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dc.contributor.authorRameau, Julien
dc.contributor.authorFollette, Katherine B.
dc.contributor.authorPueyo, Laurent
dc.contributor.authorMarois, Christian
dc.contributor.authorMacintosh, Bruce
dc.contributor.authorMillar-Blanchaer, Maxwell A.
dc.contributor.authorWang, Jason J.
dc.contributor.authorVega, David
dc.contributor.authorDoyon, René
dc.contributor.authorLafrenière, David
dc.contributor.authorNielsen, Eric L.
dc.contributor.authorBailey, Vanessa
dc.contributor.authorChilcote, Jeffrey
dc.contributor.authorClose, Laird M.
dc.contributor.authorEsposito, Thomas M.
dc.contributor.authorMales, Jared R.
dc.contributor.authorMetchev, Stanimir A.
dc.contributor.authorMorzinski, Katie M.
dc.contributor.authorRuffio, Jean-Baptiste
dc.contributor.authorWolff, Schuyler
dc.contributor.authorAmmons, S. Mark
dc.contributor.authorBarman, Travis S.
dc.contributor.authorBulger, Joanna
dc.contributor.authorCotten, Tara
dc.contributor.authorDe Rosa, Robert J.
dc.contributor.authorDuchêne, Gaspard
dc.contributor.authorFitzgerald, Michael P.
dc.contributor.authorGoodsell, Stephen J.
dc.contributor.authorGraham, James R.
dc.contributor.authorGreenbaum, Alexandra Z.
dc.contributor.authorHibon, Pascale
dc.contributor.authorHung, Li-Wei
dc.contributor.authorIngraham, Patrick
dc.contributor.authorKalas, Paul
dc.contributor.authorKonopacky, Quinn
dc.contributor.authorLarkin, James E.
dc.contributor.authorMaire, Jérôme
dc.contributor.authorMarchis, Franck
dc.contributor.authorOppenheimer, Rebecca
dc.contributor.authorPalmer, David
dc.contributor.authorPatience, Jennifer
dc.contributor.authorPerrin, Marshall
dc.contributor.authorPoyneer, Lisa
dc.contributor.authorRajan, Abhijith
dc.contributor.authorRantakyrö, Fredrik T.
dc.contributor.authorMarley, Mark S.
dc.contributor.authorSavransky, Dmitry
dc.contributor.authorSchneider, Adam C.
dc.contributor.authorSivaramakrishnan, Anand
dc.contributor.authorSong, Inseok
dc.contributor.authorSoummer, Remi
dc.contributor.authorThomas, Sandrine
dc.contributor.authorWallace, J. Kent
dc.contributor.authorWard-Duong, Kimberly
dc.contributor.authorWiktorowicz, Sloane
dc.date.accessioned2017-06-19T23:36:41Z
dc.date.available2017-06-19T23:36:41Z
dc.date.issued2017-05-08
dc.identifier.citationAn Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO 2017, 153 (6):244 The Astronomical Journalen
dc.identifier.issn1538-3881
dc.identifier.doi10.3847/1538-3881/aa6cae
dc.identifier.urihttp://hdl.handle.net/10150/624214
dc.description.abstractWe 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.
dc.description.sponsorshipDPAC; 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]en
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/1538-3881/153/i=6/a=244?key=crossref.53b93305b0aad19f17777d8bf48e49fcen
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectinstrumentation: adaptive opticsen
dc.subjectplanet-disk interactionsen
dc.subjectplanetary systemsen
dc.subjectstars: individual (HD 100546)en
dc.titleAn Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAOen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalThe Astronomical Journalen
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
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-05-18T04:13:12Z
html.description.abstractWe 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.


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