Optical polarised phase function of the HR 4796A dust ring

Milli, J.; Engler, N.; Schmid, Hans Martin; Olofsson, J.; Ménard, F.; Kral, Quentin; Boccaletti, A.; Thébault, P.; Choquet, Élodie; Mouillet, D.; Lagrange, Anne-Marie; Augereau, J.-C.; Pinte, C.; Chauvin, G.; Dominik, C.; Perrot, C.; Zurlo, A.; Henning, Thomas; Beuzit, Jean-Luc; Avenhaus, H.; Bazzon, A.; Moulin, T.; Llored, M.; Moeller-Nilsson, O.; Roelfsema, R.; Pragt, J.

doi:10.1051/0004-6361/201935363

Cited by 64 publications

(129 citation statements)

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“…Therefore, the dust grains which are probed in these data are more prone to forward scattering in polarimetry. It should be noted that in the case of strong forward scattering, the polarised phase function peaks at a smaller scattering angle as well as at the ansae (Milli et al 2019), which is visible in our best-fit model as seen in Fig. 7.…”

Section: Modeling Polarimetric Imagessupporting

confidence: 58%

Spatially resolved spectroscopy of the debris disk HD 32297

Bhowmik

Boccaletti

Thébault

et al. 2019

A&A

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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). 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. 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. 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. 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.

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Section: Modeling Polarimetric Imagessupporting

confidence: 58%

Spatially resolved spectroscopy of the debris disk HD 32297

Bhowmik

Boccaletti

Thébault

et al. 2019

A&A

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“…We note that the above parameter values are based only on MCMC fitting results, and neither may be correct given the limitation of DHS or Mie models. Specifically, these models are optimized for spectral fitting (e.g., Min et al 2007;Poteet et al 2015), but neither model is able to properly constrain the composition from scattered-light images (e.g., Milli et al 2019). See Section 5.2 for more discussion on the dust properties retrieved from radiative transfer modeling.…”

Section: Discussionmentioning

confidence: 99%

“…The halo is likely both more forward-and backward-scattering in the probed scattering angles. previous measurements (e.g., Perrin et al 2014;Frattin et al 2019;Milli et al 2019). To better constrain the polarized fraction values, we need H-band total intensity observations to rule out the wavelength-dependent effect.…”

Section: Spfmentioning

confidence: 99%

“…They are expected to be the result of the grinding down of larger dust (Wyatt 2008); however, the diversity in observables such as morphology and surface brightness suggests that they are shaped by a variety of mechanisms (e.g., Artymowicz & Clampin 1997;Stark et al 2014;Lee & Chiang 2016). Imaging studies of debris disks in scattered light use not only space-based instruments (e.g., the Space Telescope Imaging Spectrograph (STIS): Schneider et al 2009Schneider et al , 2014Schneider et al , 2016Schneider et al , 2018Konishi et al 2016;NICMOS: Soummer et al 2014;Choquet et al 2016Choquet et al , 2017Choquet et al , 2018 that offer the best telescope stability but also extreme adaptive optics-equipped ground-based instruments (e.g., GPI: Hung et al 2015;Kalas et al 2015;Millar-Blanchaer et al 2015Perrin et al 2015;Draper et al 2016;Esposito et al 2018;SPHERE: Boccaletti et al 2015;Lagrange et al 2016;Wahhaj et al 2016;Engler et al 2017;Feldt et al 2017;Matthews et al 2017;Milli et al 2017Milli et al , 2019Sissa et al 2018;Olofsson et al 2018) that provide the best angular resolution and probe closer-in regions of the disks.…”

Section: Introductionmentioning

confidence: 99%

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An Exo–Kuiper Belt with an Extended Halo around HD 191089 in Scattered Light

Ren

Choquet

Perrin

et al. 2019

ApJ

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“…Right: Image of the debris disk around HR4796, obtained with VLT/SPHERE in the optical (600-900 nm) in linearly polarized light (North is up, East to the right). Adapted fromMilli et al (2019).…”

mentioning

confidence: 99%

Linking studies of tiny meteoroids, zodiacal dust, cometary dust and circumstellar disks

Levasseur-Regourd

Lasue

Milli

et al. 2020

Planetary and Space Science

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Tiny meteoroids entering the Earth's atmosphere and inducing meteor showers have long been thought to originate partly from cometary dust. Together with other dust particles, they form a huge cloud around the Sun, the zodiacal cloud. From our previous studies of the zodiacal light, as well as other independent methods (dynamical studies, infrared observations, data related to Earth's environment), it is now established that a significant fraction of dust particles entering the Earth's atmosphere comes from Jupiterfamily comets (JFCs).This paper relies on our understanding of key properties of the zodiacal cloud and of comet 67P/Churyumov-Gerasimenko, extensively studied by the Rosetta mission to a JFC. The interpretation, through numerical and experimental simulations of zodiacal light local polarimetric phase curves, has recently allowed us to establish that interplanetary dust is rich in absorbing organics and consists of fluffy particles. The ground-truth provided by Rosetta presently establishes that the cometary dust particles are rich in organic compounds and consist of quite fluffy and irregular aggregates. Our aims are as follows: (1) to make links, back in time, between peculiar micrometeorites, tiny meteoroids, interplanetary dust particles, cometary dust particles, and the early evolution of the Solar System, and (2) to show how detailed studies of such meteoroids and of cometary dust particles can improve the interpretation of observations of dust in protoplanetary and debris disks. Future modeling of dust in such disks should favor irregular porous particles instead of more conventional compact spherical particles.

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Optical polarised phase function of the HR 4796A dust ring

Cited by 64 publications

References 59 publications

Spatially resolved spectroscopy of the debris disk HD 32297

Spatially resolved spectroscopy of the debris disk HD 32297

An Exo–Kuiper Belt with an Extended Halo around HD 191089 in Scattered Light

Linking studies of tiny meteoroids, zodiacal dust, cometary dust and circumstellar disks

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