In astronomy, interstellar reddening is a phenomenon associated with interstellar extinction where the spectroscopic lines unchanged.
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When combined with corrections for interstellar reddening, this allows for accurate determination of a galaxy's distance.
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Interstellar reddening occurs because interstellar dust absorbs and scatters blue light waves more than red light waves, making stars appear redder than they are.
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It was only after Kapteyn's death, in Amsterdam, that Robert Trumpler determined that the amount of interstellar reddening was actually much greater than had been assumed.
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Since blue light is much more strongly attenuated than red light, extinction causes objects to appear redder than expected, a phenomenon referred to as "'interstellar reddening " '.
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In any photometric system interstellar reddening can be described by color excess, defined as the difference between an object's observed color index and its intrinsic color index ( sometimes referred to as its normal color index ).
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The filters are selected so that the mean wavelengths of response functions are 364 nm for U, 442 nm for B, 540 nm for V . The zero point of the A0 main sequence stars not affected by interstellar reddening.
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Due to the extremely high interstellar reddening towards Wd1, it is very difficult to observe in the U-and B-bands, and most observations are made in the R-or I-bands at the red end of the spectrum or in the infra red.
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