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The recently discovered coreshine effect can aid in exploring the coreproperties and in probing the large grain population of the ISM. We discuss theimplications of the coreshine detected from the molecular cloud core L1506C inthe Taurus filament for the history of the core and the existence of aprimitive ISM component of large grains becoming visible in cores. Thecoreshine surface brightness of L1506C is determined from IRAC Spitzer imagesat 3.6 micron. We perform grain growth calculations to estimate the grain sizedistribution in model cores similar in gas density, radius, and turbulentvelocity to L1506C. Scattered light intensities at 3.6 micron are calculatedfor a variety of MRN and grain growth distributions to compare with theobserved coreshine. For a core with the overall physical properties of L1506C,no detectable coreshine is predicted for an MRN size distribution. Extendingthe distribution to grain radii of about 0.65 $\mu$m allows to reproduce theobserved surface brightness level in scattered light. Assuming the propertiesof L1506C to be preserved, models for the growth of grains in cores do notyield sufficient scattered light to account for the coreshine within thelifetime of the Taurus complex. Only increasing the core density and theturbulence amplifies the scattered light intensity to a level consistent withthe observed coreshine brightness. The grains could be part of primitiveomni-present large grain population becoming visible in the densest part of theISM, could grow under the turbulent dense conditions of former cores, or inL1506C itself. In the later case, L1506C must have passed through a period oflarger density and stronger turbulence. This would be consistent with thesurprisingly strong depletion usually attributed to high column densities, andwith the large-scale outward motion of the core envelope observed today.

Coreshine in L1506C - Evidence for a primitive big-grain component or indication for a turbulent core history?