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Published September 2011 | Published
Journal Article Open

Multi-wavelength modeling of the spatially resolved debris disk of HD 107146


Aims. We aim to constrain the location, composition, and dynamical state of planetesimal populations and dust around the young, sun-like (G2 V) star HD 107146. Methods. We consider coronagraphic observations obtained with the Advanced Camera for Surveys (HST/ACS) onboard the Hubble Space Telescope (HST) in broad V (λ_c ≈ 0.6 μm) and broad I (λ_c ≈ 0.8 μm) filters, a resolved 1.3 mm map obtained with the Combined Array for Research in Millimeter-wave Astronomy (CARMA), Spitzer/IRS low resolution spectra in the range of 7.6 μm to 37.0 μm, and the spectral energy distribution (SED) of the object at wavelengths ranging from 3.5 μm to 3.1 mm. We complement these data with new coronagraphic high resolution observations of the debris disk using the Near Infrared Camera and Multi-Object Spectrometer (HST/NICMOS) aboard the HST in the F110W filter (λ_c ≈ 1.1 μm). The SED and images of the disk in scattered light as well as in thermal reemission are combined in our modeling using a parameterized model for the disk density distribution and optical properties of the dust. Results. A detailed analytical model of the debris disk around HD 107146 is presented that allows us to reproduce the almost entire set of spatially resolved and unresolved multi-wavelength observations. Considering the variety of complementary observational data, we are able to break the degeneracies produced by modeling SED data alone. We find the disk to be an extended ring with a peak surface density at 131 AU. Furthermore, we find evidence for an additional, inner disk probably composed of small grains released at the inner edge of the outer disk and moving inwards due to Poynting-Robertson drag. A birth ring scenario (i.e., a more or less broad ring of planetesimals creating the dust disk trough collisions) is found to be the most likely explanation of the ringlike shape of the disk.

Additional Information

© 2011 ESO. Received 12 October 2010. Accepted 1 July 2011. Published online 15 September 2011. This work is based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program # 10177. Support for program # 10177 was provided by NASA through a grant from the Space Telescope science Institute. This work is also based in part on observations made with the Spitzer Space Telescope, which is operated by JPL/Caltech under NASA contract 1407. These observations are associated with the Spitzer Legacy Science Program FEPS, which is supported through NASA contracts 1224768, 1224634, and 1224566 administered through JPL. We thank all members of the FEPS team for their contributions to this effort. We would also like to particularly thank David Ardila for providing the HST/ACS data which represent the basis for the recent work, and Andrea Isella for producing the model subtracted images of the CARMA data. S.E. thanks for financial support from DFG under contract WO857/7-1.

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