3. Tasks
In order to get answers to the Mission questions, Euclid will measure the geometry , expansion rate and structure growth in the Universe as a function of redshift. This map, spanning 3/4 of the lifetime of the Universe will complement the single snapshot at z ≈1100 made by WMAP and Planck.
By combining the use of Redshift measurements (4.1), Weak gravitational lensing (4.2) and Baryonic Acoustic Oscillations (4.3), both Dark Energy (DE) and Dark Matter(DM) will be investigated in the following tasks:
1. Construct a three-dimensional Dark Matter map to a depth of z=2. See Figure 2.
2. Measure wΛ.
In the benchmark model, the dark energy component has an equation of state parameter wΛ= -1. There are other models where wΛ is dynamic …show more content…
5.2. Deep Survey
The Deep Survey will cover (at least) two patches of > 10 deg2 and objects down to magnitude 26.
The objectives of Euclid’s Deep Survey is
1. to investigate galaxy formation with very high statistical confidence.
2. to obtain spectroscopic redshifts required to calibrate the photometric redshifts needed for the weak lensing experiment.
3. to support the calibration of the visible PSF (point spread function, i.e. the size of a point source) by repeatedly visiting the same fields on the sky. A small PSF is vital for the weak lensing
This survey will be 2 magnitudes deeper than the wide survey, by frequently visiting the same regions in the wide survey observing mode. About 400 000 galaxies at 0 < z < 6 are expected.
6. Summary
The Euclid mission will gather a very large amount of data. After analyze, and combined with other observations (Planck), the most important results will be:
• A considerably better (5x) estimate of wΛ than we have today.
• A three-dimensional dark matter map of the (extragalactic) Universe
• The neutrino mass , with a precision better than 0.04
In order to get answers to the Mission questions, Euclid will measure the geometry , expansion rate and structure growth in the Universe as a function of redshift. This map, spanning 3/4 of the lifetime of the Universe will complement the single snapshot at z ≈1100 made by WMAP and Planck.
By combining the use of Redshift measurements (4.1), Weak gravitational lensing (4.2) and Baryonic Acoustic Oscillations (4.3), both Dark Energy (DE) and Dark Matter(DM) will be investigated in the following tasks:
1. Construct a three-dimensional Dark Matter map to a depth of z=2. See Figure 2.
2. Measure wΛ.
In the benchmark model, the dark energy component has an equation of state parameter wΛ= -1. There are other models where wΛ is dynamic …show more content…
5.2. Deep Survey
The Deep Survey will cover (at least) two patches of > 10 deg2 and objects down to magnitude 26.
The objectives of Euclid’s Deep Survey is
1. to investigate galaxy formation with very high statistical confidence.
2. to obtain spectroscopic redshifts required to calibrate the photometric redshifts needed for the weak lensing experiment.
3. to support the calibration of the visible PSF (point spread function, i.e. the size of a point source) by repeatedly visiting the same fields on the sky. A small PSF is vital for the weak lensing
This survey will be 2 magnitudes deeper than the wide survey, by frequently visiting the same regions in the wide survey observing mode. About 400 000 galaxies at 0 < z < 6 are expected.
6. Summary
The Euclid mission will gather a very large amount of data. After analyze, and combined with other observations (Planck), the most important results will be:
• A considerably better (5x) estimate of wΛ than we have today.
• A three-dimensional dark matter map of the (extragalactic) Universe
• The neutrino mass , with a precision better than 0.04