![]() ![]() However, the Δ( K s − H 2O) color is consistent with grains with little to no ice (0%–5% by mass). An apparent deficit of scattered light at 3.08 μm relative to the bracketing wavelengths ( K s and ) is evocative of ice absorption at the disk surface layer. We find strong morphological differences between the bands, including asymmetries consistent with the observed spiral arms within 100 au in. By applying reference differential imaging point-spread function subtraction, we detect the disk at high signal-to-noise ratios in all three bands. A comparison of the surface brightness at K s (2.16 μm), H 2O narrowband (3.08 μm), and (3.7 μm) allows us to probe the presence of icy grains in this (pre)transitional disk environment. We present near-infrared Large Binocular Telescope LMIRCam imagery of the disk around the Herbig Ae/Be star AB Aurigae. Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, B-3001, Leuven, BelgiumĬenter for Adaptive Optics, UC Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USAĭepartment of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA 95064, USA Steward Observatory, Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA School of Physics & Astronomy, Monash University, Clayton VIC 3800, Australiaĭepartment of Terrestrial Magnetism, Carnegie Institution for Science, Washington, DC 20015, USAĮureka Scientific, Oakland, CA 96002, USA Núcleo Milenio de Formación Planetaria (NPF), Chile LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, F-92195 Meudon, France ![]() Université Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA of Physics and Astronomy, Amherst College, Amherst, MA 01003, USAĭepartamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chileĭepartment of Astronomy, University of California, Berkeley, CA 94720, USA ![]()
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