First Scattered-Light Image of the Debris Disk Around Hd 131835 With the Gemini Planet Imager

Hung, Li Wei; Duchêne, Gaspard; Arriaga, Pauline; Fitzgerald, Michael P.; Maire, Jérôme; Marois, Christian; Millar-Blanchaer, Max; Bruzzone, Sebastian; Rajan, Abhijith; Pueyo, Laurent; Kalas, Paul; Rosa, Robert J. De; Graham, James R.; Konopacky, Quinn; Wolff, Schuyler; Ammons, S. Mark; Chen, Christine; Chilcote, Jeffrey; Draper, Zachary H.; Espósito, Thomas M.; Gerard, Benjamin L.; Goodsell, Stephen J.; Greenbaum, Alexandra Z.; Hibon, Pascale; Hinkley, Sasha; Macintosh, Bruce; Marchis, Franck; Metchev, Stanimir; Nielsen, Eric L.; Oppenheimer, Ben R.; Patience, Jennifer; Perrin, Marshall D.; Rantakyrö, Fredrik T.; Sivaramakrishnan, Anand; Wang, Jason; Ward-Duong, Kimberly; Wiktorowicz, Sloane

doi:10.1088/2041-8205/815/1/l14

Cited by 61 publications

(35 citation statements)

References 45 publications

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“…The bulk of the emission is within 1 arcsec (i.e., ∼145 au) and appears consistent with a highly inclined axisymmetric disc as found from previous resolved observations of the disc at different wavelengths (e.g. Hung et al 2015b;Feldt et al 2017). The disc parameters such as inclination, PA, and disc mass are derived in the next subsection 3.2 using an MCMC approach to fit a dust disc model to the observed visibilities.…”

Section: Dust Continuum Observationssupporting

confidence: 80%

“…An infrared (IR) excess around this star has first been reported by Moór et al (2006), establishing the presence of a bright debris disc. The disc was first resolved in mid-infrared using T-ReCS from which it could be deduced that multiple disc components were needed to fit the data (Hung et al 2015b). More recently, SPHERE observations in the near-IR led to the detection of a series of narrow concentric rings (Feldt et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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Imaging [CI] around HD 131835: reinterpreting young debris discs with protoplanetary disc levels of CO gas as shielded secondary discs

Kral

Marino

Wyatt

et al. 2018

Monthly Notices of the Royal Astronomical Society

114

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Despite being > 10Myr, there are ∼10 debris discs with as much CO gas as in protoplanetary discs. Such discs have been assumed to be "hybrid", i.e., with secondary dust but primordial gas. Here we show that both the dust and gas in such systems could instead be secondary, with the high CO content caused by accumulation of neutral carbon (C 0 ) that shields CO from photodissociating; i.e., these could be "shielded secondary discs". New ALMA observations are presented of HD131835 that detect ∼ 3 × 10 −3 M ⊕ of C 0 , the majority 40-200au from the star, in sufficient quantity to shield the previously detected CO. A simple semi-analytic model for the evolution of CO, C and O originating in a volatile-rich planetesimal belt shows how CO shielding becomes important when the viscous evolution is slow (low α parameter) and/or the CO production rate is high. Shielding by C 0 may also cause the CO content to reach levels at which CO self-shields, and the gas disc may become massive enough to affect the dust evolution. Application to the HD 131835 observations shows these can be explained if α ∼ 10 −3 ; an inner cavity in C 0 and CO may also mean the system has yet to reach steady state. Application to other debris discs with high CO content finds general agreement for α = 10 −3 to 0.1. The shielded secondary nature of these gas discs can be tested by searching for C 0 , as well as CN, N 2 and CH + , which are also expected to be shielded by C 0 .

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Section: Dust Continuum Observationssupporting

confidence: 80%

Section: Introductionmentioning

confidence: 99%

Imaging [CI] around HD 131835: reinterpreting young debris discs with protoplanetary disc levels of CO gas as shielded secondary discs

Kral

Marino

Wyatt

et al. 2018

Monthly Notices of the Royal Astronomical Society

114

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“…Combining the datacubes results in a three-dimensional Stokes cube containing the Stokes parameters {I, Q, U , V }, rotated to place North up. Finally, the Stokes cube was photometrically calibrated using the satellite spot fluxes by assuming the same satellite-spot-to-star flux ratio as we did for H-Spec and following the methods described in Hung et al (2015). We recovered only a very low S/N total intensity detection from this H-Pol data set with 3.8 • of field rotation, so we use only the H-Spec data for total intensity analysis.…”

Section: Gemini Planet Imagermentioning

confidence: 99%

Direct Imaging of the HD 35841 Debris Disk: A Polarized Dust Ring from Gemini Planet Imager and an Outer Halo from HST/STIS

Espósito

Duchêne

Kalas

et al. 2018

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We present new high resolution imaging of a light-scattering dust ring and halo around the young star HD 35841. Using spectroscopic and polarimetric data from the Gemini Planet Imager in H-band (1.6 µm), we detect the highly inclined (i = 85 • ) ring of debris down to a projected separation of ∼12 au (∼0. 12) for the first time. Optical imaging from HST /STIS shows a smooth dust halo extending outward from the ring to >140 au (>1.4 ). We measure the ring's scattering phase function and polarization fraction over scattering angles of 22 • -125 • , showing a preference for forward scattering and a polarization fraction that peaks at ∼30% near the ansae. Modeling of the scattered-light disk indicates that the ring spans radii of ∼60-220 au, has a vertical thickness similar to that of other resolved dust rings, and contains grains as small as 1.5 µm in diameter. These models also suggest the grains have a low porosity, are more likely to consist of carbon than astrosilicates, and contain significant water ice. The halo has a surface brightness profile consistent with that expected from grains pushed by radiation pressure from the main ring onto highly eccentric but still bound orbits. We also briefly investigate arrangements of a possible inner disk component implied by our spectral energy distribution models, and speculate about the limitations of Mie theory for doing detailed analyses of debris disk dust populations.

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“…Both have high fractional infrared luminosities, well characterized by two dust populations at comparable blackbody temperatures and radii (∼40 au for the inner disk and ∼150 au for the outer disk), and with comparable dust masses ∼0.3M ⊕ in the outer disk (Hung et al 2015;Moór et al 2015b). Both exhibit a significant amount of CO gas (Hughes et al 2008;Moór et al 2015a).…”

Section: Similarities With Hd 131835mentioning

confidence: 99%

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

Choquet

Milli

Wahhaj

et al. 2017

ApJL

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We present the first scattered-light images of the debris disk around 49 Ceti, a ∼40 Myr A1 main-sequence star at 59 pc, famous for hosting two massive dust belts as well as large quantities of atomic and molecular gas. The outer disk is revealed in reprocessed archival Hubble Space Telescope NICMOS-F110W images, as well as new coronagraphic H-band images from the Very Large Telescope SPHERE instrument. The disk extends from 1 1 (65 au) to 4 6 (250 au) and is seen at an inclination of 73°, which refines previous measurements at lower angular resolution. We also report no companion detection larger than 3M Jup at projected separations beyond 20 au from the star (0 34). Comparison between the F110W and H-band images is consistent with a gray color of 49 Ceti's dust, indicating grains larger than 2 μm. Our photometric measurements indicate a scattering efficiency/infrared excess ratio of 0.2-0.4, relatively low compared to other characterized debris disks. We find that 49 Ceti presents morphological and scattering properties very similar to the gas-rich HD 131835 system. From our constraint on the disk inclination we find that the atomic gas previously detected in absorption must extend to the inner disk, and that the latter must be depleted of CO gas. Building on previous studies, we propose a schematic view of the system describing the dust and gas structure around 49 Ceti and hypothetical scenarios for the gas nature and origin.

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First Scattered-Light Image of the Debris Disk Around Hd 131835 With the Gemini Planet Imager

Cited by 61 publications

References 45 publications

Imaging [CI] around HD 131835: reinterpreting young debris discs with protoplanetary disc levels of CO gas as shielded secondary discs

Imaging [CI] around HD 131835: reinterpreting young debris discs with protoplanetary disc levels of CO gas as shielded secondary discs

Direct Imaging of the HD 35841 Debris Disk: A Polarized Dust Ring from Gemini Planet Imager and an Outer Halo from HST/STIS

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

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