Imaging an 80 au radius dust ring around the F5V star HD 157587

Maxwell A. Millar-Blanchaer, Jason J. Wang, Paul Kalas, James R. Graham, Gaspard Duchêne, Eric L. Nielsen, Marshall Perrin, Dae Sik Moon, Deborah Padgett, Stanimir Metchev, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Sebastian Bruzzone, Joanna Bulger, Christine H. Chen, Jeffrey Chilcote, Tara Cotten, Robert J.De Rosa, Rene DoyonZachary H. Draper, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Benjamin L. Gerard, Alexandra Z. Greenbaum, Pascale Hibon, Sasha Hinkley, Li Wei Hung, Patrick Ingraham, Mara Johnson-Groh, Quinn Konopacky, James E. Larkin, Bruce MacIntosh, Jérôme Maire, Franck Marchis, Mark S. Marley, Christian Marois, Brenda C. Matthews, Rebecca Oppenheimer, David Palmer, Jennifer Patience, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, David Vega, J. Kent Wallace, Kimberly Ward-Duong, Sloane Wiktorowicz, Schuyler Wolff

Research output: Contribution to journalArticlepeer-review

16 Scopus citations

Abstract

We present H-band near-infrared polarimetric imaging observations of the F5V star HD 157587 obtained with the Gemini Planet Imager (GPI) that reveal the debris disk as a bright ring structure at a separation of ∼80-100 au. The new GPI data complement recent Hubble Space Telescope/STIS observations that show the disk extending out to over 500 au. The GPI image displays a strong asymmetry along the projected minor axis as well as a fainter asymmetry along the projected major axis. We associate the minor and major axis asymmetries with polarized forward scattering and a possible stellocentric offset, respectively. To constrain the disk geometry, we fit two separate disk models to the polarized image, each using a different scattering phase function. Both models favor a disk inclination of ∼70° and a 1.5 ± 0.6 au stellar offset in the plane of the sky along the projected major axis of the disk. We find that the stellar offset in the disk plane, perpendicular to the projected major axis is degenerate with the form of the scattering phase function and remains poorly constrained. The disk is not recovered in total intensity due in part to strong adaptive optics residuals, but we recover three point sources. Considering the system's proximity to the galactic plane and the point sources' positions relative to the disk, we consider it likely that they are background objects and unrelated to the disk's offset from the star.

Original languageEnglish (US)
Article number128
JournalAstronomical Journal
Volume152
Issue number5
DOIs
StatePublished - Nov 2016

Keywords

  • planet-disk interactions
  • stars: individual (HD 157587)
  • techniques: polarimetric

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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