Named SN 1957D because it was the fourth supernova to be discovered in the year 1957, it is one of only a few such objects located outside of the Milky Way Galaxy that is detectable, in both radio and optical wavelengths, decades after its explosion was observed. In 1981, astronomers saw the remnant of the exploded star in radio waves, and then in 1987 they detected the remnant at optical wavelengths, years after the light from the explosion itself faded.
A relatively short observation — about 14 hours long — from NASA’s Chandra X-ray Observatory in 2000 and 2001 did not detect any X-rays from the remnant of SN 1957D. However, a much longer observation obtained in 2010 and 2011, totaling nearly 8.5 days of Chandra time, did reveal the presence of X-ray emission. The X-ray brightness in 2000 and 2001 was about the same as or lower than it is in this deep image.
This new Chandra image of M83 is one of the deepest X-ray observations ever made of a spiral galaxy beyond our own. This full-field view of the spiral galaxy shows the low, medium, and high-energy X-rays observed by Chandra in red, green, and blue, respectively. The location of SN 1957D, which is found on the inner edge of the spiral arm just above the galaxy’s center, is outlined in the box.
The new X-ray data from SN 1957D provides important information about the nature of this explosion, which astronomers think happened when a massive star ran out of fuel and collapsed. The distribution of X-rays suggests that SN 1957D contains a neutron star — a rapidly spinning, dense star formed when the core of pre-supernova star collapsed. This neutron star, or pulsar, may be producing a cocoon of charged particles moving at close to the speed of light known as a pulsar wind nebula.
If this interpretation is correct, the pulsar in SN 1957D is observed at an age of 55 years, one of the youngest pulsars ever seen. (The remnant SN 1979C in the galaxy M100 contains another candidate for the youngest pulsar, but astronomers are still unsure whether a black hole or a pulsar lies at the center of the remnant.
An image from the Hubble Space Telescope (in the box labeled “Optical Close-Up”) shows that the debris of the explosion that created SN 1957D is located at the edge of a star cluster less than 10 million years old. Many of these stars are estimated to have masses about 17 times that of the Sun. This is just the right mass for a star’s evolution to result in a core-collapse supernova, as is thought to be the case in SN 1957D.