Two cold belts in the debris disk around the G-type star NZ Lupi

Boccaletti, A.; Thébault, P.; Pawellek, N.; Lagrange, A.-M.; Galicher, R.; Desidera, S.; Milli, J.; Kral, Quentin; Bonnefoy, M.; Augereau, J.-C.; Maire, Anne-Lise; Henning, Th.; Beust, H.; Rodet, L.; Avenhaus, H.; Bhowmik, T.; Bonavita, M.; Chauvin, G.; Cheetham, A.; Cudel, M.; Feldt, M.; Gratton, R.; Hagelberg, J.; Janin-Potiron, Pierre; Langlois, M.; Ménard, F.; Mesa, D.; Meyer, Michael; Peretti, S.; Perrot, C.; Schmidt, T. O. B.; Sissa, E.; Vigan, A.; Rickman, E. L.; Magnard, Y.; Maurel, D.; Moeller-Nilsson, O.; Perret, D.; Sauvage, J.-F.

doi:10.1051/0004-6361/201935135

Cited by 18 publications

(17 citation statements)

References 75 publications

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“…Doing so, we predict the per-pixel contrast would be roughly at the 1σlevel (∼10 −7 ) in our f  image, likely explaining the lack of a significant detection. No polarized intensity detection has yet been published for NZ Lup's disk, although Boccaletti et al (2019) presented additional total intensity images, so we can only speculate that the disk's polarized signal is fainter than our achieved sensitivity.…”

Section: Nondetectionsmentioning

confidence: 67%

“…b HD 141569 radii are for the inner ring only (as seen in the GPI images) and the millimeter uncertainties are ∼95% confidence intervals. c NZ Lup's R in is for the inner belt only and R 0 is the mean of both belts (with the uncertainty spanning the range of their individual R 0 values) in the two-belt "gap" model from Boccaletti et al (2019). quantity cannot be measured from GPI data.…”

Section: Sample-wide Results On Debris Disk Propertiesmentioning

confidence: 99%

“…Several special cases are worth noting. For NZ Lup, we aim to represent the entire disk by taking R 0 as the mean of both belts (with individual R 0 values of 86 and 121 au) in the two-belt "gap" model by Boccaletti et al (2019). For HD143675, our MCMC only determined a lower limit for the dust density critical radius r c , so we assumed R 0 to be the average of the better constrained r in and r out .…”

Section: Disk Radiimentioning

confidence: 99%

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Debris Disk Results from the Gemini Planet Imager Exoplanet Survey's Polarimetric Imaging Campaign

Espósito

Kalas

Fitzgerald

et al. 2020

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We report the results of a ∼4 yr direct imaging survey of 104 stars to resolve and characterize circumstellar debris disks in scattered light as part of the Gemini Planet Imager (GPI) Exoplanet Survey. We targeted nearby (150 pc), young (500 Myr) stars with high infrared (IR) excesses (L IR /L å >10 −5), including 38 with previously resolved disks. Observations were made using the GPI high-contrast integral field spectrograph in H-band (1.6 μm) coronagraphic polarimetry mode to measure both polarized and total intensities. We resolved 26 debris disks and 3 protoplanetary/transitional disks. Seven debris disks were resolved in scattered light for the first time, including newly presented HD117214 and HD156623, and we quantified basic morphologies of five of them using radiative transfer models. All of our detected debris disks except HD156623 have dust-poor inner holes, and their scattered-light radii are generally larger than corresponding radii measured from resolved thermal emission and

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Section: Nondetectionsmentioning

confidence: 67%

Section: Sample-wide Results On Debris Disk Propertiesmentioning

confidence: 99%

Section: Disk Radiimentioning

confidence: 99%

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Debris Disk Results from the Gemini Planet Imager Exoplanet Survey's Polarimetric Imaging Campaign

Espósito

Kalas

Fitzgerald

et al. 2020

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“…A comparison between the science image and the noiseless model masked with an effective aperture is credible as the disk has high S/N assuming that there is no over-subtraction due to the combination of noise and disk. Also, in Boccaletti et al (2019) a comparison between forward modeling with noiseless models and the injected model into the science image at a different PA with a certain flux resulted in similar χ 2 values. Therefore, we refrain from doing the latter due to reduced computational momentum.…”

Section: Modeling Total Intensity With a Single Phase Functionmentioning

confidence: 82%

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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“…In this way, planets can create wide empty gaps in dusty disks and shape them into ring structures. This scenario for the evolution of a planetary system provides one possible explanation for the multiple concentric rings observed in protoplanetary disks (e.g., Andrews et al 2018) and debris disks (Golimowski et al 2011;Perrot et al 2016;Feldt et al 2017;Bonnefoy et al 2017;Marino et al 2018;Engler et al 2019;Boccaletti et al Based on data collected at the European Southern Observatory, Chile under program 1100.C-0481. 2019).…”

Section: Introductionmentioning

confidence: 99%

HD 117214 debris disk: scattered-light images and constraints on the presence of planets

Engler

Lazzoni

Gratton

et al. 2020

A&A

Self Cite

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Context. Young stars with debris disks are the most promising targets for an exoplanet search because debris indicate a successful formation of planetary bodies. Debris disks can be shaped by planets into ring structures that give valuable indications on the presence and location of planets in the disk. Aims. We performed observations of the Sco-Cen F star HD 117214 to search for planetary companions and to characterize the debris disk structure. Methods. HD 117214 was observed with the SPHERE subsystems IRDIS, IFS, and ZIMPOL at optical and near-IR wavelengths using angular and polarimetric differential imaging techniques. This provided the first images of scattered light from the debris disk with the highest spatial resolution of 25 mas and the inner working angle < 0.1 . With the observations with IRDIS and IFS we derived detection limits for substellar companions. The geometrical parameters of the detected disk were constrained by fitting 3D models for the scattering of an optically thin dust disk. Investigating the possible origin of the disk gap, we introduced putative planets therein and modeled the planet-disk and planet-planet dynamical interactions. The obtained planetary architectures were compared with the detection limit curves.Results. The debris disk has an axisymmetric ring structure with a radius of 0.42(±0.01) or ∼45 au and an inclination of 71(±2.5) • and exhibits a 0.4 (∼40 au) wide inner cavity. From the polarimetric data, we derive a polarized flux contrast for the disk of (F pol ) disk /F * > (3.1 ± 1.2) · 10 −4 in the RI band. Conclusions. The fractional scattered polarized flux of the disk is eight times lower than the fractional IR flux excess. This ratio is similar to the one obtained for the debris disk HIP 79977, indicating that dust radiation properties are similar for these two disks. Inside the disk cavity we achieve high-sensitivity limits on planetary companions with a mass down to ∼ 4 M J at projected radial separations between 0.2 and 0.4 . We can exclude stellar companions at a radial separation larger than 75 mas from the star.

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Two cold belts in the debris disk around the G-type star NZ Lupi

Cited by 18 publications

References 75 publications

Debris Disk Results from the Gemini Planet Imager Exoplanet Survey's Polarimetric Imaging Campaign

Debris Disk Results from the Gemini Planet Imager Exoplanet Survey's Polarimetric Imaging Campaign

Spatially resolved spectroscopy of the debris disk HD 32297

HD 117214 debris disk: scattered-light images and constraints on the presence of planets

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