Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 857, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/2041-8213/aab7f5
Keywords
protoplanetary disks; stars: imaging; stars: individual (MWC 758)
Categories
Funding
- 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 Directorate
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1518332] Funding Source: National Science Foundation
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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. 758's 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 3 sigma 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 3 sigma 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.
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