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

A. Meredith Hughes, Jesse Lieman-Sifry, Kevin M. Flaherty, Cail M. Daley, Aki Roberge, Ágnes Kóspál, A. Moór, Inga Kamp, David J. Wilner, Sean M. Andrews, Joel H. Kastner, P. Ábrahám

Research output: Article

14 Citations (Scopus)

Abstract

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 gas-bearing 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.

Original languageEnglish
Article number86
JournalAstrophysical Journal
Volume839
Issue number2
DOIs
Publication statusPublished - ápr. 20 2017

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debris
dust
profiles
gases
gas
gas bearings
radii
image resolution
visibility
A stars
power law
spectral energy distribution
wavelength
continuums
broadband
stars
energy

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Hughes, A. M., Lieman-Sifry, J., Flaherty, K. M., Daley, C. M., Roberge, A., Kóspál, Á., ... Ábrahám, P. (2017). Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti. Astrophysical Journal, 839(2), [86]. https://doi.org/10.3847/1538-4357/aa6b04

Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti. / Hughes, A. Meredith; Lieman-Sifry, Jesse; Flaherty, Kevin M.; Daley, Cail M.; Roberge, Aki; Kóspál, Ágnes; Moór, A.; Kamp, Inga; Wilner, David J.; Andrews, Sean M.; Kastner, Joel H.; Ábrahám, P.

In: Astrophysical Journal, Vol. 839, No. 2, 86, 20.04.2017.

Research output: Article

Hughes, AM, Lieman-Sifry, J, Flaherty, KM, Daley, CM, Roberge, A, Kóspál, Á, Moór, A, Kamp, I, Wilner, DJ, Andrews, SM, Kastner, JH & Ábrahám, P 2017, 'Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti', Astrophysical Journal, vol. 839, no. 2, 86. https://doi.org/10.3847/1538-4357/aa6b04
Hughes AM, Lieman-Sifry J, Flaherty KM, Daley CM, Roberge A, Kóspál Á et al. Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti. Astrophysical Journal. 2017 ápr. 20;839(2). 86. https://doi.org/10.3847/1538-4357/aa6b04
Hughes, A. Meredith ; Lieman-Sifry, Jesse ; Flaherty, Kevin M. ; Daley, Cail M. ; Roberge, Aki ; Kóspál, Ágnes ; Moór, A. ; Kamp, Inga ; Wilner, David J. ; Andrews, Sean M. ; Kastner, Joel H. ; Ábrahám, P. / Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti. In: Astrophysical Journal. 2017 ; Vol. 839, No. 2.
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abstract = "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 gas-bearing 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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AU - Kóspál, Ágnes

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AB - 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 gas-bearing 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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