The Crab Nebula – in the constellation Taurus – is seen in new light by James Webb Space Telescope as new details are uncovered
Although the Crab Nebula is one of the best-studied supernova remnants, questions about its progenitor, the nature of the explosion that created it still remain unanswered. The NASA/ESA/CSA James Webb Space Telescope is on the case as it sleuths for any clues that remain within the supernova remnant. Webb’s infrared sensitivity and spatial resolution are offering astronomers a more comprehensive understanding of the still-expanding scene.
Similar to the Hubble optical wavelength image released in 2005, with Webb the remnant appears to consist of a crisp, cage-like structure of fluffy red-orange filaments of gas that trace doubly ionised sulphur (sulphur III). Within the remnant’s interior, yellow-white and green fluffy ridges form large-scale loop-like structures, which represent areas where dust particles reside.
The area is composed of translucent, milky material. This material is emitting synchrotron radiation, which is emitted across the electromagnetic spectrum but becomes particularly vibrant thanks to Webb’s sensitivity and spatial resolution. It is generated by particles accelerated to extremely high speeds as they wind around magnetic field lines. The the synchrotron radiation can be traced throughout the majority of the Crab Nebula’s interior.
Locate the wisps that follow a ripple-like pattern in the middle. In the centre of this ring-like structure is a bright white dot: a rapidly rotating neutron star. Further out from the core, follow the thin white ribbons of the radiation. The curvy wisps are closely grouped together, following different directions that mimic the structure of the pulsar’s magnetic field. Note how certain gas filaments are bluer in colour. These areas contain singly ionised iron (iron II).
Credit: NASA, ESA, CSA, STScI, T. Temim (Princeton University)
The NASA/ESA/CSA James Webb Space Telescope has gazed at the Crab Nebula, a supernova remnant located 6500 light-years away in the constellation Taurus. Since this energetic event was recorded in 1054 CE by 11th-century astronomers, the Crab Nebula has continued to draw attention and additional study as scientists seek to understand the conditions, behaviour, and after-effects of supernovae by carefully studying this relatively close example.
With Webb’s NIRCam (Near-Infrared Camera) and MIRI (Mid-Infrared Instrument), the game is afoot as new details are uncovered—including the first complete map of dust distribution—in the search for answers about the Crab Nebula’s origins.
Similar to the Hubble optical wavelength image released in 2005, with Webb the remnant appears to consist of a crisp, cage-like structure of fluffy red-orange filaments of gas that trace doubly ionised sulphur (sulphur III). Within the remnant’s interior, yellow-white and green fluffy ridges form large-scale loop-like structures, which represent areas where dust particles reside.
The area is composed of translucent, milky material. This material is emitting synchrotron radiation, which is emitted across the electromagnetic spectrum but becomes particularly vibrant thanks to Webb’s sensitivity and spatial resolution. It is generated by particles accelerated to extremely high speeds as they wind around magnetic field lines. The synchrotron radiation can be traced throughout the majority of the Crab Nebula’s interior.
Locate the wisps that follow a ripple-like pattern in the middle. In the centre of this ring-like structure is a bright white dot: a rapidly rotating neutron star. Further out from the core, follow the thin white ribbons of the radiation. The curvy wisps are closely grouped together, following different directions that mimic the structure of the pulsar’s magnetic field. Note how certain gas filaments are bluer in colour. These areas contain singly ionised iron (iron II).
Credit: NASA, ESA, CSA, STScI, T. Temim (Princeton University)
At first glance the general shape of the nebula is reminiscent of the 2005 optical wavelength image from the NASA/ESA Hubble Space Telescope. In Webb’s infrared observation, a crisp, cage-like structure of fluffy gaseous filaments are shown in red and orang. However, in the central regions, emission from dust grains (yellow-white and green) is mapped out by Webb for the first time. The Hubble and Webb images of this object can be contrasted here.
In Webb’s infrared observation, a crisp, cage-like structure of fluffy red-orange filaments and knots of dust surround the object’s central area. However, some aspects of the inner workings of the Crab Nebula become more prominent and increase in detail in infrared light. In particular, Webb highlights what is known as synchrotron emission, seen here with a milky smoke-like appearance throughout the majority of the Crab Nebula’s interior.
Credit: NASA, ESA, CSA, STScI, T. Temim (Princeton University)
Additional aspects of the inner workings of the Crab Nebula become more prominent and are seen in greater detail in the infrared light captured by Webb. In particular, Webb highlights what is known as synchrotron radiation: emission produced from charged particles, like electrons, moving around magnetic field lines at relativistic speeds. The radiation appears here as milky smoke-like material throughout the majority of the Crab Nebula’s interior.
This feature is a product of the nebula’s pulsar, a rapidly rotating neutron star. The pulsar’s strong magnetic fields accelerate particles to extremely high speeds and cause them to emit radiation as they wind around magnetic field lines. Though emitted across the electromagnetic spectrum, the synchrotron radiation becomes particularly vibrant in the infrared with Webb’s NIRCam instrument.
To locate the Crab Nebula’s pulsar heart, trace the wisps that follow a circular ripple-like pattern in the middle to the bright white dot in the centre. Further out from the core, follow the thin white ribbons of the radiation. The curvy wisps are closely grouped together, outlining the structure of the pulsar’s magnetic fields, which sculpt and shape the nebula.
At centre left and right, the white material curves sharply inward from the filamentary dust cage’s edges and goes toward the neutron star’s location, as if the waist of the nebula is pinched. This abrupt slimming may be caused by the confinement of the supernova wind’s expansion by a belt of dense gas.
The wind produced by the pulsar heart continues to push the shell of gas and dust outward at a rapid pace. Notice how the filaments tend to be longer toward the upper right side of the nebula, in the same direction the pulsar is moving – not restricted by the belt of gas. Among the remnant’s interior, yellow-white and green mottled filaments form large-scale loop-like structures, which represent areas where dust grains reside.
The search for answers about the Crab Nebula’s past continues as astronomers further analyse the Webb data and consult previous observations of the nebula taken by other telescopes. Scientists will have newer Hubble data to review within the next year or so from the telescope’s reimaging of the supernova remnant. This will mark Hubble’s first look at the Crab Nebula in over 20 years, and will enable astronomers to more accurately compare Webb and Hubble’s findings.
Press release from ESA Webb.