M 1 - Crab Nebula

M1, the Crab Nebula (NGC 1952), is a supernova remnant in the constellation Taurus, located in the Perseus Arm of the Milky Way, and is one of the best-known objects in the Messier Catalogue. It was formed by the explosion of a massive star that was documented in the year 1054 AD by Chinese and Arab astronomers. The distance to Earth is about 6,200 to 6,500 light-years. The nebula has an diameter of 11 to 13 light-years and continues to expand at high velocity into the surrounding interstellar medium.

At the center of the Crab Nebula lies a rapidly rotating neutron star, the so-called Crab Pulsar. It formed during the collapse of the original star and emits intense radiation across nearly the entire electromagnetic spectrum. The visible structure of the nebula consists of a complex network of filamentary gas structures, composed mainly of ionized hydrogen, helium, and heavier elements, which are energized and made to glow by the pulsar’s radiation.

The structure of the Crab Nebula is especially well revealed in dual-band imaging, as used in the accompanying image. The filter highlights the fine filaments of the expanding gas cloud in particular detail.

Shooting Data