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dc.contributor.authorWagner, Kevin
dc.contributor.authorFollete, Katherine B.
dc.contributor.authorClose, Laird M.
dc.contributor.authorApai, Dániel
dc.contributor.authorGibbs, Aidan
dc.contributor.authorKeppler, Miriam
dc.contributor.authorMüller, André
dc.contributor.authorHenning, Thomas
dc.contributor.authorKasper, Markus
dc.contributor.authorWu, Ya-Lin
dc.contributor.authorLong, Joseph
dc.contributor.authorMales, Jared
dc.contributor.authorMorzinski, Katie
dc.contributor.authorMcClure, Melissa
dc.date.accessioned2018-12-05T20:18:30Z
dc.date.available2018-12-05T20:18:30Z
dc.date.issued2018-08-10
dc.identifier.citationKevin Wagner et al 2018 ApJL 863 L8en_US
dc.identifier.issn2041-8213
dc.identifier.doi10.3847/2041-8213/aad695
dc.identifier.urihttp://hdl.handle.net/10150/631103
dc.description.abstractPDS 70b is a recently discovered and directly imaged exoplanet within the wide (greater than or similar to 40 au) cavity around PDS 70. Ongoing accretion onto the central star suggests that accretion onto PDS 70b may also be ongoing. We present the first high-contrast images at H alpha (656 nm) and nearby continuum (643 nm) of PDS 70 utilizing the MagAO system. The combination of these filters allows for the accretion rate of the young planet to be inferred, as hot infalling hydrogen gas will emit strongly at H alpha over the optical continuum. We detected a source in H alpha at the position of PDS 70b on two sequential nights in 2018 May, for which we establish a false positive probability of <0.1%. We conclude that PDS 70b is a young, actively accreting planet. We utilize the H alpha line luminosity to derive a mass accretion rate of (M) over dot = 10(-8 +/- 1) M-Jup yr(-1), where the large uncertainty is primarily due to the unknown amount of optical extinction from the circumstellar and circumplanetary disks. PDS 70b represents the second case of an accreting planet interior to a disk gap, and is among the early examples of a planet observed during its formation.en_US
dc.description.sponsorshipNASA's Science Mission Directorate; NASA Exoplanets Research Program [NNX16AD44G]; DFG priority program [SPP 1992, MU 4172/1-1]; NSF ATI [1506818]; NSF AAG program [1615408]; NASA XRP program [80NSSC18K0441]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/2041-8205/863/i=1/a=L8?key=crossref.0e80dcceb3e83e0b3fe3b60896cfbd26en_US
dc.rights© 2018. The American Astronomical Society. All rights reserved.en_US
dc.subjectplanet-disk interactionsen_US
dc.subjectplanets and satellites: detectionen_US
dc.subjectplanets and satellites: formationen_US
dc.subjectstars: pre-main sequenceen_US
dc.titleMagellan Adaptive Optics Imaging of PDS 70: Measuring the Mass Accretion Rate of a Young Giant Planet within a Gapped Disken_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben_US
dc.identifier.journalASTROPHYSICAL JOURNAL LETTERSen_US
dc.description.collectioninformationThis 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.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal
dc.source.volume863
dc.source.issue1
dc.source.beginpageL8
refterms.dateFOA2018-12-05T20:18:30Z


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