Constraining the Movement of the Spiral Features and the Locations of Planetary Bodies Within the Ab Aur System

Lomax, Jamie R.; Wisniewski, John P.; Grady, C. A.; McElwain, Michael W.; Hashimoto, Jun; Kudo, Tomoyuki; Kusakabe, Nobuhiko; Okamoto, Y.; Fukagawa, Misato; Abe, Lyu; Brandner, W.; Brandt, Timothy D.; Carson, J.; Currie, Thayne; Egner, Sebastian; Feldt, M.; Goto, Miwa; Guyon, Olivier; Hayano, Yutaka; Hayashi, Masahiko; Hayashi, Saeko S.; Henning, Thomas; Hodapp, Klaus W.; Inoue, Akio; Ishii, Miki; Iye, Masanori; Janson, Markus; Kandori, Ryo; Knapp, G. R.; Kuzuhara, Masayuki; Kwon, Jungmi; Matsuo, Taro; Mayama, Satoshi; Miyama, Shoken M.; Momose, Munetake; Morino, Jun-Ichi; Moro‐Martín, Amaya; Nishimura, Tetsuo; Pyo, Tae‐Soo; Schneider, Glenn; Serabyn, Eugene; Sitko, Michael L.; Suenaga, Takuya; Shimada, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro; Miki, Takami; Takato, Naruhisa; Terada, Hiroshi; Thalmann, Christian; Tomono, Daigo; Turner, Edwin L.; Watanabe, Makoto; Yamada, Tōru; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide

doi:10.3847/0004-637x/828/1/2

Cited by 7 publications

(4 citation statements)

References 34 publications

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“…We do achieve a good fit at longer wavelengths, suggesting that our model is accurate for the outer disk. There is also a residual envelope of material around this system, although it is unclear if this contributes significantly to the mid-IR flux (Lomax et al 2016;van der Marel et al 2016).…”

Section: Appendixmentioning

confidence: 99%

Protoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurus

Ballering

Eisner

2019

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Measuring the masses of protoplanetary disks is crucial for understanding their planet-forming potential. Typically, dust masses are derived from (sub-)millimeter flux density measurements plus assumptions for the opacity, temperature, and optical depth of the dust. Here we use radiative transfer models to quantify the validity of these assumptions with the aim of improving the accuracy of disk dust mass measurements. We first carry out a controlled exploration of disk parameter space. We find that the disk temperature is a strong function of disk size, while the optical depth depends on both disk size and dust mass. The millimeter-wavelength spectral index can be significantly shallower than the naive expectation due to a combination of optical depth and deviations from the Rayleigh-Jeans regime. We fit radiative transfer models to the spectral energy distributions (SEDs) of 132 disks in the Taurus-Auriga region using a Markov chain Monte Carlo approach. We used all available data to produce the most complete SEDs used in any extant modeling study. We perform the fitting twice: first with unconstrained disk sizes and again imposing the disk size-brightness relation inferred for sources in Taurus. This constraint generally forces the disks to be smaller, warmer, and more optically thick. From both sets of fits, we find disks to be ∼1-5 times more massive than when derived using (sub-)millimeter measurements and common assumptions. With the uncertainties derived from our model fitting, the previously measured dust mass-stellar mass correlation is present in our study but only significant at the 2σ level.

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Section: Appendixmentioning

confidence: 99%

Protoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurus

Ballering

Eisner

2019

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“…Companion-driven arms co-rotate with their driver. Therefore, by measuring their pattern speed, the orbital period, thus semi-major axis, of their companion can be constrained (e.g., Lomax et al 2016). We perform such an exercise for the spiral arm system MWC 758, taking advantage of observations of the arms over a decade-long baseline established by a 2005 HST/NICMOS observation and 2015/2017 VLT/SPHERE and Keck/NIRC2 observations.…”

Section: Introductionmentioning

confidence: 99%

A Decade of MWC 758 Disk Images: Where Are the Spiral-arm-driving Planets?

Ren

Dong

Espósito

et al. 2018

ApJL

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Large-scale spiral arms have been revealed in scattered light images of a few protoplanetary disks. Theoretical models suggest that such arms may be driven by and co-rotate with giant planets, which has called for remarkable observational efforts to look for them. By examining the rotation of the spiral arms for the MWC 758 system over a 10-yr timescale, we are able to provide dynamical constraints on the locations of their perturbers. We present reprocessed Hubble Space Telescope (HST)/NICMOS F110W observations of the target in 2005, and the new Keck/NIRC2 L -band observations in 2017. MWC 758's two well-known spiral arms are revealed in the NICMOS archive at the earliest observational epoch. With additional Very Large Telescope (VLT)/SPHERE data, our joint analysis leads to a pattern speed of 0. • 6 +3. • 3 −0.• 6yr −1 at 3σ for the two major spiral arms. If the two arms are induced by a perturber on a near-circular orbit, its best fit orbit is at 89 au (0. 59), with a 3σ lower limit of 30 au (0. 20). This finding is consistent with the simulation prediction of the location of an arm-driving planet for the two major arms in the system.

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“…For the first model, we use the "ground-truth" disk model contained in the simulated data-referred to hereafter as the "ideal" case. This should be regarded as an absolute upper limit on the accuracy of corrections derived this way; for similarly complicated disks, modeling results do not typically approach this accuracy and often do not attempt to reproduce nonaxisymmetric structures at all (e.g., Lomax et al 2016;Betti et al 2022). The second model instead emulates a more realistic modeling result, consisting of a simple two-ring disk model without any spiral structures but which generally reproduces the bulk of the disk's shape and brightnessreferred to hereafter as the "realistic" case.…”

Section: Pcrdi Throughputmentioning

confidence: 99%

Constrained Reference Star Differential Imaging: Enabling High-fidelity Imagery of Highly Structured Circumstellar Disks ^*

Lawson

Currie

Wisniewski

et al. 2022

ApJL

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High-contrast imaging presents us with the opportunity to study circumstellar disks and the planets still embedded within them, providing key insights into the formation and evolution of planetary systems. However, the postprocessing techniques that are often needed to suppress stellar halo light typically result in significant and variable loss of circumstellar light, even when using relatively conservative approaches like reference star differential imaging (RDI). We introduce “constrained reference star differential imaging” (constrained RDI), a new class of RDI point-spread-function (PSF) subtraction techniques for systems with circumstellar disks. Constrained RDI utilizes either high-resolution polarized-intensity (PI) images or disk models to severely limit or even eliminate the signal loss due to oversubtraction that is common to RDI. We demonstrate the ability of constrained RDI utilizing polarimetric data to yield an oversubtraction-free detection of the AB Aurigae protoplanetary disk in total intensity. PI-constrained RDI allows us to decisively recover the spectral signature of the confirmed, recently discovered protoplanet, AB Aurigae b. We further demonstrate that constrained RDI can be a powerful analysis tool for soon-to-be-acquired James Webb Space Telescope coronagraphic imaging of disks. In both cases, constrained RDI provides analysis-ready products that enable more detailed studies of disks and more robust verification of embedded exoplanets.

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Constraining the Movement of the Spiral Features and the Locations of Planetary Bodies Within the Ab Aur System

Cited by 7 publications

References 34 publications

Protoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurus

Protoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurus

A Decade of MWC 758 Disk Images: Where Are the Spiral-arm-driving Planets?

Constrained Reference Star Differential Imaging: Enabling High-fidelity Imagery of Highly Structured Circumstellar Disks ^*

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Constraining the Movement of the Spiral Features and the Locations of Planetary Bodies Within the Ab Aur System

Cited by 7 publications

References 34 publications

Protoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurus

Protoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurus

A Decade of MWC 758 Disk Images: Where Are the Spiral-arm-driving Planets?

Constrained Reference Star Differential Imaging: Enabling High-fidelity Imagery of Highly Structured Circumstellar Disks *

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Product

Resources

About

Constrained Reference Star Differential Imaging: Enabling High-fidelity Imagery of Highly Structured Circumstellar Disks ^*