Discovery of an 86 AU Radius Debris Ring around HD 181327

Schneider, Glenn; Silverstone, M. D.; Hines, Dean C.; Augereau, J.-C.; Pinte, C.; Ménard, F.; Krist, John; Clampin, Mark; Grady, C. A.; Golimowski, D. A.; Ardila, D. R.; Henning, Thomas; Wolf, S.; Rodmann, J.

doi:10.1086/506507

Cited by 109 publications

(156 citation statements)

References 54 publications

Supporting

Mentioning

145

Contrasting

Order By: Relevance

“…The 24.2 mJy/beam peak flux density is positioned on the star (within the pointing accuracy) with a 3σ peak located 22 away at a PA of 107 ± 7 • (with the uncertainty determined as the angle subtended by the pointing accuracy ±4 at the peak centre). A 4σ peak is also found on the opposite north-west (NW) extension of the disk, thus, the extended submm features are consistent with the orientation of the inclined dust ring previously imaged in scattered light by HST/NICMOS (PA of 107 ± 2 • ; Schneider et al 2006). In addition to the emission along the disk, we find a marginally resolved feature orthogonal to the disk, in the southward direction.…”

Section: Hd 181327supporting

confidence: 89%

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Nilsson

Liseau

Brandeker

et al. 2009

A&A

View full text Add to dashboard Cite

Context. Previous observations with the Infrared Astronomical Satellite and the Infrared Space Observatory, and ongoing observations with Spitzer and AKARI, have led to the discovery of over 200 debris disks, based on detected mid-and far infrared excess emission, indicating warm circumstellar dust. To constrain the properties of these systems, e.g., to more accurately determine the dust mass, temperature and radial extent, follow-up observations in the submillimetre wavelength region are needed. Aims. The β Pictoris moving group is a nearby stellar association of young (∼12 Myr) co-moving stars including the classical debris disk star β Pictoris. Due to their proximity and youth, they are excellent targets when searching for submillimetre emission from cold, extended, dust components produced by collisions in Kuiper-Belt-like disks. They also allow an age independent study of debris disk properties as a function of other stellar parameters. Methods. We observed 7 infrared-excess stars in the β Pictoris moving group with the LABOCA bolometer array, operating at a central wavelength of 870 μm at the 12-m submillimetre telescope APEX. The main emission at these wavelengths comes from large, cold dust grains, which constitute the main part of the total dust mass, and hence, for an optically thin case, make better estimates on the total dust mass than earlier infrared observations. Fitting the spectral energy distribution with combined optical and infrared photometry gives information on the temperature and radial extent of the disk. Results. From our sample, β Pic, HD 181327, and HD 172555 were detected with at least 3σ certainty, while all others are below 2σ and considered non-detections. The image of β Pic shows an offset flux density peak located near the south-west extension of the disk, similar to the one previously found by SCUBA at the JCMT. We present SED fits for detected sources and give an upper limit on the dust mass for undetected ones. Conclusions. We find a mean fractional dust luminosityf dust = 1.1 × 10 −3 at t ≈ 12 Myr, which together with recent data at 100 Myr suggests an f dust ∝ t −α decline of the emitting dust, with α > 0.8.

show abstract

Section: Hd 181327supporting

confidence: 89%

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

Nilsson

Liseau

Brandeker

et al. 2009

A&A

View full text Add to dashboard Cite

show abstract

“…The new profiles, displayed in the top panel of Fig. 5, show a peak at a distance of 88.6 AU and a surface brightness fainter by ∼21% (0.76 mJy arcsec −2 at the peak position) compared to the original Schneider et al (2006) study.…”

Section: Model Setupmentioning

confidence: 78%

An icy Kuiper belt around the young solar-type star HD 181327

Lebreton

Augereau

Thi

et al. 2012

A&A

105

161

View full text Add to dashboard Cite

Context. HD 181327 is a young main sequence F5/F6 V star belonging to the β Pictoris moving group (age ∼ 12 Myr). It harbors an optically thin belt of circumstellar material at radius ∼90 AU, presumed to result from collisions in a population of unseen planetesimals. Aims. We aim to study the dust properties in the belt in details, and to constrain the gas-to-dust ratio. Methods. We obtained far-infrared photometric observations of HD 181327 with the PACS instrument onboard the Herschel Space Observatory , complemented by new 3.2 mm observations carried with the ATCA array. The geometry of the belt is constrained with newly reduced HST/NICMOS scattered light images that allow the degeneracy between the disk geometry and the dust properties to be broken. We then use the radiative transfer code GRaTeR to compute a large grid of models, and we identify the grain models that best reproduce the spectral energy distribution (SED) through a Bayesian analysis. We attempt to detect the oxygen and ionized carbon fine-structure lines with Herschel/PACS spectroscopy, providing observables to our photochemical code ProDiMo. Results. The HST observations confirm that the dust is confined in a narrow belt. The continuum is detected with Herschel/PACS completing nicely the SED in the far-infrared. The disk is marginally resolved with both PACS and ATCA. A medium integration of the gas spectral lines only provides upper limits on the [OI] and [CII] line fluxes. We show that the HD 181327 dust disk consists of micron-sized grains of porous amorphous silicates and carbonaceous material surrounded by an important layer of ice, for a total dust mass of ∼0.05 M ⊕ (in grains up to 1 mm). We discuss evidences that the grains consists of fluffy aggregates. The upper limits on the gas atomic lines do not provide unambiguous constraints: only if the PAH abundance is high, the gas mass must be lower than ∼17 M ⊕ . Conclusions. Despite the weak constraints on the gas disk, the age of HD 181327 and the properties of the dust disk suggest that it has passed the stage of gaseous planets formation. The dust reveals a population of icy planetesimals, similar to the primitive Edgeworth-Kuiper belt, that may be a source for the future delivery of water and volatiles onto forming terrestrial planets.

show abstract

“…However, the model based on the Hedman & Stark fit shows the degree to which the total brightness of the disc in scattered light may be underestimated. Accordingly, non-Mie fits to observed discs find weaker anisotropy, with g < 0.5 (e. g., Kalas et al 2005;Schneider et al 2006;Debes et al 2008;Thalmann et al 2011;Schneider et al 2014). …”

Section: Spectral Energy Distributions and Imagesmentioning

confidence: 99%

Collisions and drag in debris discs with eccentric parent belts

Löhne

Krivov

Kirchschlager

et al. 2017

A&A

View full text Add to dashboard Cite

Context. High-resolution images of circumstellar debris discs reveal off-centred rings that indicate past or ongoing perturbation, possibly caused by secular gravitational interaction with unseen stellar or substellar companions. The purely dynamical aspects of this departure from radial symmetry are well understood. However, the observed dust is subject to additional forces and effects, most notably collisions and drag. Aims. To complement the studies of dynamics, we therefore aim to understand how new asymmetries are created by the addition of collisional evolution and drag forces, and existing ones strengthened or overridden. Methods. We augmented our existing numerical code "Analysis of Collisional Evolution" (ACE) by an azimuthal dimension, the longitude of periapse. A set of fiducial discs with global eccentricities ranging from 0 to 0.4 is evolved over giga-year timescales. Size distribution and spatial variation of dust are analysed and interpreted. The basic impact of belt eccentricity on spectral energy distributions (SEDs) and images is discussed. Results. We find features imposed on characteristic timescales. First, radiation pressure defines size cutoffs that differ between periapse and apoapse, resulting in an asymmetric halo. The differences in size distribution make the observable asymmetry of the halo depend on wavelength. Second, collisional equilibrium prefers smaller grains on the apastron side of the parent belt, reducing the effect of pericentre glow and the overall asymmetry. Third, Poynting-Robertson drag fills the region interior to an eccentric belt such that the apastron side is more tenuous. Interpretation and prediction of the appearance in scattered light is problematic when spatial and size distribution are coupled.

show abstract

Discovery of an 86 AU Radius Debris Ring around HD 181327

Cited by 109 publications

References 54 publications

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

A submillimetre search for cold extended debris disks in the $\mathsf{\beta}$ Pictoris moving group

An icy Kuiper belt around the young solar-type star HD 181327

Collisions and drag in debris discs with eccentric parent belts

Contact Info

Product

Resources

About