Euclid Space Telescope
Euclid is named after the Greek mathematician Euclid of Alexandria, who lived around 300 BC and founded the subject of geometry. As the density of matter and energy is linked to the geometry of the universe, the mission was named in his honor.
Mission objectives
Euclid is designed to explore the evolution of the dark Universe. It will make a 3D-map of the Universe (with time as the third dimension) by observing billions of galaxies out to 10 billion light-years, across more than a third of the sky.
While dark energy accelerates the expansion of the Universe and dark matter governs the growth of cosmic structures, scientists remain unsure about what dark energy and dark matter actually are.
By observing the Universe evolving over the past 10 billion years, Euclid will reveal how it has expanded and how structure has formed over cosmic history – and from this, astronomers can infer the properties of dark energy, dark matter and gravity, to reveal more about their precise nature.
This addresses two core themes of ESA’s Cosmic Vision program: What are the fundamental physical laws of the Universe? and How did the Universe originate and what is it made of?
Key questions
Euclid is designed to tackle some of the most important questions in cosmology:
What is the structure and history of the cosmic web?
What is the nature of dark matter?
How has the expansion of the Universe changed over time?
What is the nature of dark energy?
Is our understanding of gravity complete?
Spacecraft and Instruments
The Euclid spacecraft is approximately 4.7 m tall and 3.7 m in diameter. It consists of two major components: the service module and the payload module.
The payload module comprises a 1.2-m-diameter telescope and two scientific instruments: a visible-wavelength camera (the VISible instrument, VIS) and a near-infrared camera/spectrometer (the Near-Infrared Spectrometer and Photometer, NISP). The service module contains the satellite systems: electric power generation and distribution, attitude control, data processing electronics, propulsion, telecommand and telemetry, and thermal control.
The VIS Instrument
The VIS instrument is one of two instruments on Euclid. It is a large format imager, with 609 million pixels covering a field of view of 0.57 deg2 (almost 3 times the solid angle of the full Moon) with 0.1 arcsec sampling. The full image is transmitted to ground, making these the largest images yet for an astronomical satellite. VIS slightly under-samples the telescope point spread function, but this is recovered through multiple exposures, so its effective angular resolution is 0.18 arcsec.
The focal plane consists of 36 CCD273-84, custom designed and manufactured for VIS by e2v (now Teledyne e2v). They are read out from the four corners, resulting in 144 channels of information. The signals in the pixels are digitized to 16 bits resolution, each bit corresponding to 3.4 electrons. The internal noise of the VIS detection chain is less than 4.4 electrons in all channels.
For the Euclid Wide Survey, VIS is typically used in a regular observing sequence lasting just over 4200 sec. During this time four nominal duration exposures of 565 sec and two shorter exposures of 100 sec are taken, together with a number of calibration exposures. These are all sequenced with the NISP instrument to maximize Euclid’s observing efficiency. Euclid will make small pointing displacements between the four nominal exposures to ensure that stars falling in the small gaps between the closely butted detectors are exposed with at least three exposures. Approximately 20 of these fields are observed each day. With three exposures per field, it is expected that a signal-to-noise ratio of 10 will be achieved for a source of IE(AB)=26.0 with 92% of flux within a 1.3 arcsec diameter aperture, typical for a distant galaxy. VIS pixels are saturated at ~200 000 electrons, so that the bright limit (for stars) in the nominal exposure is mAB=17.8 and for the short exposure is IE(AB)=16.0.
This means it can separate objects that are only 0.1 AR seconds or about 500 M
apart at a distance of 10 billion light years!
NISP Instrument
The Near Infrared Spectrometer and Photometer NISP observes two different types of data, as the name already implies. Using a single optical system, NISP covers the same field-of-view as VIS, the other instrument onboard Euclid, but in near-infrared (NIR) light between ~950 and 2020nm. NISP creates images with 16 Teledyne “H2RG” detectors, with each 2k by 2k pixels, or about 64 million pixels in total, with a sampling on the sky of 0.3 arcseconds per pixel, at a field of view of 0.57 square degrees for every exposure.
This is somewhat undersampling the diffraction-limited beam of light entering NISP, but the primary goal of NISP is not to create high-resolution images – that’s the purpose of VIS – but to gather spectral information. NISP’s two modes create on one side images through broad-band filters in the YE, JE, and HE band – the “photometric channel” – as an input into calculation of so-called “photometric redshifts”, hence rough distances, of more than a billion galaxies. The other, “spectroscopic channel” is creating NIR spectra with a spectral resolution of >400, which provide very precise distance measurement for a subset of ~50 million galaxies.
NISP receives light from a dichroic beamsplitter that reflects-off visible wavelength light into VIS. With four lenses of different materials the light is projected through optical elements in two wheels, a grism wheel – containing four different dispersing grisms -, and a filter wheel – with three passband filters and a closed position. Any of these 7 science elements or the closed position can be chosen to filter the light, that is then projected onto the detector array. The filters of 130mm diameter, are the largest NIR filters in an astronomical space mission so far.
For calibration of the sensitivity and linearity of each detector pixel an LED-based calibration lamp can shine light onto the detector array, at 5 choosable wavelengths.
NISP will operate its 565s spectroscopic observations in parallel to VIS, followed by 112s-long exposures in each of the YE, JE, and HE photometric bands. Standard wide-survey NISP images will be sensitive to ~24.3mag (AB) point sources at signal-to-noise of 5, and have a bright limit around 16.5mag.
NISP slitless spectroscopic observations will be able to detect Lyman-alpha emission lines across the Universe, out to redshifts of 1.9, when the Universe was only 3.5 billion years old. The power of this mode is the combination of good sensitivity to detect an emission line from even very compact distant galaxies and covering an area corresponding to almost 3x the area of the full moon on the sky in every observation.
In the Euclid Wide Survey, NISP will observe about 10 square degrees every day, covering every 5-6 days an area similar to what the Hubble Space Telescope has covered during its 30+ year lifetime in total.
What can Euclid do that the James Webb Space Telescope cannot?
Where Webb can observe extremely far back in time and zoom into the details, Euclid can go fast and wide. In a single observation Euclid can record the data from an area of the sky more than one hundred times bigger than that imaged by Webb’s camera, NIRCam. This means that Euclid can map a third of the sky to the required sensitivity in six years in space – a feat that would be impossible with Webb.
What will Euclid’s image quality be?
Euclid’s images will be at least four times sharper than those achieved by ground-based sky surveys. In the absence of Earth’s atmosphere, and with optics of the highest quality, the angular resolution of a telescope is determined by the size of its primary mirror. Since Euclid has a smaller primary mirror than the Hubble Space Telescope, it will resolve fewer fine details, but the image quality will be outstanding and the lower resolution will be adequate to achieve its scientific goals. The telescope and its optics are designed to deliver a large field of view and a stable image quality throughout the survey.