Difference: TimeVariationOfDifferentialReddeningTowardsNGC4833 ( vs. 1)

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Time variation of differential reddening towards NGC 4833

Johanna Itam Daniel Pfenniger Gérard Jasniewicz Denis Puy Nicolas Mauron (LUPM, Montpellier, France)

Light passing through clouds of atomic and/or molecular hydrogen is significantly obscured by the dust they contain. One of the major questions in the study of the interstellar medium is the size of the smallest structure of these neutral clouds - is the hierarchical or "fractal" structure extending down to AU-sized clumps such that significant amounts of mass may be hidden in the smallest, densest clumps? The globular cluster NGC 4833 lies behind dusty regions at a latitude of -8°, and provides an
ideal means of looking for small-scale time variations of the extinction. This globular cluster has already been observed by our team in 2006. Old observations of NGC 4833 have been reduced and are promising. It is particularly relevant to study photometric variations of stars due to variable reddening in the light of sight near of the galactic plane, because Gaia should be able to detect them.

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