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Chandra X-ray Image of
G292.0+1.8
(Credit: NASA/CXC/Penn State/S.Park et al.)

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G292.0+1.8:
Stellar Forensics with Striking Image from Chandra



Credit: X-ray: NASA/CXC/Penn State/S.Park et al.; Optical: Pal.Obs. DSS

The aftermath of the death of a massive star is shown in beautiful detail in this new composite image of G292.0+1.8. In color is the Chandra X-ray Observatory image - easily the deepest X-ray image ever obtained of this supernova remnant - and in white is optical data from the Digitized Sky Survey. Although considered a "textbook" case of a supernova remnant, the intricate structure shown here reveals a few surprises.

Near the center of G292.0+1.8 is the so-called pulsar wind nebula, most easily seen in high energy X-rays. This is the magnetized bubble of high-energy particles that surrounds the "pulsar", a rapidly rotating neutron star that remained behind after the original, massive star exploded. The narrow, jet-like feature running from north to south in the image is likely parallel to the spin axis of the pulsar.

The pulsar is located slightly below and to the left of the center of G292.0+1.8. Assuming that the pulsar was born at the center of the remnant, it is thought that recoil from the lopsided explosion may have kicked the pulsar in this direction. However, the kick direction and the pulsar spin direction do not appear to be aligned, in contrast to apparent spin-kick alignments seen in some other supernova remnants.

Another key feature of this remnant is the long white line running from left to right across the center called the equatorial belt. This structure is thought to be created when the star - before it died - expelled material from around its equator via winds. The orientation of the equatorial belt suggests the parent star maintained the same spin axis both before and after it exploded.

One puzzling aspect of the image is the lack of evidence for thin filaments of high energy X-ray emission, thought to be an important site for cosmic ray acceleration in supernova remnants. These filaments are seen in other supernova remnants such as Cassiopeia A, Tycho and Kepler. One explanation may be that efficient acceleration occurs primarily in very early stages of supernova remnant evolution, and G292.0+1.8, with an estimated age of several thousand years, is too old to show these effects. Casseiopeia A, Tycho and Kepler, with ages of several hundred years, are much younger.

Fast Facts for G292.0+1.8:
Credit  X-ray: NASA/CXC/Penn State/S.Park et al.; Optical: Pal.Obs. DSS
Scale  Image is 11.5 arcmin per side
Category  Supernovas & Supernova Remnants
Coordinates (J2000)  RA 11h 24m 36.00s | Dec -59° 16' 00.00"
Constellation  Centaurus
Observation Date  6 pointings from Sept 13 - Oct 20, 2006
Observation Time  142 hours
Obs. ID  6677- 6680, 8221, 8447
Color Code  X-ray: Red (0.580-710 & 0.880-950 keV), Orange (0.980-1.100 keV), Green (1.280-1.430 keV), Blue (1.810-2.050 and 2.400-2.620 keV); Optical (white)
Instrument  ACIS
References Park, S. et al, 2007, ApJ, Accepted
Distance Estimate  About 20,000 light years
Release Date  October 23, 2007