PROBING FOR EXOPLANETS HIDING IN DUSTY DEBRIS DISKS: DISK IMAGING, CHARACTERIZATION, AND EXPLORATION WITH<i>HST</i>/STIS MULTI-ROLL CORONAGRAPHY

Schneider, Glenn; Grady, C. A.; Hines, Dean C.; Stark, Christopher C.; Debes, John H.; Carson, J.; Kuchner, Marc J.; Perrin, Marshall D.; Weinberger, Alycia J.; Wisniewski, John P.; Silverstone, M. D.; Jang‐Condell, Hannah; Henning, Thomas; Woodgate, B. E.; Serabyn, Eugene; Moro‐Martín, Amaya; Tamura, Motohide; Hinz, Philip M.; Rodigas, Timothy J.

doi:10.1088/0004-6256/148/4/59

Cited by 206 publications

(335 citation statements)

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“…Another asymmetric feature is seen on the east side up to 8 arcsec, but can not be easily related to the structures seen with SPHERE. Different asymmetries at different scales have already been noticed for HD 106906 (Kalas et al 2015) and HD 32297 (Esposito et al 2014;Schneider et al 2014) for example. One candidate companion (#1, see Appendix B) could lie within the structures revealed by STIS and the arc seen with SPHERE.…”

Section: Discussionmentioning

confidence: 80%

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

Bonnefoy

Milli

Ménard

et al. 2017

A&A

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Aims. In 2015, we initiated a survey of Scorpius-Centaurus A-F stars that are predicted to host warm-inner and cold-outer belts of debris similar to the case of the system HR 8799. The survey aims to resolve the disks and detect planets responsible for the disk morphology. In this paper, we study the F-type star HIP 67497 and present a first-order modelization of the disk in order to derive its main properties. Methods. We used the near-infrared integral field spectrograph (IFS) and dual-band imager IRDIS of VLT/SPHERE to obtain angulardifferential imaging observations of the circumstellar environnement of HIP 67497. We removed the stellar halo with PCA and TLOCI algorithms. The disk emission was modeled with the GRaTeR code. Results. We resolve a ring-like structure that extends up to ∼450 mas (∼50 au) from the star in the IRDIS and IFS data. It is best reproduced by models of a non-eccentric ring with an inclination of 80 ± 1 • , a position angle of −93 ± 1 • , and a semi-major axis of 59 ± 3 au. We also detect an additional, but fainter, arc-like structure with a larger extension (0.65 arcsec) South of the ring that we model as a second belt of debris at ∼130 au. We detect ten candidate companions at separations ≥1 . We estimate the mass of putative perturbers responsible for the disk morphology and compare this to our detection limits. Additional data are needed to find those perturbers, and to relate our images to large-scale structures seen with HST/STIS.

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Section: Discussionmentioning

confidence: 80%

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

Bonnefoy

Milli

Ménard

et al. 2017

A&A

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“…Later on, Shen et al (2009) showed that the results from Graham et al (2007) can be reproduced by a distribution of sphere cluster aggregates with size distribution index −3.5, volume-equivalent radii between 0.1 and 0.4 µm, and a porosity of 60%. In this work, our models are compared with the optical and near-IR surface brightness profiles from Fitzgerald et al (2007) and Schneider et al (2014) and with the measured degree of polarisation from Graham et al (2007). Since our modelling deals with axisymmetric discs, all observed profiles had been averaged over the SE and NW disc sides in order to remove the observed surface brightness anomalies.…”

Section: Scattered Lightmentioning

confidence: 99%

“…To account for the extended halo of small particles, the flux was integrated up to stellocentric distances of r = 150 au for each line of sight. We also compared with the radial profiles extracted from the high-resolution HST/STIS image by Schneider et al (2014). In their Fig.…”

Section: Impact On Scattered Lightmentioning

confidence: 99%

“…In addition, asymmetries on small and large scales with several local brightness maxima and minima have been detected at stellocentric distances beyond 20 au (Liu 2004;Krist et al 2005;Fitzgerald et al 2007). In the latest high spatial resolution Space Telescope Imaging Spectrograph (STIS) images, Schneider et al (2014) have found a distinct brightness enhancement above the disc midplane on the south-eastern (SE) side at about 13 au from the star. Furthermore, a disc warp is discernible on the north-western (NW) side between 13 and 45 au, opposite to the SE brightness bump.…”

Section: Introductionmentioning

confidence: 99%

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Collisional modelling of the AU Microscopii debris disc

Schüppler

Löhne

Krivov

et al. 2015

A&A

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AU Microscopii's debris disc is one of the most famous and best-studied debris discs and one of only two resolved debris discs around M stars. We perform in-depth collisional modelling of the AU Mic disc including stellar radiative and corpuscular forces (stellar winds), aiming at a comprehensive understanding of the dust production and the dust and planetesimal dynamics in the system. Our models are compared to a suite of observational data for thermal and scattered light emission, ranging from the ALMA radial surface brightness profile at 1.3 mm to spatially resolved polarisation measurements in the visible. Most of the data are shown to be reproduced with dust production in a belt of planetesimals with an outer edge at around 40 au and subsequent inward transport of dust by stellar winds. A low dynamical excitation of the planetesimals with eccentricities up to 0.03 is preferred. The radial width of the planetesimal belt cannot be constrained tightly. Belts that are 5 au and 17 au wide, as well as a broad 44 au-wide belt, are consistent with observations. All models show surface density profiles that increase with distance from the star up to ≈40 au, as inferred from observations. The best model is achieved by assuming a stellar mass loss rate that exceeds the solar one by a factor of 50. The models reproduce the spectral energy distribution and the shape of the ALMA radial profile well, but deviate from the scattered light observations more strongly. The observations show a bluer disc colour and a lower degree of polarisation for projected distances <40 au than predicted by the models. These deviations may be reduced by taking irregularly shaped dust grains which have scattering properties different from the Mie spheres used in this work. From tests with a handful of selected dust materials, we favour mixtures of silicate, carbon, and ice of moderate porosity. We also address the origin of the unresolved central excess emission detected by ALMA and show that it cannot stem from an additional inner belt alone. Instead, it should derive, at least partly, from the chromosphere of the central star.

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“…Other debris disk systems with exterior massive perturbers are likely not uncommon; surveys indicate that~25% of debris disks exist in binary or triple star systems (Rodriguez & Zuckerman 2012). Planetary-mass exterior companions like HD 106906b may be responsible for the asymmetries in observed debris disks such as HD 61005 (Hines et al 2007;Esposito et al 2016) and HD 15115 (Rodigas et al 2012;Schneider et al 2014;MacGregor et al 2015), for example.…”

mentioning

confidence: 99%

HD 106906: A Case Study for External Perturbations of a Debris Disk

Nesvold

Naoz²,

Fitzgerald³

2017

ApJL

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Models of debris disk morphology are often focused on the effects of a planet orbiting interior to or within the disk. Nonetheless, an exterior planetary-mass perturber can also excite eccentricities in a debris disk, via LaplaceLagrange secular perturbations in the coplanar case or Kozai-Lidov perturbations for mutually inclined companions and disks. HD 106906 is an ideal example of such a a system, as it harbors a confirmed exterior M 11 Jup companion at a projected separation of 650 au outside a resolved, asymmetric disk. We use collisional and dynamical simulations to investigate the interactions between the disk and the companion, and to use the disk's observed morphology to place constraints on the companion's orbit. We conclude that the disk's observed morphology is consistent with perturbations from the observed exterior companion. Generalizing this result, we suggest that exterior perturbers, as well as interior planets, should be considered when investigating the cause of observed asymmetries in a debris disk.

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PROBING FOR EXOPLANETS HIDING IN DUSTY DEBRIS DISKS: DISK IMAGING, CHARACTERIZATION, AND EXPLORATION WITHHST/STIS MULTI-ROLL CORONAGRAPHY

Cited by 206 publications

References 109 publications

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

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

Collisional modelling of the AU Microscopii debris disc

HD 106906: A Case Study for External Perturbations of a Debris Disk

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