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  Spatially resolved spectroscopy of the debris disk HD 32297. Further evidence of small dust grains

Bhowmik, T., Boccaletti, A., Thébault, P., Kral, Q., Mazoyer, J., Milli, J., et al. (2019). Spatially resolved spectroscopy of the debris disk HD 32297. Further evidence of small dust grains. Astronomy and Astrophysics, 630.

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Bhowmik, T.1, Author
Boccaletti, A.1, Author
Thébault, P.1, Author
Kral, Q.1, Author
Mazoyer, J.1, Author
Milli, J.1, Author
Maire, A. L.1, Author
van Holstein, R. G.1, Author
Augereau, J. -C.1, Author
Baudoz, P.1, Author
Feldt, M.1, Author
Galicher, R.1, Author
Henning, T.1, Author
Lagrange, A. -M.1, Author
Olofsson, J.1, Author
Pantin, E.1, Author
Perrot, C.1, Author
Affiliations:
1Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners, ou_2421692              

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Free keywords: techniques: image processing stars: individual: HD 32297 techniques: high angular resolution methods: data analysis infrared: planetary systems
 Abstract: Context. Spectro-photometry of debris disks in total intensity and polarimetry can provide new insight into the properties of the dust grains therein (size distribution and optical properties). <BR /> Aims: We aim to constrain the morphology of the highly inclined debris disk HD 32297. We also intend to obtain spectroscopic and polarimetric measurements to retrieve information on the particle size distribution within the disk for certain grain compositions. <BR /> Methods: We observed HD 32297 with SPHERE in Y, J, and H bands in total intensity and in J band in polarimetry. The observations are compared to synthetic models of debris disks and we developed methods to extract the photometry in total intensity overcoming the data-reduction artifacts, namely the self-subtraction. The spectro-photometric measurements averaged along the disk mid-plane are then compared to model spectra of various grain compositions. <BR /> Results: These new images reveal the very inner part of the system as close as 0.15″. The disk image is mostly dominated by the forward scattering making one side (half- ellipse) of the disk more visible, but observations in total intensity are deep enough to also detect the back side for the very first time. The images as well as the surface brightness profiles of the disk rule out the presence of a gap as previously proposed. We do not detect any significant asymmetry between the northeast and southwest sides of the disk. The spectral reflectance features a "gray to blue" color which is interpreted as the presence of grains far below the blowout size. <BR /> Conclusions: The presence of sub-micron grains in the disk is suspected to be the result of gas drag and/or "avalanche mechanisms". The blue color of the disk could be further investigated with additional total intensity and polarimetric observations in K and H bands respectively to confirm the spectral slope and the fraction of polarization. Reduced images are also available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz- bin/cat/J/A+A/630/A85">http://cdsarc.u-strasbg.fr/viz- bin/cat/J/A+A/630/A85</A>Based on data collected at the European Southern Observatory, Chile under the programs 098.C-0686(A) and 098.C-0686(B).

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 Dates: 2019
 Publication Status: Published in print
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Title: Astronomy and Astrophysics
Source Genre: Journal
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Pages: - Volume / Issue: 630 Sequence Number: - Start / End Page: - Identifier: -