An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO
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Author
Rameau, Julien
Follette, Katherine B.

Pueyo, Laurent
Marois, Christian

Macintosh, Bruce

Millar-Blanchaer, Maxwell A.

Wang, Jason J.

Vega, David
Doyon, René
Lafrenière, David

Nielsen, Eric L.

Bailey, Vanessa
Chilcote, Jeffrey

Close, Laird M.

Esposito, Thomas M.

Males, Jared R.

Metchev, Stanimir A.

Morzinski, Katie M.

Ruffio, Jean-Baptiste

Wolff, Schuyler

Ammons, S. Mark

Barman, Travis S.

Bulger, Joanna
Cotten, Tara

De Rosa, Robert J.

Duchêne, Gaspard

Fitzgerald, Michael P.

Goodsell, Stephen J.

Graham, James R.
Greenbaum, Alexandra Z.
Hibon, Pascale

Hung, Li-Wei
Ingraham, Patrick
Kalas, Paul
Konopacky, Quinn

Larkin, James E.

Maire, Jérôme
Marchis, Franck

Oppenheimer, Rebecca

Palmer, David
Patience, Jennifer
Perrin, Marshall

Poyneer, Lisa
Rajan, Abhijith

Rantakyrö, Fredrik T.

Marley, Mark S.

Savransky, Dmitry

Schneider, Adam C.
Sivaramakrishnan, Anand

Song, Inseok

Soummer, Remi

Thomas, Sandrine
Wallace, J. Kent
Ward-Duong, Kimberly

Wiktorowicz, Sloane

Affiliation
Univ Arizona, Steward ObservIssue Date
2017-05-08Keywords
instrumentation: adaptive opticsplanet-disk interactions
planetary systems
stars: individual (HD 100546)
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IOP PUBLISHING LTDCitation
An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO 2017, 153 (6):244 The Astronomical JournalJournal
The Astronomical JournalRights
© 2017. 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
We present H band spectroscopic and H alpha photometric observations of HD 100546 obtained with the Gemini Planet Imager and the Magellan Visible AO camera. We detect H band emission at the location of the protoplanet HD 100546 b, but show that the choice of data processing parameters strongly affects the morphology of this source. It appears point-like in some aggressive reductions, but rejoins an extended disk structure in the majority of the others. Furthermore, we demonstrate that this emission appears stationary on a timescale of 4.6 years, inconsistent at the 2 sigma level with a Keplerian clockwise orbit at 59 au in the disk plane. The H band spectrum of the emission is inconsistent with any type of low effective temperature object or accreting protoplanetary disk. It strongly suggests a scattered-light origin, as this is consistent with the spectrum of the star and the spectra extracted at other locations in the disk. A nondetection at the 5 sigma level of HD 100546 b in differential H alpha imaging places an upper limit, assuming the protoplanet lies in a gap free of extinction, on the accretion luminosity of 1.7 x 10(-4) L-circle dot and M(M) over dot < 6.3 x 10(-7) M-Jup(2) yr(-1) for 1 R-Jup. These limits are comparable to the accretion luminosity and accretion rate of T-Tauri stars or LkCa 15 b. Taken together, these lines of evidence suggest that the H band source at the location of HD 100546 b is not emitted by a planetary photosphere or an accreting circumplanetary disk but is a disk feature enhanced by the point-spread function subtraction process. This non-detection is consistent with the non-detection in the K. band reported in an earlier study but does not exclude the possibility that HD 100546 b is deeply embedded.ISSN
1538-3881Version
Final published versionSponsors
DPAC; Fonds de Recherche du Quebec; NASA through the Sagan Fellowship Program; NSF [AST-1411868, AST-141378]; NASA [NNX14AJ80G, NNX15AD95G, NNX16AD44G]; U.S. Department of Energy by the Lawrence Livermore National Laboratory [DE-AC52-07NA27344]Additional Links
http://stacks.iop.org/1538-3881/153/i=6/a=244?key=crossref.53b93305b0aad19f17777d8bf48e49fcae974a485f413a2113503eed53cd6c53
10.3847/1538-3881/aa6cae