Dynamical Evidence of a Spiral Arm–driving Planet in the MWC 758 Protoplanetary Disk

Ren, Bin; Dong, Ruobing; Holstein, R. van; Ruffio, Jean Baptiste; Calvin, Benjamin; Girard, J.; Benisty, M.; Boccaletti, A.; Espósito, Thomas M.; Choquet, Élodie; Mawet, Dimitri; Pueyo, Laurent; Stolker, T.; Chiang, Eugene; Boer, J. de; Debes, John H.; Garufi, A.; Grady, C. A.; Hines, Dean C.; Maire, Anne-Lise; Ménard, F.; Millar-Blanchaer, M.; Perrin, Marshall D.; Poteet, C. A.; Schneider, Glenn

doi:10.3847/2041-8213/aba43e

Cited by 40 publications

(48 citation statements)

References 55 publications

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“…To measure the motion of the S1 spiral, we follow the procedure in Ren et al (2020). Specifically, in the surface density distribution map on the disk plane, we first fit Gaussian profiles to the radial profile at each angular position to obtain the peak position for the arm, then use dummy variables as proxies to obtain morphological parameters under polynomial description for the arm, and simultaneously quantify the arm motion rates under two hypotheses (i.e., either planet-driven motion or local Keplerian motion; Ren et al 2020). In the planet-driven scenario, the entire spiral moves as a solid body, and the spiral pattern motion traces the orbital motion of the driver; in the local Keplerian motion scenario, the motion of the spiral is faster when its location is closer to the star.…”

Section: Spiralsmentioning

confidence: 99%

“…We analyze the deprojected surface density maps on the disk plane to minimize stellar illumination and projection effects. We fit S1 in polar coordinates with p-degree polynomials as in Ren et al (2020), and obtain minimized Akaike and Schwarz information criteria (AIC and SIC) at p = 1, which corresponds to a linear description of an arm in polar coordinates in the solid body motion scenario.…”

Section: Spiralsmentioning

confidence: 99%

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A Layered Debris Disk around M Star TWA 7 in Scattered Light

Ren

Choquet

Perrin

et al. 2021

ApJ

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We have obtained Hubble Space Telescope (HST) coronagraphic observations of the circumstellar disk around M star TWA 7 using the Space Telescope Imaging Spectrograph (STIS) instrument in visible light. Together with archival observations, including HST/NICMOS using the F160W filter and Very Large Telescope/SPHERE at the H-band in polarized light, we investigate the system in scattered light. By studying this nearly face-on system using geometric disk models and Henyey-Greenstein phase functions, we report a new discovery of a tertiary ring and a clump. We identify a layered architecture: three rings, a spiral, and an ≈150 au 2 elliptical clump. The most extended ring peaks at 28 au, and the other components are on its outskirts. Our point-source detection-limit calculations demonstrate the necessity of disk modeling in imaging fainter planets. Morphologically, we witness a clockwise spiral motion, and the motion pattern is consistent with both solid body motion and local Keplerian motion; we also observe underdensity regions for the secondary ring that might result from mean-motion resonance or moving shadows: both call for re-observations to determine their nature. Comparing multi-instrument observations, we obtain blue STIS-NICMOS color, a STIS-SPHERE radial distribution peak difference for the tertiary ring, and a high SPHERE-NICMOS polarization fraction; these aspects indicate that TWA 7 could retain small dust particles. By viewing the debris disk around M star TWA 7 at a nearly face-on vantage point, our study allows for the understanding of such disks in scattered light in both system architecture and dust property.

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Section: Spiralsmentioning

confidence: 99%

Section: Spiralsmentioning

confidence: 99%

A Layered Debris Disk around M Star TWA 7 in Scattered Light

Ren

Choquet

Perrin

et al. 2021

ApJ

Self Cite

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“…From continued observation of such disks, the movement of the features can be measured, which can then be used to discriminate between their two likely causes: yet-unseen companions and gravitational instability. 38 While total intensity observations might also enable such investigations, it would be much more challenging given that the amount and location of disk attenuation will likely vary between epochs. Being free of significant attenuation, PDI data will significantly strengthen such investigations.…”

Section: Discussionmentioning

confidence: 99%

High-contrast integral field spectropolarimetry of planet-forming disks with SCExAO/CHARIS

Lawson

Currie

Wisniewski

et al. 2021

Techniques and Instrumentation for Detection of Exoplanets X

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We describe a new high-contrast imaging capability well suited for studying planet-forming disks: near-infrared (NIR) high-contrast spectropolarimetric imaging with the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) integral field spectrograph (IFS). The advent of extreme adaptive optics (AO) systems, like SCExAO, has enabled recovery of planet-mass companions at the expected locations of gas-giant formation in young disks alongside disk structures (such as gaps or spirals) that may indicate protoplanet formation. In combination with SCExAO, the CHARIS IFS in polarimetry mode allows characterization of these systems at wavelengths spanning the NIR J, H, and K bands (1.1 − 2.4 µm, R ∼ 20) and at angular separations as small as 0. 04. By comparing the resulting images with forward-modeled scattered light or 3D radiative-transfer models, the likely origins of any observed features can be assessed. Utilization of swift optimization algorithms, such as differential evolution (DE), to identify model parameters that best reproduce the observations allows plausible disk geometries to be explored efficiently. The recent addition of CHARIS's unique integral field spectropolarimetry mode has further facilitated the study of planet-forming disks -aiding in the confirmation of candidate protoplanets, the diagnosis of disk structures, and the characterization of dust grain populations. We summarize preliminary results for two young planet-forming disk systems based on observations with the novel integral field spectropolarimetry mode for SCExAO/CHARIS.

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“…Considering that planets are born in protoplanetary disks, the observed structures have been frequently linked with the presence of planets forming within the disk (e.g., Muto et al 2012;Pohl et al 2015;Dong et al 2018a;Calcino et al 2020;Ren et al 2020). These planets perturb the disks via gravitational interactions, and these perturbations can cause the formation of spirals.…”

Section: Introductionmentioning

confidence: 99%

A multiwavelength analysis of the spiral arms in the protoplanetary disk around WaOph 6

Brown-Sevilla

Keppler

Barraza-Alfaro

et al. 2021

A&A

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Context. In recent years, protoplanetary disks with spiral structures have been detected in scattered light, millimeter continuum, and CO gas emission. The mechanisms causing these structures are still under debate. A popular scenario to drive the spiral arms is the one of a planet perturbing the material in the disk. However, if the disk is massive, gravitational instability isusually the favored explanation. Multiwavelength studies could be helpful to distinguish between the two scenarios. So far, only a handful of disks with spiral arms have been observed in both scattered light and millimeter continuum. Aims. We aim to perform an in-depth characterization of the protoplanetary disk morphology around WaOph 6 analyzing data obtained at different wavelengths, as well as to investigate the origin of the spiral features in the disk. Methods. We present the first near-infrared polarimetric observations of WaOph 6 obtained with SPHERE at the VLT and compare them to archival millimeter continuum ALMA observations. We traced the spiral features in both data sets and estimated the respective pitch angles. We discuss the different scenarios that can give rise to the spiral arms in WaOph 6. We tested the planetary perturber hypothesis by performing hydrodynamical and radiative transfer simulations to compare them with scattered light and millimeter continuum observations. Results. We confirm that the spiral structure is present in our polarized scattered light H-band observationsof WaOph 6, making it the youngest disk with spiral arms detected at these wavelengths. From the comparison to the millimeter ALMA-DSHARP observations, we confirm that the disk is flared. We explore the possibility of a massive planetary perturber driving the spiral arms by running hydrodynamical and radiative transfer simulations, and we find that a planet of minimum 10 MJup outside of the observed spiral structure is able to drive spiral arms that resemble the ones in the observations. We derive detection limits from our SPHERE observations and get estimates of the planet’s contrast from different evolutionary models. Conclusions. Up to now, no spiral arms had been observed in scattered light in disks around K and/or M stars with ages <1 Myr. Future observations of WaOph 6 could allow us to test theoretical predictions for planet evolutionary models, as well as give us more insightinto the mechanisms driving the spiral arms.

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Dynamical Evidence of a Spiral Arm–driving Planet in the MWC 758 Protoplanetary Disk

Cited by 40 publications

References 55 publications

A Layered Debris Disk around M Star TWA 7 in Scattered Light

A Layered Debris Disk around M Star TWA 7 in Scattered Light

High-contrast integral field spectropolarimetry of planet-forming disks with SCExAO/CHARIS

A multiwavelength analysis of the spiral arms in the protoplanetary disk around WaOph 6

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