Belt(s) of debris resolved around the Sco-Cen star HIP 67497

Bonnefoy, M.; Milli, J.; Ménard, F.; Vigan, A.; Lagrange, Anne-Marie; Delorme, P.; Boccaletti, A.; Lazzoni, C.; Galicher, R.; Desidera, S.; Chauvin, G.; Augereau, J.-C.; Mouillet, D.; Pinte, C.; Plas, G. van der; Gratton, R.; Beust, H.; Beuzit, J. L.

doi:10.1051/0004-6361/201628929

Cited by 38 publications

(47 citation statements)

References 69 publications

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“…However, the acceptable values of α in can be very broad when the mask size decreases, so it is difficult make conclusions from this first approach. The best inclination is about ∼ 85 − 86 • , the position of the planetesimal belt is at ∼ 90 − 95 au, and the asymmetric scattering factor is g ∼ 0.6 indicating a rather high value of forward scattering (but similar to other debris disks: Lagrange et al 2016;Olofsson et al 2016;Bonnefoy et al 2017). Regarding the scale height, both h = 0.01 and h = 0.02 fit equally well at least in the case of model mask1.…”

Section: One-belt Scenariomentioning

confidence: 78%

“…Planets, if already formed, are expected to produce indirect signatures in the form of a departure from a pure axisymmetrical disk morphology. Recently, the advance of high-contrast imaging, in particular with the installation of SPHERE (Spectro-Polarimetic High contrast imager for Exoplanets REsearch, Beuzit et al 2019) and GPI (Gemini Planet Imager, Macintosh et al 2008), has yielded a significant number of new discoveries in this field either revealing new disks (Lagrange et al 2016;Kalas et al 2015;Currie et al 2015;Bonnefoy et al 2017;Sissa et al 2018) or new structures in known disks (Boccaletti et al 2015;Perrin et al 2015;Garufi et al 2016;Perrot et al 2016;Milli et al 2017). These observations are definitely pointing to the presence of planets.…”

Section: Introductionmentioning

confidence: 99%

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

Boccaletti

Thébault

Pawellek

et al. 2019

A&A

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Context. Planetary systems hold the imprint of the formation and of the evolution of planets especially at young ages, and in particular at the stage when the gas has dissipated leaving mostly secondary dust grains. The dynamical perturbation of planets in the dust distribution can be revealed with high-contrast imaging in a variety of structures. Aims. SPHERE, the high-contrast imaging device installed at the VLT, was designed to search for young giant planets in long period, but is also able to resolve fine details of planetary systems at the scale of astronomical units in the scattered-light regime. As a young and nearby star, NZ Lup was observed in the course of the SPHERE survey. A debris disk had been formerly identified with HST/NICMOS. Methods. We observed this system in the near-infrared with the camera in narrow and broad band filters and with the integral field spectrograph. High contrasts are achieved by the mean of pupil tracking combined with angular differential imaging algorithms. Results. The high angular resolution provided by SPHERE allows us to reveal a new feature in the disk which is interpreted as a superimposition of two belts of planetesimals located at stellocentric distances of ∼85 and ∼115 au, and with a mutual inclination of about 5 • . Despite the very high inclination of the disk with respect to the line of sight, we conclude that the presence of a gap, that is, a void in the dust distribution between the belts, is likely. Conclusions. We discuss the implication of the existence of two belts and their relative inclination with respect to the presence of planets.

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Section: One-belt Scenariomentioning

confidence: 78%

Section: Introductionmentioning

confidence: 99%

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

Boccaletti

Thébault

Pawellek

et al. 2019

A&A

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“…Observable ringlike structures in such circumstellar debris disks seem to be a common feature (e.g., Bonnefoy et al 2017;Feldt et al 2017). The locations and surface brightness (SB) distributions of such rings may inform upon the architectures of these exoplanetary debris systems and offer constraints on planet masses and orbits even when the planets themselves remain undetected (e.g., Chiang et al 2009;Rodigas et al 2014;Thilliez & Maddison 2016).…”

Section: Introductionmentioning

confidence: 99%

The HR 4796A Debris System: Discovery of Extensive Exo-ring Dust Material

Schneider

Debes

Grady

et al. 2018

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The optically and IR-bright and starlight-scattering HR 4796A ringlike debris disk is one of the most-(and best-) studied exoplanetary debris systems. The presence of a yet-undetected planet has been inferred (or suggested) from the narrow width and inner/outer truncation radii of its r=1 05 (77 au) debris ring. We present new, highly sensitive Hubble Space Telescope (HST) visible-light images of the HR 4796A circumstellar debris system and its environment over a very wide range of stellocentric angles from 0 32 (23 au) to ≈15″ (1100 au). These very highcontrast images were obtained with the Space Telescope Imaging Spectrograph (STIS) using six-roll PSF template-subtracted coronagraphy suppressing the primary light of HR 4796A, with three image-plane occulters, and simultaneously subtracting the background light from its close angular proximity M2.5V companion. The resulting images unambiguously reveal the debris ring embedded within a much larger, morphologically complex, and biaxially asymmetric exo-ring scattering structure. These images at visible wavelengths are sensitive to and map the spatial distribution, brightness, and radial surface density of micron-size particles over 5 dex in surface brightness. These particles in the exo-ring environment may be unbound from the system and interacting with the local ISM. Herein, we present a new morphological and photometric view of the larger-than-prior-seen HR 4796A exoplanetary debris system with sensitivity to small particles at stellocentric distances an order of magnitude greater than has previously been observed.

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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

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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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Belt(s) of debris resolved around the Sco-Cen star HIP 67497

Cited by 38 publications

References 69 publications

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

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

The HR 4796A Debris System: Discovery of Extensive Exo-ring Dust Material

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

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