β PICTORIS' INNER DISK in POLARIZED LIGHT and NEW ORBITAL PARAMETERS for β PICTORIS b

Maxwell A. Millar-Blanchaer, James R. Graham, Laurent Pueyo, Paul Kalas, Rebekah I. Dawson, Jason Wang, Marshall D. Perrin, Dae Sik Moon, Bruce Macintosh, S. Mark Ammons, Travis Barman, Andrew Cardwell, Christine H. Chen, Eugene Chiang, Jeffrey Chilcote, Tara Cotten, Robert J.De Rosa, Zachary H. Draper, Jennifer Dunn, Gaspard DuchêneThomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Stephen J. Goodsell, Alexandra Z. Greenbaum, Markus Hartung, Pascale Hibon, Sasha Hinkley, Patrick Ingraham, Rebecca Jensen-Clem, Quinn Konopacky, James E. Larkin, Douglas Long, Jérôme Maire, Franck Marchis, Mark S. Marley, Christian Marois, Katie M. Morzinski, Eric L. Nielsen, David W. Palmer, Rebecca Oppenheimer, Lisa Poyneer, Abhijith Rajan, Fredrik T. Rantakyrö, Jean Baptiste Ruffio, Naru Sadakuni, Leslie Saddlemyer, Adam C. Schneider, Anand Sivaramakrishnan, Remi Soummer, Sandrine Thomas, Gautam Vasisht, David Vega, J. Kent Wallace, Kimberly Ward-Duong, Sloane J. Wiktorowicz, Schuyler G. Wolff

Research output: Contribution to journalArticle

48 Scopus citations

Abstract

We present H-band observations of β Pic with the Gemini Planet Imager's (GPI's) polarimetry mode that reveal the debris disk between ∼0.″3 (6 AU) and ∼1.″7 (33 AU), while simultaneously detecting β Pic b. The polarized disk image was fit with a dust density model combined with a Henyey-Greenstein scattering phase function. The best-fit model indicates a disk inclined to the line of sight () with a position angle (PA) (slightly offset from the main outer disk, ), that extends from an inner disk radius of to well outside GPI's field of view. In addition, we present an updated orbit for β Pic b based on new astrometric measurements taken in GPI's spectroscopic mode spanning 14 months. The planet has a semimajor axis of , with an eccentricity The PA of the ascending node is offset from both the outer main disk and the inner disk seen in the GPI image. The orbital fit constrains the stellar mass of β Pic to Dynamical sculpting by β Pic b cannot easily account for the following three aspects of the inferred disk properties: (1) the modeled inner radius of the disk is farther out than expected if caused by β Pic b; (2) the mutual inclination of the inner disk and β Pic b is when it is expected to be closer to zero; and (3) the aspect ratio of the disk () is larger than expected from interactions with β Pic b or self-stirring by the disk's parent bodies.

Original languageEnglish (US)
Article number18
JournalAstrophysical Journal
Volume811
Issue number1
DOIs
StatePublished - Sep 20 2015

Keywords

  • astrometry
  • planet-disk interactions
  • planets and satellites: individual (β Pic b)
  • techniques: polarimetric

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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    Millar-Blanchaer, M. A., Graham, J. R., Pueyo, L., Kalas, P., Dawson, R. I., Wang, J., Perrin, M. D., Moon, D. S., Macintosh, B., Ammons, S. M., Barman, T., Cardwell, A., Chen, C. H., Chiang, E., Chilcote, J., Cotten, T., Rosa, R. J. D., Draper, Z. H., Dunn, J., ... Wolff, S. G. (2015). β PICTORIS' INNER DISK in POLARIZED LIGHT and NEW ORBITAL PARAMETERS for β PICTORIS b. Astrophysical Journal, 811(1), [18]. https://doi.org/10.1088/0004-637X/811/1/18