File:The Galactic Center.jpg

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English: The center of our Milky Way Galaxy is located in the constellation of Sagittarius. In visible light the lion's share of stars are hidden behind thick clouds of dust. This obscuring dust becomes increasingly transparent at infrared wavelengths. This 2MASS image, covering a field roughly 10 x 8 degrees (about the area of your fist held out at arm's length) reveals multitudes of otherwise hidden stars, penetrating all the way to the central star cluster of the Galaxy.

This central core, seen in the upper left portion of the image, is about 25,000 light years away and is thought to harbor a supermassive black hole. The reddening of the stars here and along the Galactic Plane is due to scattering by the dust; it is the same process by which the sun appears to redden as it sets.

The densest fields of dust still show up in this mosaic. Also evident are several nebulae to the lower right, including the Cat's Paw Nebula. The 2MASS analysis software has identified and measured the properties of almost 10 million stars in this spectacular field alone.
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Source http://www.ipac.caltech.edu/2mass/gallery/showcase/galcen/index.html
Author 2MASS/G. Kopan, R. Hurt
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http://www.ipac.caltech.edu/2mass/gallery/showcase/copyright.html -- Atlas Image [or Atlas Image mosaic] obtained as part of the Two Micron All Sky Survey (2MASS), a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.
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Public domain This work has been released into the public domain by its author, 2MASS/G. Kopan, R. Hurt. This applies worldwide.
In some countries this may not be legally possible; if so:
2MASS/G. Kopan, R. Hurt grants anyone the right to use this work for any purpose, without any conditions, unless such conditions are required by law.

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current19:38, 30 June 2011Thumbnail for version as of 19:38, 30 June 20114,100 × 5,300 (23.86 MB)Spitzersteph (talk | contribs)

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