Uploaded September 2021 | Updated September 2026, 5 hours ago
The Mid-InfraRed Instrument (MIRI) of the James Webb Space Telescope (Webb) sees light in the mid-infrared region of the electromagnetic spectrum, at wavelengths that are longer than our eyes can see.
To support the whole range of Webb’s science goals, from observing our own Solar System and other planetary systems, to studying the early Universe, MIRI allows scientists to use multiple observing techniques: imaging, spectroscopy and coronagraphy.
To pack all these modes in a single instrument, engineers have designed an intricate optical system in which light coming from Webb’s telescope follows a complex 3D path before finally reaching MIRI’s detectors.
This artist’s rendering shows the path for MIRI’s Medium Resolution Spectroscopy module, or MRS. Whereas the Low Resolution Spectroscopy mode is designed to observe single, compact objects like very distant galaxies or single stars, the MRS can produce spectra of its entire field of view. As a result, this part of MIRI is ideally suited for observations of more complex and extended objects, such as closer-by galaxies, crowded fields of stars and galaxies, or nebulae.
We first take a look at its mechanical structure with its three protruding pairs of carbon fibre struts that will attach it to Webb’s instrument compartment at the back of the telescope.
The beam of light coming from the telescope is then shown in deep blue entering the instrument through the pick-off mirror located at the top of the instrument and acting like a periscope.
Then, a series of mirrors redirect the light toward the bottom of the instruments where a set of 4 spectroscopic modules are located. Once there, the beam of light is divided by optical elements called dichroics in 4 beams corresponding to different parts of the mid-infrared region. Each beam enters its own integral field unit; these components split and reformat the light from the whole field of view, ready to be dispersed into spectra. This requires the light to be folded, bounced and split many times, making this probably one of Webb’s most complex light paths.
To finish this amazing voyage, the light of each beam is dispersed by gratings, creating spectra that then projects on 2 MIRI detectors (2 beams per detector). An amazing feat of engineering!
Source: https://www.esa.int/ESA_Multimedia/Videos/2021/09/Webb_MIRI_spectroscopy_animation
The Mid-InfraRed Instrument (MIRI) of the James Webb Space Telescope (Webb) sees light in the mid-infrared region of the electromagnetic spectrum, at wavelengths that are longer than our eyes can see.
To support the whole range of Webb’s science goals, from observing our own Solar System and other planetary systems, to studying the early Universe, MIRI allows scientists to use multiple observing techniques: imaging, spectroscopy and coronagraphy.
To pack all these modes in a single instrument, engineers have designed an intricate optical system in which light coming from Webb’s telescope follows a complex 3D path before finally reaching MIRI’s detectors.
This artist’s rendering shows the path for MIRI’s Medium Resolution Spectroscopy module, or MRS. Whereas the Low Resolution Spectroscopy mode is designed to observe single, compact objects like very distant galaxies or single stars, the MRS can produce spectra of its entire field of view. As a result, this part of MIRI is ideally suited for observations of more complex and extended objects, such as closer-by galaxies, crowded fields of stars and galaxies, or nebulae.
We first take a look at its mechanical structure with its three protruding pairs of carbon fibre struts that will attach it to Webb’s instrument compartment at the back of the telescope.
The beam of light coming from the telescope is then shown in deep blue entering the instrument through the pick-off mirror located at the top of the instrument and acting like a periscope.
Then, a series of mirrors redirect the light toward the bottom of the instruments where a set of 4 spectroscopic modules are located. Once there, the beam of light is divided by optical elements called dichroics in 4 beams corresponding to different parts of the mid-infrared region. Each beam enters its own integral field unit; these components split and reformat the light from the whole field of view, ready to be dispersed into spectra. This requires the light to be folded, bounced and split many times, making this probably one of Webb’s most complex light paths.
To finish this amazing voyage, the light of each beam is dispersed by gratings, creating spectra that then projects on 2 MIRI detectors (2 beams per detector). An amazing feat of engineering!
Source: https://www.esa.int/ESA_Multimedia/Videos/2021/09/Webb_MIRI_spectroscopy_animation
![Gale Crater - Mars Science Laboratory (MSL) Curiosity Rover Landing Site [HD]](https://i.ytimg.com/vi/w5DK3SxolJI/mqdefault.jpg "Gale Crater - Mars Science Laboratory (MSL) Curiosity Rover Landing Site [HD]
...http://www.telescopefeed.com/
A birds-eye view of Curiositys landing site: Mars Gale Crater.
Transcript: John Grotzinger: Im John Grotzinger, the project scientist for Mars Science Laboratory the Curiosity rover and were going to take Curiosity to our chosen landing site in Gale crater, which sits at the border between the southern highlands of Mars and the northern lowlands, a really exciting spot because its very low and thats the kind of place where water might have pooled and possibly formed lakes.
So here we see a different view of Gale crater that has a different perspective. You can see our landing ellipse down at the bottom, which is the white circle. And in the middle of Gale crater is this mountain of rock that is 5 kilometers high, made layer by layer by layer. But the layers at the bottom are the ones that were most interested in, because we think that those were deposited in an aqueous environment, which is very important for understanding habitability. What you can see here now is that were about to land very close to the center of the landing ellipse, and we have a couple of different routes that we can take. The scientists on the team prefer the one on the right. And so what we would do is drive along it.
And now you can see at the base of this mountain where these lower layers are. And the layers are important because they allow us to sort of read a geological book. You start at the bottom of the mountain and those are the oldest layers. And then the layers that occur up near the top, those are the youngest parts, the youngest chapters in the book.
We will drive along, up to this outcrop that we call the fence. And when we get there, were going to study it. Its a really attractive spot for us because it contains the kind of minerals that formed in water. And then, when were done with that, were going to go beyond. And were going to enter a canyon. And this kind of terrain around here reminds us a lot of Sedona, Arizona. And all the rocks around here formed in aqueous environments. And so, theres a lot of rock, hundreds of meters of it, layer after layer, that we can study to tell us about the history of Mars at Gale crater.
Now we cross a boundary and we go into a very different type of rock. You can see how it weathers very differently. Its really rugged. So at that point in the mission, well be beyond our initial mission of two Earth years. This will take us into many years afterwards of exploration as we drive around this very rugged terrain. If we make it, well be able to look back over the area that we have previously studied, back down in towards the bottom of Gale crater, back towards our landing ellipse.
Source: http://www.nasa.gov/multimedia/videogallery/index.html?media_id=102633381")
