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The Gray Needle: Large Grains in the HD 15115 Debris Disk from LBT/PISCES/Ks and LBTI/LMIRcam/L′ Adaptive Optics Imaging

  • Authors: Timothy J. Rodigas, Philip M. Hinz, Jarron Leisenring, Vidhya Vaitheeswaran, Andrew J. Skemer, Michael Skrutskie, Kate Y. L. Su, Vanessa Bailey, Glenn Schneider, Laird Close, Filippo Mannucci, Simone Esposito, Carmelo Arcidiacono, Enrico Pinna, Javier Argomedo, Guido Agapito, Daniel Apai, Giuseppe Bono, Kostantina Boutsia, Runa Briguglio, Guido Brusa, Lorenzo Busoni, Giovanni Cresci, Thayne Currie, Silvano Desidera, Josh Eisner, Renato Falomo, Luca Fini, Kate Follette, Adriano Fontana, Peter Garnavich, Raffaele Gratton, Richard Green, Juan Carlos Guerra, J. M. Hill, William F. Hoffmann, Terry J. Jones, Megan Krejny, Craig Kulesa, Jared Males, Elena Masciadri, Dino Mesa, Don McCarthy, Michael Meyer, Doug Miller, Matthew J. Nelson, Alfio Puglisi, Fernando Quiros-Pacheco, Armando Riccardi, Eleonora Sani, Paolo Stefanini, Vincenzo Testa, John Wilson, Charles E. Woodward, and Marco Xompero

Rodigas et al. 2012 The Astrophysical Journal 752 57.

  • Provider: AAS Journals

Caption: Figure 8.

Disk color vs. distance from the star, expressed as Δ( Ks − L′) = ( Ks − L′) Disk −( KsL′) Star. This is calculated only where the disk is detected at both the Ks band and at L′. To constrain dust grain size, we also plot model colors from Inoue et al. (2008) (colored horizontal lines). The data suggest that the eastern side of the disk becomes redder than the western side with increasing distance from the star. 1–10 μm grains are the best fit to the western side, while 3–10 μm grains are the best match to eastern side. This may suggest that the west side of the disk is composed of smaller grains than the east side.

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