Authors

Juan Sebastián Bruzzone, Western University
Stanimir Metchev, Western University
Gaspard Duchene, University of California, Berkeley
Maxwell A. Millar-Blanchaer, Jet Propulsion Laboratory
Ruobing Dong, University of Victoria
Thomas M. Esposito, University of California, Berkeley
Jason J. Wang, University of California, Berkeley
James R. Graham, University of California, Berkeley
Johan Mazoyer, Jet Propulsion Laboratory
Schuyler Wolff, Space Telescope Science Institute
S. Mark Ammons, Lawrence Livermore National Laboratory
Adam C. Schneider, School of Earth and Space Exploration
Alexandra Z. Greenbaum, University of Michigan, Ann Arbor
Brenda C. Matthews, University of Victoria
Pauline Arriaga, University of California, Los Angeles
Vanessa P. Bailey, Jet Propulsion Laboratory
Travis Barman, The University of Arizona
Joanna Bulger, National Institutes of Natural Sciences - National Astronomical Observatory of Japan
Jeffrey Chilcote, Stanford University
Tara Cotten, University of Georgia
Robert J. De Rosa, University of California, Berkeley
Rene Doyon, Institut de Recherche sur les Exoplanètes
Michael P. Fitzgerald, University of California, Los Angeles
Katherine B. Follette, Amherst College
Benjamin L. Gerard, University of Victoria
Stephen J. Goodsell, Gemini Observatory
Pascale Hibon, European Southern Observatory Santiago
Justin Hom, School of Earth and Space Exploration
Li Wei Hung, University of California, Los Angeles
Patrick Ingraham, Large Synoptic Survey Telescope
Paul Kalas, University of California, Berkeley
Quinn Konopacky, Center for Astrophysics & Space Sciences
Kimberly Ward-Duong, Amherst CollegeFollow
et al, Various Institutions

Document Type

Article

Publication Date

2-1-2020

Publication Title

Astronomical Journal

Abstract

We present the first polarimetric detection of the inner disk component around the pre-main-sequence B9.5 star HD 141569A. Gemini Planet Imager H-band (1.65 μm) polarimetric differential imaging reveals the highest signal-to-noise ratio detection of this ring yet attained and traces structure inward to 0.″25 (28 au at a distance of 111 pc). The radial polarized intensity image shows the east side of the disk, peaking in intensity at 0.″40 (44 au) and extending out to 0.″9 (100 au). There is a spiral arm-like enhancement to the south, reminiscent of the known spiral structures on the outer rings of the disk. The location of the spiral arm is coincident with 12CO J = 3-2 emission detected by ALMA and hints at a dynamically active inner circumstellar region. Our observations also show a portion of the middle dusty ring at ∼220 au known from previous observations of this system. We fit the polarized H-band emission with a continuum radiative transfer Mie model. Our best-fit model favors an optically thin disk with a minimum dust grain size close to the blowout size for this system, evidence of ongoing dust production in the inner reaches of the disk. The thermal emission from this model accounts for virtually all of the far-infrared and millimeter flux from the entire HD 141569A disk, in agreement with the lack of ALMA continuum and CO emission beyond ∼100 au. A remaining 8-30 μm thermal excess a factor of ∼2 above our model argues for an as-yet-unresolved warm innermost 5-15 au component of the disk.

Volume

159

Issue

2

DOI

10.3847/1538-3881/ab5d2e

ISSN

00046256

Rights

© 2020. The American Astronomical Society

Comments

Archived as published.

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