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Young and dynamically active planetary systems can form disks of debris thatare easier to image than the planets themselves. The morphology and evolutionof these disks can help to infer the properties of the putative planetsresponsible for generating and shaping the debris structures. We presentintegral field spectroscopy and dual-band imaging from VLT/SPHERE ($1.0 - 1.7\mu m$) of the debris disk around the young F2V/F3V star HD 115600. We aim to1) characterize the geometry and composition of the debris ring, 2) search forthermal emission of young giant planets, and 3) in the absence of detectedplanets, to refine the inferred properties of plausible planets around HD115600 to prepare future attempts to detect them. Using a different dustscattering model (ZODIPIC) than in the discovery paper (Henyey-Greenstein) tomodel the disk geometry, we find $a_0 = 46 \pm 2$ au for the disk's centralradius and offsets $\Delta \alpha$, $\Delta \delta$ = $ -1.0 \pm 0.5, 0.5 \pm0.5$ au. This offset is smaller than previously found, suggesting that unseenplanets of lower masses could be sculpting the disk. Spectroscopy of the diskin Y-J bands with SPHERE shows reddish color, which becomes neutral or slightlyblue in H band seen with GPI, broadly consistent with a mixed bulk diskcomposition of processed organics and water ice. While our observed fieldcontains numerous background objects at wide separations, no exoplanet has beendirectly observed to a mass sensitivity limit of $2-3(5-7) M_{\rm J}$ between aprojected separation of 40 and 200 au for hot (cold)-start models.

the astronomical journal

VLT/SPHERE Multi-Wavelength High-Contrast Imaging of the HD 115600  Debris Disk: New Constraints on the Dust Geometry and the Presence of Young  Giant Planets