Description: |
This side-by-side comparison shows
observations of the Southern Ring Nebula
in near-infrared light, at left, and
mid-infrared light, at right, from
NASA’s Webb Telescope..
.
This scene
was created by a white dwarf star –
the remains of a star like our Sun after
it shed its outer layers and stopped
burning fuel though nuclear fusion.
Those outer layers now form the ejected
shells all along this view..
.
In the
Near-Infrared Camera (NIRCam) image, the
white dwarf appears to the lower left of
the bright, central star, partially
hidden by a diffraction spike. The same
star appears – but brighter, larger,
and redder – in the Mid-Infrared
Instrument (MIRI) image. This white
dwarf star is cloaked in thick layers of
dust, which make it appear larger.
.
.
The brighter star in both images
hasn’t yet shed its layers. It closely
orbits the dimmer white dwarf, helping
to distribute what it’s
ejected..
.
Over thousands of years and
before it became a white dwarf, the star
periodically ejected mass – the
visible shells of material. As if on
repeat, it contracted, heated up – and
then, unable to push out more material,
pulsated. Stellar material was sent in
all directions – like a rotating
sprinkler – and provided the
ingredients for this asymmetrical
landscape..
.
Today, the white dwarf is
heating up the gas in the inner regions
– which appear blue at left and red at
right. Both stars are lighting up the
outer regions, shown in orange and blue,
respectively..
.
The images look very
different because NIRCam and MIRI
collect different wavelengths of light.
NIRCam observes near-infrared light,
which is closer to the visible
wavelengths our eyes detect. MIRI goes
farther into the infrared, picking up
mid-infrared wavelengths. The second
star more clearly appears in the MIRI
image, because this instrument can see
the gleaming dust around it, bringing it
more clearly into view..
.
The stars –
and their layers of light – steal more
attention in the NIRCam image, while
dust plays the lead in the MIRI image,
specifically dust that is illuminated.
.
.
Peer at the circular region at the
center of both images. Each contains a
wobbly, asymmetrical belt of material.
This is where two “bowls” that make
up the nebula meet. (In this view, the
nebula is at a 40-degree angle.) This
belt is easier to spot in the MIRI image
– look for the yellowish circle –
but is also visible in the NIRCam
image..
.
The light that travels through
the orange dust in the NIRCam image –
which look like spotlights – disappear
at longer infrared wavelengths in the
MIRI image..
.
In near-infrared light,
stars have more prominent diffraction
spikes because they are so bright at
these wavelengths. In mid-infrared
light, diffraction spikes also appear
around stars, but they are fainter and
smaller (zoom in to spot
them)..
.
Physics is the reason for the
difference in the resolution of these
images. NIRCam delivers high-resolution
imaging because these wavelengths of
light are shorter. MIRI supplies
medium-resolution imagery because its
wavelengths are longer – the longer
the wavelength, the coarser the images
are. But both deliver an incredible
amount of detail about every object they
observe – providing never-before-seen
vistas of the universe..
.
For a full
array of Webb’s first images and
spectra, including downloadable files,
please visit:
https://webbtelescope.org/news/first-ima
ges .
.
NIRCam was built by a team at
the University of Arizona and Lockheed
Martin’s Advanced Technology
Center..
.
MIRI was contributed by ESA
and NASA, with the instrument designed
and built by a consortium of nationally
funded European Institutes (The MIRI
European Consortium) in partnership with
JPL and the University of Arizona. |