The progenitor star of the Vela SNR experienced a cataclysmic explosion, known as a type II supernova, approximately 11,000-12,000 years ago. This explosion birthed the Vela pulsar, a highly magnetized rotating neutron star. The existence of the Vela pulsar provides the first concrete observational proof that supernova explosions indeed form neutron stars.
Moreover, the Vela SNR shares the cosmic stage with Puppis A, another SNR located four times further away. These two celestial bodies are renowned for being amongst the most expansive and brightest X-ray sources.
In terms of angular size, Vela is considered one of the largest SNRs. Its apparent diameter in the sky outmeasures four degrees, dwarfing the full Moon's half-degree span. Depending on the observation wavelength, its appearance varies significantly. In radio, Vela is depicted as a shell housing a pulsar and its corresponding pulsar wind nebula. However, in optical bands, only specific filaments are visible. When viewed in X-rays, the central region becomes more prominent, while its shell appears irregular. This variability has led to its classification as a composite remnant[1].
Accompanying this text is a composite image of the Vela SNR, captured using ESO's Very Large Telescope situated at Cerro Paranal, Chile. Various broadband filters were used to create this image, revealing the beauty and complexity of the Vela SNR.
Image credit goes to the ESO/VPHAS+ team, with an acknowledgement to the Cambridge Astronomical Survey Unit.
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