope Advanced Camera for Surveys coronagraphic imaging of the AU Microscopii debris disk. Astronomical Journal. 2005 Feb;129(2):1008-1017. https://doi.org/10.1086/426755
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, Zlatan ; White, R. L. ; Zheng, W. / Hubble Space Telescope Advanced Camera for Surveys coronagraphic imaging of the AU Microscopii debris disk. In: Astronomical Journal. 2005 ; Vol. 129, No. 2. pp. 1008-1017.
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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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AU - Krist, John E.

AU - Ardila, D. R.

AU - Golimowski, D. A.

AU - Clampin, M.

AU - Ford, H. C.

AU - Illingworth, G. D.

AU - Hartig, G. F.

AU - Bartko, F.

AU - Benítez, N.

AU - Blakeslee, J. P.

AU - Bouwens, R. J.

AU - Bradley, L. D.

AU - Broadhurst, T. J.

AU - Brown, R. A.

AU - Burrows, C. J.

AU - Cheng, E. S.

AU - Cross, N. J G

AU - Demarco, R.

AU - Feldman, P. D.

AU - Franx, M.

AU - Goto, T.

AU - Gronwall, C.

AU - Holden, B.

AU - Homeier, N.

AU - Infante, L.

AU - Kimble, R. A.

AU - Lesser, M. P.

AU - Martel, A. R.

AU - Mei, S.

AU - Menanteau, F.

AU - Meurer, G. R.

AU - Miley, G. K.

AU - Motta, V.

AU - Postman, M.

AU - Rosati, P.

AU - Sirianni, M.

AU - Sparks, W. B.

AU - Tran, H. D.

AU - Tsvetanov, Zlatan

AU - White, R. L.

AU - Zheng, W.

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N2 - 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.

AB - 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.

KW - Circumstellar matter

KW - Stars: individual (AU Microscopii)

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