|
|
More Images of W49B
| 1 |
|
Chandra Broadband X-ray Image of
W49B
This Chandra X-ray image reveals a barrel-shaped supernova remnant
around a glowing bar of intense X-radiation. These X-rays are produced
by jets of 15 million degree Celsius gas that is rich in iron and
nickel. These features indicate that W49B was produced when the core
of a rapidly-rotating massive star collapsed to form a black hole,
triggering the ejection of high-energy jets of material.
Scale: Image is 5.7 arcmin per side
(Credit: NASA/CXC/SSC/J. Keohane et al.) |
| 2 |
|
Chandra Fe K-line Image of W49B
This Chandra image shows the X-rays from hot iron ions that have been
stripped of all but their inner electrons, called K-shell electrons.
The intensity of the radiation from iron ions, and their concentration
in the jet-like feature indicate that W49B was produced when the core
of a rapidly-rotating massive star collapsed to form a black hole,
triggering the ejection of high-energy jets of iron-rich material.
Scale: Image is 5.7 arcmin per side
(Credit: NASA/CXC/SSC/J. Keohane et al.)
|
| 3 |
|
|
|
|
|
Palomar Infrared Images
of W49B
These infrared images, when combined with Chandra X-ray data, help
reveal a barrel-shaped supernova remnant consisting of bright infrared
rings around a glowing bar of intense X-radiation. The infrared data
was observed with the Palomar Hale 200" WIRC (Wide InfraRed Camera).
Scale: Images are 5.7 arcmin per side
(Credit: Caltech/SSC/J.Rho and T. Jarrett)
|
|
4 |
|
|
|
|
|
Chandra 3-Color X-ray
Image of W49B
Chandra X-ray data reveal a barrel-shaped supernova remnant around
a glowing bar of intense X-radiation. These X-rays are produced by
jets of 15 million degree Celsius gas that is rich in iron and nickel.
These features indicate that W49B was produced when the core of a
rapidly-rotating massive star collapsed to form a black hole, triggering
the ejection of high-energy jets of material. The colors red, green
and blue in the images correspond to low, medium and high-energy X-rays,
respectively.
Scale: Image is 5.7 arcmin per side
(Credit: NASA/CXC/SSC/J. Keohane et al.) |
Return to W49B (02 Jun04)
|
