Near-infrared Imaging of a Spiral in the CQ Tau Disk

Uyama, Taichi; Muto, Takayuki; Mawet, Dimitri; Christiaens, Valentin; Hashimoto, Jun; Kudo, Tomoyuki; Kuzuhara, Masayuki; Ruane, Garreth; Beichman, Charles; Absil, Olivier; Akiyama, Eiji; Bae, Jaehan; Bottom, Michael; Choquet, Élodie; Currie, Thayne; Dong, Ruobing; Follette, Katherine B.; Fukagawa, Misato; Guidi, Greta; Huby, Elsa; Kwon, Jungmi; Mayama, Satoshi; Meshkat, Tiffany; Reggiani, Maddalena; Ricci, Luca; Serabyn, Eugene; Tamura, Motohide; Testi, L.; Wallack, Nicole L.; Williams, Jonathan P.; Zhu, Zhaohuan

doi:10.3847/1538-3881/ab7006

Cited by 22 publications

(33 citation statements)

References 65 publications

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“…In addition to Ubeira Gabellini et al (2019) we clearly note a drop in the peak intensity of all isotopologues and integrated intensity of C 18 O by roughly 35-60% (with respect to the peak) in the northwest and southeast parts of the disc along the minor axis (symmetric pair of dips), which becomes especially prominent in the C 18 O data and colocates with a possible under-brightness in near-infrared (NIR) scattered light (see Fig. 4 of Uyama et al 2020). Similar to the NIR under-brightness, the drop in peak intensity appears to be more pronounced (relative to the peak ∼7-12% deeper dip) on the southeast side of the disc (compare also Sect.…”

Section: Integrated Intensity and Brightness Temperature Mapsmentioning

confidence: 67%

“…The authors performed 3D hydrodynamical simulations which suggest a hidden planet of several M J located at ∼20 au as a possible cause for the observed gas and dust depleted regions. Even though such a planet could not be detected in combined Keck/NIRC2 and Subaru/AO188+HiCIAO observations of CQ Tau (Uyama et al 2020), due to a lack of contrast (compare their Fig. 3), the data reveal the presence of a small spiral seen in small dust grains on scales of 30-60 au that might be induced by a companion candidate.…”

Section: Targetmentioning

confidence: 75%

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A highly non-Keplerian protoplanetary disc

Wölfer

Facchini

Kurtovic

et al. 2021

A&A

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Context. In recent years high-angular-resolution observations have revealed that circumstellar discs appear in a variety of shapes with diverse substructures being ubiquitous. This has given rise to the question of whether these substructures are triggered by planet–disc interactions. Besides direct imaging, one of the most promising methods to distinguish between different disc-shaping mechanisms is to study the kinematics of the gas disc. In particular, the deviations of the rotation profile from Keplerian velocity can be used to probe perturbations in the gas pressure profile that may be caused by embedded (proto-) planets. Aims. In this paper we aim to analyse the gas brightness temperature and kinematics of the transitional disc around the intermediate-mass star CQ Tau in order to resolve and characterise substructure in the gas caused by possible perturbers. Methods. For our analysis we used spatially resolved ALMA observations of the three CO isotopologues 12CO, 13CO, and C18O (J = 2−1) from the disc around CQ Tau. We further extracted robust line centroids for each channel map and fitted a number of Keplerian disc models to the velocity field. Results. The gas kinematics of the CQ Tau disc present non-Keplerian features, showing bent and twisted iso-velocity curves in 12CO and 13CO. Significant spiral structures are detected between ~10 and 180 au in both the brightness temperature and the rotation velocity of 12CO after subtraction of an azimuthally symmetric model, which may be tracing planet–disc interactions with an embedded planet or low-mass companion. We identify three spirals, two in the brightness temperature and one in the velocity residuals, spanning a large azimuth and radial extent. The brightness temperature spirals are morphologically connected to spirals observed in near-infrared scattered light in the same disc, indicating a common origin. Together with the observed large dust and gas cavity, these spiral structures support the hypothesis of a massive embedded companion in the CQ Tau disc.

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Section: Integrated Intensity and Brightness Temperature Mapsmentioning

confidence: 67%

Section: Targetmentioning

confidence: 75%

A highly non-Keplerian protoplanetary disc

Wölfer

Facchini

Kurtovic

et al. 2021

A&A

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“…The bright extended feature at position angle (PA) between ∼ 170 • and ∼ 270 • is clearly co-located with the spiral detected by SPHERE ('Spiral 1' in Muro-Arena et al 2020) and this detection is one of several cases that the spiral feature is clearly resolved in L -band (e.g. HD 142527, HD 100546, MWC 758, and CQ Tau; Rameau et al 2012;Currie et al 2015;Reggiani et al 2018;Uyama et al 2020a). To test the potential contamination of the disk feature around the reference stars in L band, we checked the archival VLT/SPHERE H-band polarimetric data set of WaOph6 taken on UT 2018 June 22 (ESO GTO program 1100.C-0481(Q), PI: J.-L. Beuzit).…”

Section: Rdimentioning

confidence: 73%

Early High-contrast Imaging Results with Keck/NIRC2-PWFS: The SR 21 Disk

Uyama

Ren

Mawet

et al. 2020

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High-contrast imaging of exoplanets and protoplanetary disks depends on wavefront sensing and correction made by adaptive optics instruments. Classically, wavefront sensing has been conducted at optical wavelengths, which made high-contrast imaging of red targets such as M-type stars or extincted T Tauri stars challenging. Keck/NIRC2 has combined near-infrared (NIR) detector technology with the pyramid wavefront sensor (PWFS). With this new module we observed SR 21, a young star that is brighter at NIR wavelengths than at optical wavelengths. Compared with the archival data of SR 21 taken with the optical wavefront sensing we achieved ∼20% better Strehl ratio in similar natural seeing conditions. Further post-processing utilizing angular differential imaging and reference-star differential imaging confirmed the spiral feature reported by the VLT/SPHERE polarimetric observation, which is the first detection of the SR 21 spiral in total intensity at L band. We also compared the contrast limit of our result (10 −4 at 0. 4 and 2 × 10 −5 at 1. 0) with the archival data that were taken with optical wavefront sensing and confirmed the improvement, particularly at ≤ 0. 5. Our observation demonstrates that the NIR PWFS improves AO performance and will provide more opportunities for red targets in the future.

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“…Although their model showed good agreement with polarimetric data in the J band, it had some differences between GPI-based JH-band total intensity and H-band polarized intensity. Another intriguing feature in the HD 34700 A disk is its spiral features: previous high angular resolution observations have indicated a variety of morphology in disks at various evolutionary stages (e.g., AB Aur, SAO 206462, MWC 758, HD 100453, HD 100546, HD 142527, Elias 2-27, CQ Tau, GG Tau;Hashimoto et al 2011;Muto et al 2012;Grady et al 2013;Avenhaus et al 2014;Currie et al 2015;Wagner et al 2015;Pérez et al 2016;Keppler et al 2020;Uyama et al 2020). Among these disks this object has the largest number of spirals in a disk, the mechanism for which is still unclear.…”

Section: Introductionmentioning

confidence: 99%

SCExAO/CHARIS High-contrast Imaging of Spirals and Darkening Features in the HD 34700 A Protoplanetary Disk

Uyama

Currie

Christiaens

et al. 2020

ApJ

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We present Subaru/SCExAO+Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) broadband (JHK-band) integral field spectroscopy of HD 34700 A. CHARIS data recover HD 34700 A's disk ring and confirm multiple spirals discovered by Monnier et al. We set limits on substellar companions of ∼12 M Jup at 0 3 (in the ring gap) and ∼5 M Jup at 0 75 (outside the ring). The data reveal darkening effects on the ring and spiral, although we do not identify the origin of each feature such as shadows or physical features related to the outer spirals. Geometric albedos converted from the surface brightness suggest a greater scale height and/or prominently abundant submicron dust at position angles between ∼45°and 90°. Spiral fitting resulted in very large pitch angles (∼30°-50°); a stellar flyby of HD 34700 B or infall from a possible envelope is perhaps a reasonable scenario to explain the large pitch angles.

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Near-infrared Imaging of a Spiral in the CQ Tau Disk

Cited by 22 publications

References 65 publications

A highly non-Keplerian protoplanetary disc

A highly non-Keplerian protoplanetary disc

Early High-contrast Imaging Results with Keck/NIRC2-PWFS: The SR 21 Disk

SCExAO/CHARIS High-contrast Imaging of Spirals and Darkening Features in the HD 34700 A Protoplanetary Disk

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