A Complete ALMA Map of the Fomalhaut Debris Disk

MacGregor, Meredith A.; Matrà, Luca; Kalas, Paul; Wilner, David J.; Pan, Margaret; Kennedy, Grant M.; Wyatt, M. C.; Duchêne, Gaspard; Hughes, A. Meredith; Rieke, G. H.; Clampin, Mark; Fitzgerald, Michael P.; Graham, James R.; Holland, W. S.; Panić, Olja; Shannon, Andrew; Su, Kate

doi:10.3847/1538-4357/aa71ae

Cited by 107 publications

(104 citation statements)

References 51 publications

(128 reference statements)

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“…Fomalhaut's disk (see Fig. 1) is perhaps a better example, being brighter and larger on the sky so that the offset and asymmetries are more clearly seen (Kalas et al 2005;MacGregor et al 2017), with additional azimuthal structure also evident (Kalas et al 2013).…”

Section: Dynamical Structuresmentioning

confidence: 99%

Extrasolar Kuiper belts

Wyatt

2020

The Trans-Neptunian Solar System

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Extrasolar debris disks are the dust disks found around nearby main sequence stars arising from the break-up of asteroids and comets orbiting the stars. Far-IR surveys (e.g., with Herschel) showed that ∼ 20% of stars host detectable dust levels. While dust temperatures suggest a location at 10s of au comparable with our Kuiper belt, orders of magnitude more dust is required implying a planetesimal population more comparable with the primordial Kuiper belt. High resolution imaging (e.g., with ALMA) has mapped the nearest and brightest disks, providing evidence for structures shaped by an underlying planetary system. Some of these are analogous to structures in our own Kuiper belt (e.g., the hot and cold classical, resonant, scattered disk and cometary populations), while others have no Solar System counterpart. CO gas is seen in some debris disks, and inferred to originate in the destruction of planetesimals with a similar volatile-rich composition to Solar System comets. This chapter reviews our understanding of extrasolar Kuiper belts and of how our own Kuiper belt compares with those of neighbouring stars.

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Section: Dynamical Structuresmentioning

confidence: 99%

Extrasolar Kuiper belts

Wyatt

2020

The Trans-Neptunian Solar System

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“…Disk morphologies suggestive of influences from unseen planets, such as resonance clumps (Wyatt 2003) and/or apo-center glow (Pan et al 2016), are also best observed at submillimeter/millimeter wavelengths (e.g., Ertel et al 2012;Löhne et al 2017). Existing ALMA data on debris disks show a large variety of Kuiper-belt analogs: some systems have very narrow rings of parent bodies (e.g., Fomalhaut, Boley et al 2012;MacGregor et al 2017, andEri, Booth et al 2017), and some have either multiple rings (HD 107146, Ricci et al 2015a) or broad disks (HR 8799, Booth et al 2016;τ Ceti, MacGregor et al 2016;61 Vir, Marino et al 2017). The parent body distributions are therefore giving insights to the possible overall structure of the planetary systems.…”

Section: Introductionmentioning

confidence: 99%

ALMA 1.3 mm Map of the HD 95086 System

Su¹,

MacGregor²,

Booth³

et al. 2017

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Planets and minor bodies such as asteroids, Kuiper-belt objects and comets are integral components of a planetary system. Interactions among them leave clues about the formation process of a planetary system. The signature of such interactions is most prominent through observations of its debris disk at millimeter wavelengths where emission is dominated by the population of large grains that stay close to their parent bodies. Here we present ALMA 1.3 mm observations of HD 95086, a young early-type star that hosts a directly imaged giant planet b and a massive debris disk with both asteroid-and Kuiper-belt analogs. The location of the Kuiper-belt analog is resolved for the first time. The system can be depicted as a broad (∆R/R ∼0.84), inclined (30• ±3• ) ring with millimeter emission peaked at 200±6 au from the star. The 1.3 mm disk emission is consistent with a broad disk with sharp boundaries from 106±6 to 320±20 au with a surface density distribution described by a power law with an index of -0.5±0.2. Our deep ALMA map also reveals a bright source located near the edge of the ring, whose brightness at 1.3 mm and potential spectral energy distribution are consistent with it being a luminous star-forming galaxy at high redshift. We set constraints on the orbital properties of planet b assuming co-planarity with the observed disk.

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“…The nature of the warm components is less certain, as they reside closer to the star and cannot easily be spatially resolved. For example, the nearby (7.7 pc) star Fomalhaut hosts a well-studied cold belt that has been resolved at several wavelengths (Kalas et al 2005;Acke et al 2012;Boley et al 2012;MacGregor et al 2017). From analyses of its SED and infrared images, Fomalhaut also hosts a warm component (Stapelfeldt et al 2004;Su et al 2013), but obtaining resolved images of this warm component to confirm its properties remains difficult .…”

Section: Introductionmentioning

confidence: 99%

What Sets the Radial Locations of Warm Debris Disks?

Ballering

Rieke

et al. 2017

ApJ

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The architectures of debris disks encode the history of planet formation in these systems. Studies of debris disks via their spectral energy distributions (SEDs) have found infrared excesses arising from cold dust, warm dust, or a combination of the two. The cold outer belts of many systems have been imaged, facilitating their study in great detail. Far less is known about the warm components, including the origin of the dust. The regularity of the disk temperatures indicates an underlying structure that may be linked to the water snow line. If the dust is generated from collisions in an exo-asteroid belt, the dust will likely trace the location of the water snow line in the primordial protoplanetary disk where planetesimal growth was enhanced. If instead the warm dust arises from the inward transport from a reservoir of icy material farther out in the system, the dust location is expected to be set by the current snow line. We analyze the SEDs of a large sample of debris disks with warm components. We find that warm components in single-component systems (those without detectable cold components) follow the primordial snow line rather than the current snow line, so they likely arise from exo-asteroid belts. While the locations of many warm components in two-component systems are also consistent with the primordial snow line, there is more diversity among these systems, suggesting additional effects play a role.

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A Complete ALMA Map of the Fomalhaut Debris Disk

Cited by 107 publications

References 51 publications

Extrasolar Kuiper belts

Extrasolar Kuiper belts

ALMA 1.3 mm Map of the HD 95086 System

What Sets the Radial Locations of Warm Debris Disks?

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