Discovery of an Edge-on Circumstellar Debris Disk around BD+45° 598: A Newly Identified Member of the β Pictoris Moving Group

Hinkley, Sasha; Matthews, Elisabeth C.; Lefèvre, Charlène; Lestrade, J. F.; Kennedy, Grant M.; Mawet, Dimitri; Stapelfeldt, K.; Ray, Shrishmoy; Mamajek, Eric E.; Bowler, Brendan P.; Wilner, David J.; Williams, Jonathan P.; Ansdell, Megan; Wyatt, M. C.; Lau, Alexis; Phillips, Mark; Fernández, Jorge Fernández; Gagné, Jonathan; Bubb, Emma J.; Sutlieff, Ben J.; Wilson, Thomas J. G.; Matthews, Brenda C.; Ngo, Henry; Piskorz, Danielle; Crepp, Justin R.; Gonzalez, Erica; Mann, Andrew W.; Mace, Gregory N.

doi:10.3847/1538-4357/abec6e

Cited by 18 publications

(18 citation statements)

References 84 publications

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“…Other debris disk candidates that are bright and close to edge-on include the disk around β Pictoris (e.g., Smith & Terrile 1984;Matrà et al 2019;Janson et al 2021) and the recently discovered disk around BD+45°598 (Hinkley et al 2021). If these candidates could be observed at both high resolution, necessary to resolve their vertical structures, and at multiple wavelengths such that the relationship between observed wavelengths and disk aspect ratio is significant, then their collisional cascades could be parameterized in a similar fashion to the process described in this work.…”

Section: Future Workmentioning

confidence: 99%

Multiwavelength Vertical Structure in the AU Mic Debris Disk: Characterizing the Collisional Cascade

Vizgan

Hughes

Carter

et al. 2022

ApJ

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Debris disks are scaled-up analogs of the Kuiper Belt in which dust is generated by collisions between planetesimals. In the collisional cascade model of debris disks, the dust lost to radiation pressure and winds is constantly replenished by grinding collisions between planetesimals. The model assumes that collisions are destructive and involve large velocities; this assumption has not been tested beyond our solar system. We present 0.″25 (≈2.4 au) resolution observations of the λ = 450 μm dust continuum emission from the debris disk around the nearby M dwarf AU Microscopii with the Atacama Large Millimeter/submillimeter Array. We use parametric models to describe the disk structure, and a Monte Carlo Markov Chain (MCMC) algorithm to explore the posterior distributions of the model parameters; we fit the structure of the disk to both our data and archival λ = 1.3 mm data (Daley et al. 2019), from which we obtain two aspect ratio measurements at 1.3 mm (h 1300 = 0.025 − 0.002 + 0.008 ) and at 450 μm (h 450 = 0.019 − 0.001 + 0.006 ), as well as the grain-size distribution index q = 3.03 ± 0.02. Contextualizing our aspect ratio measurements within the modeling framework laid out in Pan & Schlichting (2012), we derive a power-law index of velocity dispersion as a function of grain size p = 0.28 ± 0.06 for the AU Mic debris disk. This result implies that smaller bodies are more easily disrupted than larger bodies by collisions, which is inconsistent with the strength regime usually assumed for such small bodies. Possible explanations for this discrepancy are discussed.

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Section: Future Workmentioning

confidence: 99%

Multiwavelength Vertical Structure in the AU Mic Debris Disk: Characterizing the Collisional Cascade

Vizgan

Hughes

Carter

et al. 2022

ApJ

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“…We implement a Markov-chain Monte Carlo (MCMC) (Foreman-Mackey et al 2013) analysis to fit for the six orbital parameters and the mass of planet b. MCMC has been extensively used to do orbit fitting, e.g. first by Hou et al (2012) and more recently by Blunt et al (2019), Nowak et al (2020), Hinkley et al (2021) and Wang et al (2021). As discussed in Sec.…”

Section: Mcmc Resultsmentioning

confidence: 99%

Constraining the Orbit and Mass of epsilon Eridani b with Radial Velocities, Hipparcos IAD-Gaia DR2 Astrometry, and Multi-epoch Vortex Coronagraphy Upper Limits

Llop-Sayson,

Wang,

Ruffio

et al. 2021

Preprint

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Eridani is a young planetary system hosting a complex multi-belt debris disk and a confirmed Jupiter-like planet orbiting at 3.48 AU from its host star. Its age and architecture are thus reminiscent of the early Solar System. The most recent study of Mawet et al. (2019), which combined radial velocity (RV) data and Ms-band direct imaging upper limits, started to constrain the planet's orbital parameters and mass, but are still affected by large error bars and degeneracies. Here we make use of the most recent data compilation from three different techniques to further refine Eridani b's properties: RVs, absolute astrometry measurements from the Hipparcos and Gaia missions, and new Keck/NIRC2 Ms-band vortex coronagraph images. We combine this data in a Bayesian framework. We find a new mass, M b = 0.66 +0.12 −0.09 M Jup , and inclination, i = 77.95 •+28.50 −21.06 , with at least a factor 2 improvement over previous uncertainties. We also report updated constraints on the longitude of the ascending node, the argument of the periastron, and the time of periastron passage. With these updated parameters, we can better predict the position of the planet at any past and future epoch, which can greatly help define the strategy and planning of future observations and with subsequent data analysis. In particular, these results can assist the search for a direct detection with JWST and the Nancy Grace Roman Space Telescope's coronagraph instrument (CGI).

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“…To build the noise map, we compute the standard deviation per pixel in a small ring centered to the star. To take account for the correlation between pixels we add to the standard deviation an inflation term as described in Hinkley et al (2021). This inflation term considers the spatial correlation of the PSF through the instrumental FWHM (40 mas or 3.3 pixels) and the radial elongation of the speckles due to the filter's bandwidth.…”

Section: Noise Map and Uncertaintiesmentioning

confidence: 99%

Morphology of the gas-rich debris disk around HD 121617 with SPHERE observations in polarized light

Perrot¹,

Olofsson²,

Kral³

et al. 2023

Preprint

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Context. Debris disks are the signposts of collisionally eroding planetesimal circumstellar belts, whose study can put important constraints on the structure of extrasolar planetary systems. The best constraints on the morphology of disks are often obtained from spatially resolved observations in scattered light. Here, we investigate the young (∼16 Myr) bright gas-rich debris disk around HD 121617. Aims. We use new scattered-light observations with VLT/SPHERE to characterize the morphology and the dust properties of this disk. From these properties we can then derive constraints on the physical and dynamical environment of this system, for which significant amounts of gas have been detected. Methods. The disk morphology is constrained by linear-polarimetric observations in the J band. Based on our modeling results and archival photometry, we also model the SED to put constraints on the total dust mass and the dust size distribution. We explore different scenarios that could explain these new constraints. Results. We present the first resolved image in scattered light of the debris disk HD 121617. We fit the morphology of the disk, finding a semi-major axis of 78.3 ± 0.2 au, an inclination of 43.1 ± 0.2 • and a position angle of the major axis with respect to north, of 239.8 ± 0.3 • , compatible with the previous continuum and CO detection with ALMA. Our analysis shows that the disk has a very sharp inner edge, possibly sculpted by a yet-undetected planet or gas drag. While less sharp, its outer edge is steeper than expected for unperturbed disks, which could also be due to a planet or gas drag, but future observations probing the system farther from the main belt would help explore this further. The SED analysis leads to a dust mass of 0.21 ± 0.02 M ⊕ and a minimum grain size of 0.87 ± 0.12 µm, smaller than the blowout size by radiation pressure, which is not unexpected for very bright collisionally active disks.

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Discovery of an Edge-on Circumstellar Debris Disk around BD+45° 598: A Newly Identified Member of the β Pictoris Moving Group

Cited by 18 publications

References 84 publications

Multiwavelength Vertical Structure in the AU Mic Debris Disk: Characterizing the Collisional Cascade

Multiwavelength Vertical Structure in the AU Mic Debris Disk: Characterizing the Collisional Cascade

Constraining the Orbit and Mass of epsilon Eridani b with Radial Velocities, Hipparcos IAD-Gaia DR2 Astrometry, and Multi-epoch Vortex Coronagraphy Upper Limits

Morphology of the gas-rich debris disk around HD 121617 with SPHERE observations in polarized light

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