<i>Herschel</i>discovery of a new class of cold, faint debris discs

Eiroa, C.; Marshall, Jonathan P.; Mora, A.; Krivov, A. V.; Montesinos, B.; Absil, Olivier; Ardila, D. R.; Arévalo, M. J.; Augereau, J.-C.; Bayo, A.; Danchi, W. C.; Burgo, C. del; Ertel, S.; Fridlund, M.; González-García, B. M.; Heras, A. M.; Lebreton, J.; Liseau, R.; Maldonado, J.; Meeus, G.; Montes, D.; Pilbratt, G. L.; Roberge, Aki; Sanz-Forcada, J.; Stapelfeldt, K.; Thébault, P.; White, G. J.; Wolf, S.

doi:10.1051/0004-6361/201117797

Cited by 41 publications

(56 citation statements)

References 22 publications

(20 reference statements)

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“…, and producing extended emission at wavelengths up to 250 µm, which is not observed. These properties would place it amongst those "cold disc candidates" identified in Eiroa et al (2011), Eiroa et al (2013), and Marshall et al (2013), albeit much brighter than those previously identified and therefore inconsistent with the explanation for the phenomenon proposed in Krivov et al (2013). We therefore disfavour this explanation for the shape of the SED.…”

Section: Hip 22263contrasting

confidence: 55%

Interpreting the extended emission around three nearby debris disc host stars

Marshall¹,

Kirchschlager²,

Augereau³

et al. 2014

A&A

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Context. Cool debris discs are a relic of the planetesimal formation process around their host star, analogous to the solar system's Edgeworth-Kuiper belt. As such, they can be used as a proxy to probe the origin and formation of planetary systems like our own. Aims. The Herschel open time key programmes "DUst around NEarby Stars" (DUNES) and "Disc Emission via a Bias-free Reconnaissance in the Infrared/Submillimetre" (DEBRIS) observed many nearby, sun-like stars at far-infrared wavelengths seeking to detect and characterize the emission from their circumstellar dust. Excess emission attributable to the presence of dust was identified from around ∼20% of stars. Herschel's high angular resolution (∼7 FWHM at 100 µm) provided the capacity for resolving debris belts around nearby stars with radial extents comparable to the solar system (50-100 au). Methods. As part of the DUNES and DEBRIS surveys, we obtained observations of three debris disc stars, HIP 22263 (HD 30495), HIP 62207 (HD 110897), and HIP 72848 (HD 131511), at far-infrared wavelengths with the Herschel PACS instrument. Combining these new images and photometry with ancilliary data from the literature, we undertook simultaneous multi-wavelength modelling of the discs' radial profiles and spectral energy distributions using three different methodologies: single annulus, modified black body, and a radiative transfer code. Results. We present the first far-infrared spatially resolved images of these discs and new single-component debris disc models. We characterize the capacity of the models to reproduce the disc parameters based on marginally resolved emission through analysis of two sets of simulated systems (based on the HIP 22263 and HIP 62207 data) with the noise levels typical of the Herschel images. We find that the input parameter values are recovered well at noise levels attained in the observations presented here.

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Section: Hip 22263contrasting

confidence: 55%

Interpreting the extended emission around three nearby debris disc host stars

Marshall¹,

Kirchschlager²,

Augereau³

et al. 2014

A&A

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“…The colder disc component postulated here would be analogous to the "cold debris discs" candidates identified in Eiroa et al (2011). In addition to the requirement that the grains are large, they should have a low absorption in the visible, perhaps through the presence of icy material on the grain surface.…”

Section: Circumstellar Emissionmentioning

confidence: 70%

“…Several intriguing debris disc candidate sources have been identified in DUNES Herschel PACS and SPIRE observations of nearby stars (Eiroa et al 2011). These "cold disc candidates" exhibit only marginal excess emission at wavelengths shortward of 100 µm, a peak in the spectral energy distribution (SED) at 160 µm and no detectable sub-mm excess in SPIRE observations.…”

Section: Introductionmentioning

confidence: 99%

Herschelobservations of the debris disc around HIP 92043

Marshall¹,

Krivov²,

Burgo³

et al. 2013

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Context. Typical debris discs are composed of particles ranging from several micron sized dust grains to km sized asteroidal bodies, and their infrared emission peaks at wavelengths 60-100 µm. Recent Herschel DUNES observations have identified several debris discs around nearby Sun-like stars (F, G and K spectral type) with significant excess emission only at 160 µm. Aims. We observed HIP 92043 (110 Her, HD 173667) at far-infrared and sub-millimetre wavelengths with Herschel PACS and SPIRE. Identification of the presence of excess emission from HIP 92043 and the origin and physical properties of any excess was undertaken through analysis of its spectral energy distribution (SED) and the PACS images. Methods. The PACS and SPIRE images were produced using the HIPE photProject map maker routine. Fluxes were measured using aperture photometry. A stellar photosphere model was scaled to optical and near infrared photometry and subtracted from the farinfared and sub-mm fluxes to determine the presence of excess emission. Source radial profiles were fitted using a 2D Gaussian and compared to a PSF model based on Herschel observations of α Boo to check for extended emission. Results. Clear excess emission from HIP 92043 was observed at 70 and 100 µm. Marginal excess was observed at 160 and 250 µm. Analysis of the images reveals that the source is extended at 160 µm. A fit to the source SED is inconsistent with a photosphere and single temperature black body. Conclusions. The excess emission from HIP 92043 is consistent with the presence of an unresolved circumstellar debris disc at 70 and 100 µm, with low probability of background contamination. The extended 160 µm emission may be interpreted as an additional cold component to the debris disc or as the result of background contamination along the line of sight. The nature of the 160 µm excess cannot be determined absolutely from the available data, but we favour a debris disc interpretation, drawing parallels with previously identified cold disc sources in the DUNES sample.

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“…In addition, from a purely observational point of view, a huge population of fairly massive, but cold disks A&A 537, A110 (2012) could still be hidden below current sensitivity limits. Some of these will be revealed by Herschel (Pilbratt et al 2010;Eiroa et al 2011).…”

Section: Introductionmentioning

confidence: 96%

Modelling the huge,Herschel-resolved debris ring around HD 207129

Löhne

Augereau

Ertel

et al. 2012

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Debris disks, which are inferred from the observed infrared excess to be ensembles of dust, rocks, and probably planetesimals, are common features of stellar systems. As the mechanisms of their formation and evolution are linked to those of planetary bodies, they provide valuable information. The few well-resolved debris disks are even more valuable because they can serve as modelling benchmarks and help resolve degeneracies in modelling aspects such as typical grain sizes and distances. Here, we present an analysis of the HD 207129 debris disk, based on its well-covered spectral energy distribution and Herschel/PACS images obtained in the framework of the DUNES (DUst around NEarby Stars) programme. We use an empirical power-law approach to the distribution of dust and we then model the production and removal of dust by means of collisions, direct radiation pressure, and drag forces. The resulting best-fit model contains a total of nearly 10 −2 Earth masses in dust, with typical grain sizes in the planetesimal belt ranging from 4 to 7 µm. We constrain the dynamical excitation to be low, which results in very long collisional lifetimes and a drag that notably fills the inner gap, especially at 70 µm. The radial distribution stretches from well within 100 AU in an unusual, outward-rising slope towards a rather sharp outer edge at about 170-190 AU. The inner edge is therefore smoother than that reported for Fomalhaut, but the contribution from the extended halo of barely bound grains is similarly small. Both slowly self-stirring and planetary perturbations could potentially have formed and shaped this disk.

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Herscheldiscovery of a new class of cold, faint debris discs

Cited by 41 publications

References 22 publications

Interpreting the extended emission around three nearby debris disc host stars

Interpreting the extended emission around three nearby debris disc host stars

Herschelobservations of the debris disc around HIP 92043

Modelling the huge,Herschel-resolved debris ring around HD 207129

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