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Journal Articles The Astronomical Journal Year : 2017

An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO

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Julien Rameau
  • Function : Author
Katherine B. Follette
  • Function : Author
Laurent Pueyo
  • Function : Author
Christian Marois
Bruce Macintosh
Maxwell Millar-Blanchaer
Jason J. Wang
  • Function : Author
David Vega
  • Function : Author
René Doyon
David Lafrenière
Eric L. Nielsen
  • Function : Author
Vanessa Bailey
  • Function : Author
Jeffrey K. Chilcote
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Laird M. Close
  • Function : Author
Thomas M. Esposito
  • Function : Author
Jared R. Males
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Stanimir Metchev
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Katie M. Morzinski
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Jean-Baptiste Ruffio
  • Function : Author
Schuyler G. Wolff
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S. M. Ammons
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Travis S. Barman
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Joanna Bulger
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Tara Cotten
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Robert J. de Rosa
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Michael P. Fitzgerald
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Stephen Goodsell
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James R. Graham
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Alexandra Z. Greenbaum
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Pascale Hibon
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Li-Wei Hung
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Patrick Ingraham
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Paul Kalas
Quinn Konopacky
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James E. Larkin
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Jérôme Maire
  • Function : Author
Franck Marchis
Rebecca Oppenheimer
  • Function : Author
David Palmer
  • Function : Author
Jennifer Patience
  • Function : Author
Marshall D. Perrin
Lisa Poyneer
  • Function : Author
Abhijith Rajan
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Fredrik T. Rantakyrö
  • Function : Author
Mark S. Marley
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Dmitry Savransky
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Adam C. Schneider
  • Function : Author
Anand Sivaramakrishnan
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Inseok Song
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Remi Soummer
  • Function : Author
Sandrine Thomas
  • Function : Author
J. Kent Wallace
  • Function : Author
Kimberly Ward-Duong
  • Function : Author
Sloane Wiktorowicz

Abstract

We present H band spectroscopic and Hα 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 2σ 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 non-detection at the 5σ level of HD 100546 b in differential Hα imaging places an upper limit, assuming the protoplanet lies in a gap free of extinction, on the accretion luminosity of 1.7 × 10-4 L and M\dot{M}< 6.3× {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.

Dates and versions

insu-03692510 , version 1 (09-06-2022)

Identifiers

Cite

Julien Rameau, Katherine B. Follette, Laurent Pueyo, Christian Marois, Bruce Macintosh, et al.. An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO. The Astronomical Journal, 2017, 153, ⟨10.3847/1538-3881/aa6cae⟩. ⟨insu-03692510⟩
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