Multi-epoch Direct Imaging and Time-variable Scattered Light Morphology of the HD 163296 Protoplanetary Disk
Year: 2019
Type: article
Abstract: We present H -band polarized scattered light imagery and JHK high-contrast spectroscopy of the protoplanetary disk around HD 163296 observed with the High-Contrast Coronographic Imager for Adaptive Optics (HiCIAO) and Subaru Coronagraphic Extreme Adaptive Optics (SCExAO)/Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) instruments at Subaru Observatory. The polarimetric imagery resolve a broken ring structure surrounding HD 163296 that peaks at a distance along the major axis of 0 65 (66 au) and extends out to 0 98 (100 au) along the major axis. Our 2011 H -band data exhibit clear axisymmetry, with the NW and SE side of the disk exhibiting similar intensities. Our data are clearly different from 2016 epoch H -band observations of the Very Large Telescope (VLT)/Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE), which found a strong 2.7 × asymmetry between the NW and SE side of the disk. Collectively, these results indicate the presence of time-variable, non-azimuthally symmetric illumination of the outer disk. While our SCExAO/CHARIS data are sensitive enough to recover the planet candidate identified from NIRC2 in the thermal infrared (IR), we fail to detect an object with JHK brightness nominally consistent with this object. This suggests that the candidate is either fainter in JHK bands than model predictions, possibly due to extinction from the disk or atmospheric dust/clouds, or that it is an artifact of the data set/data processing, such as a residual speckle or partially subtracted disk feature. Assuming standard hot-start evolutionary models and a system age of 5 Myr, we set new, direct mass limits for the inner (outer) Atacama Large Millimeter/submillimeter Array (ALMA)-predicted protoplanet candidate along the major (minor) disk axis of of 1.5 (2) M J .
Source: The Astrophysical Journal
Authors: Evan A. Rich, John P. Wisniewski, Thayne Currie, Misato Fukagawa, Carol A. Grady, Michael L. Sitko, Monika Pikhartova, Jun Hashimoto, Lyu Abe, Wolfgang Brandner, Timothy D. Brandt, Joseph C. Carson, Jeffrey Chilcote, Ruobing Dong, Markus Feldt, Miwa Goto, Tyler Groff, Olivier Guyon, Yutaka Hayano, Masahiko Hayashi, Saeko S. Hayashi, Thomas Henning, Klaus W. Hodapp, Miki Ishii, Masanori Iye, Markus Janson, Nemanja Jovanovic, Ryo Kandori, Jeremy Kasdin, Gillian R. Knapp, Tomoyuki Kudo, Nobuhiko Kusakabe, Masayuki Kuzuhara, Jungmi Kwon, Julien Lozi, Frantz Martinache, Taro Matsuo, Satoshi Mayama, Michael W. McElwain, Shoken Miyama, Jun-Ichi Morino, Amaya Moro-Martin, Takao Nakagawa, Tetsuo Nishimura, Tae-Soo Pyo, Eugene Serabyn, Hiroshi Suto, Ray W. Russel, Ryuji Suzuki, Michihiro Takami, Naruhisa Takato, Hiroshi Terada, Christian Thalmann, Edwin L. Turner, Taichi Uyama, Kevin R. Wagner, Makoto Watanabe, Toru Yamada, Hideki Takami, Tomonori Usuda, Motohide Tamura
Institutions: University of Oklahoma, Ames Research Center, National Institutes of Natural Sciences, Eureka Scientific, National Astronomical Observatory of Japan, The University of Osaka, Goddard Space Flight Center, Space Science Institute, University of Cincinnati, Astrobiology Center, Centre National de la Recherche Scientifique, Lagrange Laboratory, Observatoire de la Côte d’Azur, Université Nice Sophia Antipolis, Max Planck Institute for Astronomy, Institute for Advanced Study, College of Charleston, University of Notre Dame, University of Victoria, Ludwig-Maximilians-Universität München, University of Arizona, University of Hawaii System, University of Hawaii at Hilo, Stockholm University, AlbaNova, California Institute of Technology, Princeton University, The University of Tokyo, Kyoto University, The Graduate University for Advanced Studies, SOKENDAI, Hiroshima University, Space Telescope Science Institute, Johns Hopkins University, Japan Aerospace Exploration Agency, Institute of Space and Astronautical Science, Jet Propulsion Laboratory, The Aerospace Corporation, Institute of Astronomy and Astrophysics, Academia Sinica, ETH Zurich, Hokkaido University, Tohoku University
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: bronze
Awards: G2419081464, Imaging habitable zone planets with Subaru Telescope and TMT, High-Resolution Circularly Polarized Light Observations and Ice Experiments: Toward Understanding the Origin of the Homochirality of Life, TRANSITIONAL DISKS ARE AN INTERMEDIATE STAGE BETWEEN GAS-RICH PROTOPLANETARY DISKS AND OLDER DEBRIS DISKS/YOUNG PLANETARY SYSTEMS. THEY HAVE ATTRACTED RECENT INTEREST AS HIGH RESOLUTION HIGH CONTRAST IMAGING FACILITIES HAVE BEGUN TO RESOLVE INDIRECT AND DIRECT SIGNATURES OF RECENTLY FORMED PLANETARY BODIES IN THESE SYSTEMS ACROSS A BROAD RANGE OF WAVELENGTHS (NEAR-IR MID-IR MM). REGIONS IN DISKS WHERE WE EXPECT GIANT PLANETS TO HAVE RECENTLY FORMED CAN BE IDENTIFIED BY COMPARISON OF SUB-MM IMAGERY WITH NIR HIGH CONTRAST IMAGERY. PLANETS HAVE RECENTLY BEEN DIRECTLY IMAGED IN A FEW SYSTEMS. IF THE TRANSITIONAL DISK PHASE IS A TYPICAL STEP IN CLEARING OF DISKS AND MOST OF THESE HAVE STRUCTURE CONSISTENT WITH DISK-PLANET INTERACTIONS GIANT PLANETS SHOULD BE RELATIVELY COMMON. IMAGING SURVEYS OF NEARBY MOVING GROUPS FIND A ~2% OVERALL GIANT PLANET FREQUENCY IN THE 5-150 AU RANGE. HOWEVER THE FREQUENCY OFGIANT PLANETS ON WIDE ORBITS MIGHT BE SIGNIFICANTLY HIGHER IN SYSTEMS WITH CIRCUMSTELLAR DISKS AND THERE COULD BE SIGNIFICANT DIFFERENCES IN FREQUENCY WITH HOST STAR AND DISK PROPERTIES. FOR EXAMPLE AMONG THE 8 BETA PICTORIS MOVING GROUP A - EARLY F STARS 2 PLANETS ARE ALREADY KNOWN WHILE 2 OTHER SYSTEMS HOST TRANSITING EXOCOMETS SIMILAR TO THOSE SEEN IN SPECTRA OF BETA PIC AND USED TO PREDICT THE EXISTENCE OF BETA PICTORIS B. THESE FINDINGS SUGGEST THAT THE GIANT PLANET DETECTION RATE IS>25% AND MAY REACH 50%. MOREOVER PREVIOUS EXOPLANET SURVEYS COULD REACH ONLY BODIES WITH MASSES>5 MJUP IN TRANSITIONAL DISKS AND AT INNER WORKING ANGLES (IWA)>0.15" (21 AU AT 140 PC). A NEW ERA OF HIGH CONTRAST IMAGING HAS BEGUN WITH EXTREME ADAPTIVE OPTICS AND ADVANCED CORONAGRAPHS THATACHIEVE 3X SMALLER IWAS AND AN ORDER OF MAGNITUDE HIGHER CONTRASTS WITH RESPECT TO THEIR HOST STARS. WE CAN NOW PROBE THE GIANT EXOPLANET FREQUENCY DISTRIBUTION IN FORMING PLANETARY SYSTEMS ON SCALES COMPARABLE TO OUR OUTER SOLAR SYSTEM. WE PROPOSE TO BUILD UP THE SEEDS SURVEY AND CONDUCT A 3 PART STUDY TO: 1) LOCATE LIKELY REGIONS OF RECENT PLANET FORMATION IN TRANSITIONAL DISKS; 2) CONDUCT AN IMAGING SEARCH FOR PLANETS IN THESE TRANSITIONAL DISKS WITH EVIDENCE OF RECENT PLANET FORMATION; 3) CONDUCT AN IMAGING PLANET SEARCH FOR PLANETS IN YOUNG WISE-SELECTED DEBRIS DISKS WE WILL UTILIZE EXTREME AO NIR IMAGERY BOTH FROM SUBARU AND GEMINI AS WELL AS HIGH-RESOLUTION MM IMAGERY FROM ALMA. OUR SURVEY WILL ALLOW US TO IDENTIFY PLANETS IN TRANSITIONAL DISKS WHICH ARE STILL ACCRETING MATERIAL AND TO TEST WHETHER YOUNG DEBRIS DISK PLANETS HAVE A SIMILAR SPATIAL DISTRIBUTION TO THOSE SEEN IN TRANSITIONAL DISKS IMPLYING IN SITU FORMATION AT LARGE DISTANCES FROM THEIR HOST STARS. OUR INVESTIGATION LEVERAGES A STRONG EXISTING INTERNATIONAL SET OF COLLABORATORS THE LARGEST EXTANT HIGH-CONTRAST IMAGING STUDY OF TRANSITIONAL DISKS (I.E SEEDS) AND SIGNIFICANT AMOUNT OF APPROVED OBSERVING TIME (SUBARU GEMINI ALMA SMA). THIS WORK IS DIRECTLY APPLICABLE TO THE GOALS OF THE EXOPLANET RESEARCH PROGRAM AND SPECIFICALLY THE OBJECTIVE OF DETECTION AND CHARACTERIZATION OF PLANETS AND PLANETARY SYSTEMS OUTSIDE OF OUR SOLAR SYSTEM., Earth-like Planet Search on the Subaru Telescope, G8020484511
OpenAlex ID: W2901092239