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

Creators: 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, Leonardo; Wallack, Nicole; Williams, Jonathan; Zhu, Zhaohuan

Abstract

We present L'-band Keck/NIRC2 imaging and H-band Subaru/AO188+HiCIAO polarimetric observations of the CQ Tau disk with a new spiral arm. Apart from the spiral feature, our observations could not detect any companion candidates. We traced the spiral feature from the r²-scaled High-Contrast Coronographic Imager for Adaptive Optics (HiCIAO) polarimetric intensity image and the fitted result is used for forward modeling to reproduce the ADI-reduced NIRC2 image. We estimated the original surface brightness after throughput correction in the L' band to be ~126 mJy arcsec⁻² at most. We suggest that the grain temperature of the spiral may be heated up to ~200 K in order to explain both of the H- and L'-band results. The H-band emission at the location of the spiral originates from the scattering from the disk surface while both scattering and thermal emission may contribute to the L'-band emission. If the central star is only the light source of scattered light, the spiral emission at the L' band should be thermal emission. If an inner disk also acts as the light source, the scattered light and the thermal emission may equally contribute to the L'-band spiral structure.

Additional Information

© 2020 The American Astronomical Society. Received 2019 September 3; revised 2020 January 17; accepted 2020 January 23; published 2020 February 21. The authors would like to thank the anonymous referees for the constructive comments and suggestions to improve the quality of the paper. We wish to thank Mitsuhiko Honda for constructive comments to improve our discussions with the NIRC2 result. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. A part of this research is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatories of Japan. Based in part on data collected at Subaru telescope and obtained from the SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01404.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This research has made use of NASA's Astrophysics Data System Bibliographic Services. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in Ochsenbein et al. (2000). T.U. acknowledges JSPS overseas research fellowship. This work was supported by MEXT/JSPS KAKENHI grant Nos. 15H02063, 17K05399, 18H05442, 19H00703, 19H05089, and 19K03932. Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). The material is based upon work supported by NASA under award No. 80NSSC19K0294. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (ERC grant Agreement no. 337569) and Horizon 2020 Research and Innovation Program (grant agreement No. 819155), and from the Wallonia-Brussels Federation (grant for Concerted Research Actions). V.C. acknowledges funding from the Australian Research Council via DP180104235. O.A. acknowledges funding from FRS-FNRS. J.B. acknowledges support by NASA through the NASA Hubble Fellowship grant #HST-HF2-51427.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The authors wish to acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.

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