/ftp/cats/A+A/591/A108



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J/A+A/591/A108      HD61005 SPHERE H and Ks images            (Olofsson+, 2016)
The following files can be converted to FITS (extension .fit or fit.gz)
	list.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/591/A108
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Beginning of ReadMe : J/A+A/591/A108 HD61005 SPHERE H and Ks images (Olofsson+, 2016) ================================================================================ Azimuthal asymmetries in the debris disk around HD61005. A massive collision of planetesimals? Olofsson J., Samland M., Avenhaus H., Caceres C., Henning T., Moor A., Milli J., Canovas H., Quanz S. P., Schreiber M. R., Augereau J.-C., Bayo A., Bazzon A., Beuzit J.-L., Boccaletti A., Buenzli E., Casassus S., Chauvin G., Dominik C., Desidera S., Feldt M., Gratton R., Janson M., Lagrange A.-M., Langlois M., Lannier J., Maire A.-L., Mesa D., Pinte C., Rouan D., Salter G., Thalmann C., Vigan A. <Astron. Astrophys. 591, A108 (2016)> =2016A&A...591A.108O (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: YSOs ; Morphology ; Polarization Keywords: circumstellar matter - zodiacal dust - techniques: high angular resolution Abstract: Debris disks offer valuable insights into the latest stages of circumstellar disk evolution, and can possibly help us to trace the outcomes of planetary formation processes. In the age range 10 to 100Myr, most of the gas is expected to have been removed from the system, giant planets (if any) must have already been formed, and the formation of terrestrial planets may be on-going. Pluto-sized planetesimals, and their debris released in a collisional cascade, are under their mutual gravitational influence, which may result into non-axisymmetric structures in the debris disk. Here we present new VLT/SPHERE and ALMA observations of the debris disk around the 40Myr-old solar-type star HD61005. We resolve the disk at unprecedented resolution both in the near-infrared (in scattered and polarized light) and at millimeter wavelengths. We perform a detailed modeling of these observations, including the spectral energy distribution. Thanks to the new observations, we propose a solution for both the radial and azimuthal distribution of the dust grains in the debris disk. We find that the disk has a moderate eccentricity and that the dust density is two times larger at the pericenter compared to the apocenter. With no giant planets detected in our observations, we investigate alternative explanations besides planet-disk interactions to interpret the inferred disk morphology. We postulate that the morphology of the disk could be the consequence of a massive collision between 1000km-sized bodies at 61 au. If this interpretation holds, it would put stringent constraints on the formation of massive planetesimals at large distances from the star. Description: The fits files contains the reduced ADI and DPI SPHERE observations used to produce Fig. 1 of the paper. Besides the primary card, the files consists of 6 additional ImageHDU. The first and second one contain the SPHERE IRDIS ADI H band observations and the noise map. The third and fourth contain the SPHERE IRDIS ADI Ks band observations and the corresponding noise map. Finally, the fifth and sixth ImageHDU contain the SPHERE IRDIS DPI H band data as well as the noise map. Each ADI image has 1024x1024 pixels, while the DPI images have 1800x1800 pixels. The header of the primary card contains the pixel sizes for each datasets and the wavelengths of the H and K band observations. Objects: -------------------------------------------------- RA (2000) DE Designation(s) -------------------------------------------------- 07 35 47.46 -32 12 14.0 HD 61005 = HIP 36948 --------------------------------------------------