Images by Date
Images by Category
Solar System
Stars
White Dwarfs
Supernovas
Neutron Stars
Black Holes
Milky Way Galaxy
Normal Galaxies
Quasars
Galaxy Clusters
Cosmology/Deep Field
Miscellaneous
Images by Interest
Space Scoop for Kids
Multiwavelength
Sky Map
Constellations
3D Wall
Photo Blog
Top Rated Images
Image Handouts
Desktops
High Res Prints
Fits Files
Image Tutorials
Photo Album Tutorial
False Color
Cosmic Distance
Look-Back Time
Scale & Distance
Angular Measurement
Images & Processing
AVM/Metadata
Getting Hard Copies
Image Use Policy
Web Shortcuts
Chandra Blog
RSS Feed
Chandra Mobile
Chronicle
Email Newsletter
News & Noteworthy
Image Use Policy
Questions & Answers
Glossary of Terms
Download Guide
Get Adobe Reader
More Information
Supernovas & Supernova Remnants
Related Podcasts
A Tour of Puppis A
A Tour of Puppis A (2014-09-15)
Download Image

More Information

More Images
Chandra X-ray Image of DEM L238
(Credit: NASA/CXC/NCSU/
K.Borkowski)

Animation & Video


Related Images
DEM L238 and DEM L249:
X-ray Evidence Supports Possible New Class Of Supernova



Credit: X-ray: NASA/CXC/NCSU/K.Borkowski; Optical: NOAO/CTIO/MCELS

DEM L238 and DEM L249 are two supernova remnants in the Large Magellanic Cloud. X-ray data from NASA's Chandra and ESA's XMM-Newton observatories suggest that the stars responsible for these debris fields were unusually young when they were destroyed by thermonuclear explosions.

The large field-of-view is a composite image of DEM L238 (right) and DEM L249, Chandra X-ray data in blue and optical data in white. The inset reveals how DEM L238 appears in the three bands of X-ray emission (low energy X-rays are shown in red, medium energies in green and high energies in blue.) The central region of DEM L238 is green which indicates that it is rich in iron. This overabundance of iron identifies this object as a so-called Type Ia supernova, one possible explosive death of a star.

In a Type Ia supernova, a white dwarf, the dense final stage in the evolution of a sun-like star, pulls so much mass from an orbiting companion star that it cannot support its own weight. The star collapses and temperatures become high enough for carbon fusion to occur. Fusion begins throughout the white dwarf almost simultaneously and an explosion occurs.

A surprising feature of these images is that the iron in the central regions of DEM L238 and DEM L249 is much denser that in most Type Ia supernovas. The most likely explanation for these results is that the white dwarfs exploded into very dense environments. This implies that the stars which evolved into the white dwarfs were more massive than usual, since such stars expel more gas into their surroundings. These stars would explode in much less time -- about 100 million years -- than the billions of years that astronomers think Type Ias typically require.

Fast Facts for DEM L238 and DEM L249:
Credit  X-ray: NASA/CXC/NCSU/K.Borkowski; Optical: NOAO/CTIO/MCELS
Scale  Full field image is 21 arcmin across, Inset image is 8.4 arcmin across
Category  Supernovas & Supernova Remnants
Coordinates (J2000)  RA 05h 34m 08.80s | Dec -70º 34' 28.00"
Constellation  Dorado
Observation Date  October 25, 2003
Observation Time  14 hours
Obs. ID  3908
Color Code  Full field: X-ray: Blue; Optical: Red and Green | Inset: Red: 0.3-0.7 keV; Green: 0.7-3 keV; Blue: 3-7 keV
Instrument  ACIS
References Dense, Fe-rich Ejecta in Supernova Remnants DEM L238 and DEM L249: A New Class of Type Ia Supernova? Borkowski, K.J., Hendrick, S.P., Reynolds, S.P., 2006, ApJ, 652, 1259
Distance Estimate  About 160,000 light years (distance to LMC)
Release Date  January 04, 2007