First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti

Choquet, Élodie; Milli, J.; Wahhaj, Z.; Soummer, Rémi; Roberge, Aki; Augereau, J.-C.; Booth, Mark; Absil, Olivier; Boccaletti, A.; Chen, Christine; Debes, John H.; Burgo, C. del; Dent, W. R. F.; Ertel, S.; Girard, J.; Gofas-Salas, Elena; Golimowski, D. A.; González, C.; Hagan, J.; Hibon, Pascale; Hines, Dean C.; Kennedy, Grant M.; Lagrange, A.-M.; Matrà, Luca; Mawet, Dimitri; Mouillet, D.; N’Diaye, Mamadou; Perrin, Marshall D.; Pinte, C.; Pueyo, Laurent; Rajan, Abhijith; Schneider, Glenn; Wolff, Schuyler; Wyatt, M. C.

doi:10.3847/2041-8213/834/2/l12

Cited by 51 publications

(71 citation statements)

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“…Alternatively, it is possible that the grains are predominantly carbonaceous in nature rather than silicate, which would also alter the density structure of the disk. This scenario is supported by the low albedo of 49 Ceti in previous HST NICMOS observations searching for scattered light in the outer disk (Weinberger et al 1999;Choquet et al 2017), and by the evidence for carbon overabundance in the atomic gas disk from line-of-sight UV absorption spectroscopy .…”

Section: R Xsupporting

confidence: 59%

“…Until recently, very little was known about the distribution of gas and dust in the 49 Ceti system. Hubble Space Telescope (HST) coronographic observations reprocessed with modern imaging techniques reveal a low surface brightness disk extending from 65 to 250 au, and imply that the grain size in the outer disk is m >2 m (Weinberger et al 1999;Choquet et al 2017). Subsarcecond-scale imaging at wavelengths of 12 and 18 μm with Keck (Wahhaj et al 2007) resolved an elongated distribution of small dust grains near the star, but analysis of the SED implied that most of the dust mass in the system lies at larger radii and was not spatially resolved by their observations.…”

Section: Introductionmentioning

confidence: 99%

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Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti

Hughes

Lieman-Sifry

Flaherty

et al. 2017

ApJ

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127

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We present ∼0 4 resolution images of CO(3-2) and associated continuum emission from the gas-bearing debris disk around the nearby A star 49 Ceti, observed with the Atacama Large Millimeter/Submillimeter Array (ALMA). We analyze the ALMA visibilities in tandem with the broadband spectral energy distribution to measure the radial surface density profiles of dust and gas emission from the system. The dust surface density decreases with radius between ∼100 and 310 au, with a marginally significant enhancement of surface density at a radius of ∼110 au. The SED requires an inner disk of small grains in addition to the outer disk of larger grains resolved by ALMA. The gas disk exhibits a surface density profile that increases with radius, contrary to most previous spatially resolved observations of circumstellar gas disks. While ∼80% of the CO flux is well described by an axisymmetric power-law disk in Keplerian rotation about the central star, residuals at ∼20% of the peak flux exhibit a departure from axisymmetry suggestive of spiral arms or a warp in the gas disk. The radial extent of the gas disk (∼220 au) is smaller than that of the dust disk (∼300 au), consistent with recent observations of other gasbearing debris disks. While there are so far only three broad debris disks with wellcharacterized radial dust profiles at millimeter wavelengths, 49 Ceti's disk shows a markedly different structure from two radially resolved gas-poor debris disks, implying that the physical processes generating and sculpting the gas and dust are fundamentally different.

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Section: R Xsupporting

confidence: 59%

Section: Introductionmentioning

confidence: 99%

Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti

Hughes

Lieman-Sifry

Flaherty

et al. 2017

ApJ

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127

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“…They found three such discs: HR 8799, HD 95086 and 49 Cet. While HD 95086 does have one directly imaged planet with a large gap to the inner edge of the disc (Rameau et al 2013), planets around 49 Cet are still waiting to be discovered (Choquet et al 2017). Given the fact that the discs in these two systems are extended and the planets there are either known or at least strongly suspected, we propose them to be particularly good candidates for hosting scattered discs.…”

Section: Other Systemsmentioning

confidence: 96%

The scattered disc of HR 8799

Geiler

Krivov

Booth

et al. 2018

Monthly Notices of the Royal Astronomical Society

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HR 8799 is a young F0-type star with four directly imaged giant planets and two debris belts, one located exterior and another one interior to the region occupied by the planetary orbits. Having an architecture similar to that of our Solar System, but also revealing dissimilarities such as high masses of planets, a huge radial extent and a high mass of the outer debris belt, HR 8799 is considered to be a benchmark to test formation and evolution models of planetary systems. Here we focus on the outer debris ring and its relation to the planets. We demonstrate that the models of the outer disc, proposed previously to reproduce Herschel observations, are inconsistent with the ALMA data, and vice versa. In an attempt to find a physically motivated model that would agree with both observational sets, we perform collisional simulations. We show that a narrow planetesimal belt and a radiation pressure induced dust halo cannot account for the observed radial brightness profiles. A single, wide planetesimal disc does not reproduce the data either. Instead, we propose a two-population model, comprising a Kuiper-Belt-like structure of a low-eccentricity planetesimal population ("the classical Kuiper Belt") and a high-eccentricity population of comets ("scattered disc"). We argue that such a structure of the exo-Kuiper belt of HR 8799 could be explained with planet migration scenarios analogous to those proposed for the Kuiper Belt of the Solar System.

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“…The disk around HD104860 has been previously resolved in thermal emission with Herschel-PACS at 100 and 160μm (Morales et al 2013(Morales et al , 2016, but that around HD192758 has not been resolved so far. These two new detections bring the number of debris disks first imaged in scattered light by the ALICE program to 11, demonstrating the efficacy of our post-processing method in detecting faint resolved circumstellar material Choquet et al 2016Choquet et al , 2017. Along with the five debris disks detected during its operational time, NICMOS currently holds the record of the most debris disks first imaged in scattered light.…”

Section: Introductionmentioning

confidence: 94%

HD 104860 and HD 192758: Two Debris Disks Newly Imaged in Scattered Light with the Hubble Space Telescope

Choquet

Bryden

Perrin

et al. 2018

ApJ

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We present the first scattered-light images of two debris disks around the F8 star HD104860 and the F0V star HD192758, respectively ∼45 and ∼67pc away. We detected these systems in the F110W and F160W filters through our reanalysis of archival Hubble Space Telescope (HST) NICMOS data with modern starlight-subtraction techniques. Our image of HD104860 confirms the morphology previously observed by Herschel in thermal emission with a well-defined ring at a radius of ∼114au inclined by ∼58°. Although the outer edge profile is consistent with dynamical evolution models, the sharp inner edge suggests sculpting by unseen perturbers. Our images of HD192758 reveal a disk at radius ∼95au inclined by ∼59°, never resolved so far. These disks have low scattering albedos of 10% and 13%, respectively, inconsistent with water ice grain compositions. They are reminiscent of several other disks with similar inclination and scattering albedos: Fomalhaut, HD92945, HD202628, and HD207129. They are also very distinct from brighter disks in the same inclination bin, which point to different compositions between these two populations. Varying scattering albedo values can be explained by different grain porosities, chemical compositions, or grain size distributions, which may indicate distinct formation mechanisms or dynamical processes at work in these systems. Finally, these faint disks with large infrared excesses may be representative of an underlying population of systems with low albedo values. Searches with more sensitive instruments on HST or on the James Webb Space Telescope and using state-of-the art starlightsubtraction methods may help discover more of such faint systems.

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First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti

Cited by 51 publications

References 50 publications

Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti

Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti

The scattered disc of HR 8799

HD 104860 and HD 192758: Two Debris Disks Newly Imaged in Scattered Light with the Hubble Space Telescope

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