SCExAO/CHARIS Near-infrared Integral Field Spectroscopy of the HD 15115 Debris Disk
Kellen Lawson, Thayne Currie, John P. Wisniewski, Motohide Tamura, Glenn Schneider, J.‐C. Augereau, Timothy D. Brandt, Olivier Guyon, N. Jeremy Kasdin, Tyler D. Groff, Julien Lozi, Jeffrey Chilcote, K. W. Hodapp, Nemanja Jovanović, Frantz Martinache, Nour Skaf, Eiji Akiyama, Thomas Henning, G. R. Knapp, Jungmi Kwon, Satoshi Mayama, Michael W. McElwain, Michael L. Sitko, R. Asensio-Torres, Taichi Uyama, Kevin Wagner
Abstract
Abstract We present new, near-infrared (1.1–2.4 μ m) high-contrast imaging of the debris disk around HD 15115 with the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system coupled with the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS). The SCExAO/CHARIS resolves the disk down to ρ ∼ 0.″2 ( r proj ∼ 10 au), a factor of ∼3–5 smaller than previous recent studies. We derive a disk position angle of PA ∼ 279.°4–280.°5 and an inclination of i ∼ 85.°3–86.2.°. While recent SPHERE/IRDIS imagery of the system could suggest a significantly misaligned two-ring disk geometry, CHARIS imagery does not reveal conclusive evidence for this hypothesis. Moreover, optimizing models of both one- and two-ring geometries using differential evolution, we find that a single ring having a Hong-like scattering phase function matches the data equally well within the CHARIS field of view ( ρ ≲ 1″). The disk’s asymmetry, well evidenced at larger separations, is also recovered; the west side of the disk appears, on average, around 0.4 mag brighter across the CHARIS bandpass between 0.″25 and 1″. Comparing Space Telescope Imaging Spectrograph (STIS) 50CCD optical photometry (2000–10500 Å) with CHARIS near-infrared photometry, we find a red (STIS/50CCD−CHARIS broadband) color for both sides of the disk throughout the 0.″4–1″ region of overlap, in contrast to the blue color reported at similar wavelengths for regions exterior to ∼2″. Further, this color may suggest a smaller minimum grain size than previously estimated at larger separations. Finally, we provide constraints on planetary companions and discuss possible mechanisms for the observed inner disk flux asymmetry and color.