A Decade of MWC 758 Disk Images: Where Are the Spiral-arm-driving Planets?
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Final Published Version
Author
Ren, BinDong, Ruobing
Esposito, Thomas M.

Pueyo, Laurent
Debes, John H.

Poteet, Charles A.
Choquet, Élodie
Benisty, Myriam
Chiang, Eugene

Grady, Carol A.
Hines, Dean C.

Schneider, Glenn

Soummer, Rémi
Affiliation
Univ Arizona, Steward Observ, Tucson, AZ 85719 USAUniv Arizona, Steward Observ, Tucson, AZ 85721 USA
Issue Date
2018-04-10
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IOP PUBLISHING LTDCitation
Ren, B., Dong, R., Esposito, T. M., Pueyo, L., Debes, J. H., Poteet, C. A., . . . Soummer, R. (2018). A Decade of MWC 758 Disk Images: Where Are the Spiral-arm-driving Planets? The Astrophysical Journal, 857(1). doi:10.3847/2041-8213/aab7f5Journal
ASTROPHYSICAL JOURNAL LETTERSRights
© 2018. The American Astronomical Society. All rights reserved.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
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 corotate 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 year 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 758ʼs 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 degrees(+3.3 degrees)(-0.6 degrees) yr(-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.ISSN
2041-82132041-8205
Version
Final published versionSponsors
State of Maryland grant; NASA through Hubble Fellowship by STScI [ST-HF2-51355]; AURA, Inc. [NAS5-26555]; NASA [HST-AR-12652, NNX15AD95G/NEXSS, NNX15AC89G, HST-GO-11136, HST-GO-13855, HST-GO-13331]; NSF [AST-1518332]; STScI Director's Discretionary Research funds; AURA under NASA [NAS5-26555]; NASA's Science Mission DirectorateAdditional Links
http://stacks.iop.org/2041-8205/857/i=1/a=L9?key=crossref.6a43045a3c4c3b47a40dc1f9511415d3ae974a485f413a2113503eed53cd6c53
10.3847/2041-8213/aab7f5