Astrophoto Lab
--- your online source for astronomical & satellite images ---

A Dying Star's Toxic Legacy
General Information
Special Galleries
Deep Space
Stars, Supernovae
Solar System
Earth from Space
NASA Space Programs
Other Astro Images
Space Image Gallery
Useful Links
Credits & Useage
Name: PK 166-06 1, Westbrook Nebula, IRAS 04395+3601
Description: Planetary Nebula
Position (J2000): RA 04hr 42m 53.64s Dec +36° 06' 53.4"
Constellation: Auriga
Distance: 5000 light years
Image Credit: ESA/Hubble & NASA
Release Date: March 7, 2011

   2000 Image
Click the image to buy a print


The strange and irregular bundle of jets and clouds in this curious image from the NASA/ESA Hubble Space Telescope is the result of a burst of activity late in the life of a star. As its core runs out of nuclear fuel, the star's unstable outer layers are puffing out a toxic concoction of gases including carbon monoxide and hydrogen cyanide.

The Westbrook Nebula - also known as PK166-06, CRL 618 and AFGL 618 - is a protoplanetary nebula, an opaque, dark and relatively short-lived cloud of gas that is ejected by a star as it runs out of nuclear fuel. As the star hidden deep in the center of the nebula evolves further it will turn into a hot white dwarf and the gas around it will become a glowing planetary nebula, before eventually dispersing. Because this is a relatively brief stage in the evolution process of stars, only a few hundred protoplanetary nebulae are known in the Milky Way.

Protoplanetary nebulae are cool, and so emit little visible light. This makes them very faint, posing challenges to scientists who wish to study them. What this picture shows, therefore, is a composite image representing the different tricks that the astronomers used to unravel what is going on within this strange nebula. The picture includes exposures in visible light which shows light reflected from the cloud of gas, combined with other exposures in the near-infrared part of the spectrum, showing us the dim glow, invisible to human eyes, that is coming from different elements deep in the cloud itself.

One of the nebula's names, AFGL 618, comes from its discovery by a precursor to the Hubble Space Telescope: the letters stand for Air Force Geophysics Laboratory. This US research organization launched a series of suborbital rockets with infrared telescopes on board in the 1970s, cataloguing hundreds of objects that were impossible or difficult to observe from the ground. In some respects, these were a proof of concept for later orbital infrared astronomical facilities including Hubble and ESA's Herschel Space Observatory.

This image was prepared from many separate exposures taken using Hubble's newest camera, the Wide Field Camera 3. Exposures through a green filter (F547M) were colored blue, those through a yellow/orange filter (F606W) were colored green and exposures through a filter that isolates the glow from ionized nitrogen (F658N) have been colored red. Images through filters that capture the glows from singly and doubly ionized sulfur (F673N and F953N) are also shown in red. The total exposure times were about nine minutes through each filter and the field of view is approximately 20 arc-seconds across.

From wikipedia:

The Westbrook Nebula (CRL 618) is an aspherical protoplanetary nebula. It is being formed by a star that has passed through the red giant phase and has ceased nuclear fusion at its core. This star is concealed at the center of the nebula, and is ejecting gas and dust at velocities of up to 200 km/s. The nebula is named after William E. Westbrook, who died in 1975.

This nebula began to form about 200 years ago, and primarily consists of molecular gas. The outer part of the nebula is the result of interaction between rapid bi-polar outflow and the gas that was ejected when the star was passing through its asymptotic giant branch phase. The lobes are inclined about 24° to the line of sight. The energy being radiated from the nebula consists of scattered light from the star at the core, light being emitted from a compact HII region surrounding the star, and energy from the shock-excited gas in the lobes.

The core star is believed to be of spectral class B0 and has 12,200 times the solar luminosity