Stellar Debris N49

This is a composite image of N49, the brightest supernova remnant in optical light in the Large Magellanic Cloud.

The Chandra X-ray image (blue) shows million-degree gas in the center. Much cooler gas at the outer parts of the remnant is seen in the infrared image from Spitzer (red). While astronomers expected that dust particles were generating most of the infrared emission, the study of this object indicates that much of the infrared is instead generated in heated gas.

The unique filamentary structure seen in the optical image by Hubble (white & yellow) has long set N49 apart from other well understood supernova remnants, as most supernova remnants appear roughly circular in visible light. Recent mapping of molecular clouds suggests that this supernova remnant is expanding into a denser region to the southeast, which would cause its asymmetrical appearance. This idea is confirmed by the Chandra data. Although X-rays reveal a round shell of emission, the X-rays also show brightening in the southeast, confirming the idea of colliding material in that area.

N49 is about 160,000 light years (distance to Large Magellanic Cloud) in the Dorado Constellation

Credit X-ray: NASA/CXC/Caltech/S.Kulkarni et al.; Optical: NASA/STScI/UIUC/Y.H.Chu & R.Williams et al.; IR: NASA/JPL-Caltech/R.Gehrz et al.
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More Images of N49 and Zoom into N49 with Chandra
Supernovas & Supernova Remnants from Chandra X-Ray Observatory
Taking it to the Edge RCW 86 & G347.3-0.5 Chandra & XMM Newton X-Ray Images
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