The Gemini Planet Imager View of the HD 32297 Debris Disk

Authors

Gaspard Duchene, University of California, Berkeley
Malena Rice, Yale University
Justin Hom, School of Earth and Space Exploration
Joseph Zalesky, School of Earth and Space Exploration
Thomas M. Esposito, University of California, Berkeley
Maxwell A. Millar-Blanchaer, California Institute of Technology
Bin Ren, Johns Hopkins University
Paul Kalas, University of California, Berkeley
Michael P. Fitzgerald, University of California, Los Angeles
Pauline Arriaga, University of California, Los Angeles
Sebastian Bruzzone, Western University
Joanna Bulger, University Hawaii Institute for Astronomy
Christine H. Chen, Space Telescope Science Institute
Eugene Chiang, University of California, Berkeley
Tara Cotten, University of Georgia
Ian Czekala, University of California, Berkeley
Robert J. De Rosa, Kavli Institute for Particle Astrophysics and Cosmology
Ruobing Dong, University of Victoria
Zachary H. Draper, University of Victoria
Katherine B. Follette, Amherst College
James R. Graham, University of California, Berkeley
Li Wei Hung, University of California, Los Angeles
Ronald Lopez, University of California, Los Angeles
Bruce MacIntosh, Kavli Institute for Particle Astrophysics and Cosmology
Brenda C. Matthews, University of Victoria
et al, Various Institutions
Kimberly Ward-Duong, Amherst CollegeFollow

Document Type

Article

Publication Date

6-1-2020

Publication Title

Astronomical Journal

Abstract

We present new H-band scattered light images of the HD 32297 edge-on debris disk obtained with the Gemini Planet Imager. The disk is detected in total and polarized intensity down to a projected angular separation of 0.?15, or 20 au. On the other hand, the large-scale swept-back halo remains undetected, likely a consequence of its markedly blue color relative to the parent body belt. We analyze the curvature of the disk spine and estimate a radius of ?100 au for the parent body belt, smaller than past scattered light studies but consistent with thermal emission maps of the system. We employ three different flux-preserving post-processing methods to suppress the residual starlight and evaluate the surface brightness and polarization profile along the disk spine. Unlike past studies of the system, our high-fidelity images reveal the disk to be highly symmetric and devoid of morphological and surface brightness perturbations. We find the dust scattering properties of the system to be consistent with those observed in other debris disks, with the exception of HR 4796. Finally, we find no direct evidence for the presence of a planetary-mass object in the system.

Volume

159

Issue

6

DOI

10.3847/1538-3881/ab8881

ISSN

00046256

Rights

© 2020. The American Astronomical Society

Comments

Archived as published.

Recommended Citation

Duchene, Gaspard; Rice, Malena; Hom, Justin; Zalesky, Joseph; Esposito, Thomas M.; Millar-Blanchaer, Maxwell A.; Ren, Bin; Kalas, Paul; Fitzgerald, Michael P.; Arriaga, Pauline; Bruzzone, Sebastian; Bulger, Joanna; Chen, Christine H.; Chiang, Eugene; Cotten, Tara; Czekala, Ian; De Rosa, Robert J.; Dong, Ruobing; Draper, Zachary H.; Follette, Katherine B.; Graham, James R.; Hung, Li Wei; Lopez, Ronald; MacIntosh, Bruce; Matthews, Brenda C.; al, et; and Ward-Duong, Kimberly, "The Gemini Planet Imager View of the HD 32297 Debris Disk" (2020). Astronomy: Faculty Publications, Smith College, Northampton, MA.
https://scholarworks.smith.edu/ast_facpubs/108