Imaging the 44 AU Kuiper Belt-analogue debris ring around HD 141569A with GPI polarimetry. (arXiv:1911.11814v1 [astro-ph.SR])

Imaging the 44 AU Kuiper Belt-analogue debris ring around HD 141569A with GPI polarimetry. (arXiv:1911.11814v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bruzzone_J/0/1/0/all/0/1">J. S. Bruzzone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Metchev_S/0/1/0/all/0/1">S. Metchev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duchene_G/0/1/0/all/0/1">G. Duchene</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Millar_Blanchaer_M/0/1/0/all/0/1">M. A. Millar-Blanchaer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_R/0/1/0/all/0/1">R. Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_J/0/1/0/all/0/1">J. J. Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graham_J/0/1/0/all/0/1">J. R. Graham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mazoyer_J/0/1/0/all/0/1">J. Mazoyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolff_S/0/1/0/all/0/1">S. Wolff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ammons_S/0/1/0/all/0/1">S. M. Ammons</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_A/0/1/0/all/0/1">A. C. Schneider</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greenbaum_A/0/1/0/all/0/1">A. Z. Greenbaum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matthews_B/0/1/0/all/0/1">B. C. Matthews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arriaga_P/0/1/0/all/0/1">P. Arriaga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bailey_V/0/1/0/all/0/1">V. P. Bailey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barman_T/0/1/0/all/0/1">T. Barman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulger_J/0/1/0/all/0/1">J. Bulger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chilcote_J/0/1/0/all/0/1">J. Chilcote</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cotten_T/0/1/0/all/0/1">T. Cotten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosa_R/0/1/0/all/0/1">R. J. De Rosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doyon_R/0/1/0/all/0/1">R. Doyon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fitzgerald_M/0/1/0/all/0/1">M. P. Fitzgerald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Follette_K/0/1/0/all/0/1">K. B. Follette</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerard_B/0/1/0/all/0/1">B. L. Gerard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goodsell_S/0/1/0/all/0/1">S. J. Goodsell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hibon_P/0/1/0/all/0/1">P. Hibon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hom_J/0/1/0/all/0/1">J. Hom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hung_L/0/1/0/all/0/1">L.-W. Hung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ingraham_P/0/1/0/all/0/1">P. Ingraham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kalas_P/0/1/0/all/0/1">P. Kalas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Konopacky_Q/0/1/0/all/0/1">Q. Konopacky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Larkin_J/0/1/0/all/0/1">J. E. Larkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macintosh_B/0/1/0/all/0/1">B. Macintosh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maire_J/0/1/0/all/0/1">J. Maire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marchis_F/0/1/0/all/0/1">F. Marchis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marois_C/0/1/0/all/0/1">C. Marois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morzinski_K/0/1/0/all/0/1">K. M. Morzinski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nielsen_E/0/1/0/all/0/1">E. L. Nielsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oppenheimer_R/0/1/0/all/0/1">R. Oppenheimer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palmer_D/0/1/0/all/0/1">D. Palmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patel_R/0/1/0/all/0/1">R. Patel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patience_J/0/1/0/all/0/1">J. Patience</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perrin_M/0/1/0/all/0/1">M. Perrin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poyneer_L/0/1/0/all/0/1">L. Poyneer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pueyo_L/0/1/0/all/0/1">L. Pueyo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rajan_A/0/1/0/all/0/1">A. Rajan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rameau_J/0/1/0/all/0/1">J. Rameau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rantakyro_F/0/1/0/all/0/1">F. T. Rantakyro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Savransky_D/0/1/0/all/0/1">D. Savransky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sivaramakrishnan_A/0/1/0/all/0/1">A. Sivaramakrishnan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Song_I/0/1/0/all/0/1">I. Song</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soummer_R/0/1/0/all/0/1">R. Soummer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thomas_S/0/1/0/all/0/1">S. Thomas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wallace_J/0/1/0/all/0/1">J. K. Wallace</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ward_Duong_K/0/1/0/all/0/1">K. Ward-Duong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wiktorowicz_S/0/1/0/all/0/1">S. Wiktorowicz</a>

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 micron) polarimetric differential imaging reveals the highest
signal-to-noise ratio detection of this ring yet attained and traces structure
inwards 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 blow-out size for this system: evidence of on-going 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 micron thermal excess a factor of ~2
above our model argues for a yet-unresolved warm innermost 5-15 AU component of
the disk.

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