Euclid - Royal Observatory, Edinburgh · UK Space Agency Presentation – Jan 2012: page Euclid...

UK Space Agency Presentation – Jan 2012: page

Andy Taylor

Institute for Astronomy, University of Edinburgh,

Royal Observatory, Blackford Hill, Edinburgh, UK

1

Euclid

(Euclid Simulations: Teyssier et al 2008)

DEXVIII

Thursday, 12 January 2012

11/19/2010 IoP-RAS Meeting 2

Standard Model of Cosmology

+ Einstein Gravity & Initial Conditions (Inflation).


DEXVIII – 12 Jan 2012: page

Euclid: Key Cosmological Questions

3

1. Dynamical Dark Energy:Is the dark energy simply a cosmological constant, or is it a field that evolves dynamically with the expansion of the Universe?

2. Modified Gravity:Is the apparent acceleration due to a breakdown of Einstein Gravity on the largest scales?

3. Dark Matter:What is dark matter? What is the absolute neutrino mass scale and what is the number of relativistic species in the Universe?

4. Initial Conditions:What is the power spectrum of primordial density fluctuations, which seeded large-scale structure, and are they described by a Gaussian probability distribution?



Euclid Primary Science Probes3-D Weak Lensing:Galaxy images are distorted (sheared), γ, by ~1%.

Measure shear and redshifts ➡ projected mass maps, κ (convergence).

4

10 100 1000 10000Wavelength, l

Invert to see 3-D mass maps and evolution of structure.

Cκκ(l,z)

Cββ (l,z) Measure power

spectrum

Kiessling, Taylor, Heavens, 2010

Massey, et al 2007DEXVIII



Photometric Redshifts

5

UK Space Agency Presentation – Jan 2012: page 20

The need for Infrared imaging & photometry

•  The distance (redshift) is determined by modelling the measured intensities of each galaxy in several bands optical + infrared: photometric redshifts (photo-Z)

•  Deep infrared photometry over the entire sky can only be done from space: incorporated in Euclid

redshift redshift

reds

hift

reds

hift

quality of redshift determinations: Abdalla et al (2008)

Technique 1: Weak Lensing (ctd)

Abdalla et al (2008)

• Need Infrared Photometry from space.

• Galaxy distances (redshifts) measured by modelling intensity in passbands.

• Bands griz can be done from ground (e.g. Pan-STARRS, DES).

• Required accuracy reached by adding IR (Y,J,H) from Euclid.



Euclid Primary Science ProbesGalaxy Clustering:• Clustering pattern imprinted with plasma sound-wave at ~150Mpc.

• Baryonic Acoustic Oscillation from recombination - Standard Ruler.

6

Comoving Separation Mpc/h

ξ(r)

Pattern also distorted by gravitational

peculiar velocitiesgenerated by mass.

Figure 2 The redshift-space correlation function for the 2dFGRS, !(", #),plotted as a function of transverse (") and radial (#) pair separation. The func-tion was estimated by counting pairs in boxes of side 0.2 h!1 Mpc (assuming an! = 1 geometry), and then smoothing with a Gaussian of rms width 0.5 h!1 Mpc.To illustrate deviations from circular symmetry, the data from the first quadrantare repeated with reflection in both axes. This plot clearly displays redshiftdistortions, with ‘fingers of God’ elongations at small scales and the coherentKaiser flattening at large radii. The overplotted contours show model predic-tions with flattening parameter $ ! !0.6/b = 0.4 and a pairwise dispersion of"p = 400 km s!1. Contours are plotted at ! = 10, 5, 2, 1, 0.5, 0.2, 0.1.

The model predictions assume that the redshift-space power spectrum(Ps) may be expressed as a product of the linear Kaiser distortion and a radialconvolution14: Ps(k) = Pr(k) (1 + $µ2)2 (1 + k2"2

pµ2/2H20 )!1, where µ = k̂ · r̂,

and "p is the rms pairwise dispersion of the random component of the galaxy ve-locity field. This model gives a very accurate fit to exact nonlinear simulations15.For the real-space power spectrum, Pr(k), we take the estimate obtained by de-projecting the angular clustering in the APM survey13,16. This agrees very wellwith estimates that can be made directly from the 2dFGRS, as will be discussedelsewhere. We use this model only to estimate the scale dependence of thequadrupole-to-monopole ratio (although Fig. 2 shows that it does match the full!(", #) data very well).

The presence of bias is an inevitable consequence of the nonlinear nature of galaxy for-mation, and the relation between mass and galaxy tracers is complex18,19,20. However,there are good theoretical reasons to expect that b can indeed be treated as a constanton large scales, where the density fluctuations are linear21,22. Redshift-space distortions

4

DEXVIII

Peacock et al 2001

Eisenstein et al 2005



Parameterise post-ΛCDM Universe:

7

1. Dynamical Dark Energy:Model dark energy by varying equation of state,

w(a) = P/ρc² = wp + wa(ap-a)2. Modified Gravity:

Parameterise deviation to growth rate, γ=0.55 for GR, of matter clustering,

δ ∝ af, f = Ωmγ, 3. Dark Matter:

Add the contribution from a species of massive neutrinos with mass,

mν.4. Initial Conditions: Departures from primordial Gaussianity of matter clustering parameterized by

fNL.



Optimise Primary Euclid Science

• Combining Weak Lensing and Galaxy Clustering maximises Euclid Primary Science: FoM = 1/[Δwp x Δwa].

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8DEXVIII


DEXVIII – 12 Jan 2012: page 9

Euclid: Key Cosmological Questions

Predicted accuracy of post-ΛCDM parameters:

Primary = WL + GCAll = Primary + Cluster Counts & ISW



Euclid Instruments

10DEXVIII

• To do this we require:

•Visible Image Channel (UK): - 36 4069x4069 CCD273 detectors.- Broad-band R+I+Z (550-900nm)

•Near Infrared Spectroscopy (Fr):- Wavelength range 0.9-2.0µm- Slitless spectroscopy

• Near Infrared Photometry (Fr):- 16 NIR HgCdTe detectors.- 3 bands Y,J,H (1.0-1.7µm)

• Beam splitter sends images to VIS and NISP Instruments.

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+

VIS

NISP



Euclid Mission

11DEXVIII

• Launch date 2019. L2 orbit.• 6-year primary mission, 7-yr total.• Telescope 3 mirrors with 1.2m primary.• 0.18 arcsecond Point Spread Function.• 0.1 arcsec pixels (VIS)• 0.5 square degree field of view.• Wide Survey - 15,000 sq deg:

VIS = 24.5, median z = 0.9NISP = 24

• Deep Survey - 40 sq deg: VIS = 29 NISP = 26.



Primary Euclid Science Measurements3-D Weak Lensing:• Images and redshifts to 1.5 Billion galaxies.

• Measure ~165 auto- and cross-power spectra

Cκκ(l,z,z’), Cββ (l,z,z’), Cκβ (l,z,z’) to sub-percent accuracy.

• Accurate 2-D and 3-D mass mapping.

12DEXVIII

Cκκ(l,z)

Cββ (l,z) 10 100 1000 10000

Wavelength, l

Cκκ(l,z)

Cββ (l,z)

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Galaxy Clustering• Redshifts for 50 Million galaxies.

• Measure the redshift-space galaxy power spectrum: P(k,z)

BAO & redshift-distortion.

Kiessling, ANT, Heavens, 2010

Percival, Baugh et al 2010, Euclid Red Book 2010



Primary Euclid Science Measurements

• Weak Lensing 3-D shear power: C′(l,z,z’) = (1+m)2C(l,z,z’) + σ2sys

- Require: m < 2 ×10−3 and σ2sys < 10−7

• Photo-z’s: - Require Δz ≤ 0.05(1+z), <10% failures.

• Galaxy Clustering:- Slit-less Spectroscopy (Hα emission in star-forming galaxies).- Sky density 3,500/sq deg.- Redshift Completeness >45% (slitless confusion).

Calibration bias Uncorrected Systematics

13DEXVIII



WL SWG

GC SWG

OUs

SDC-FR

WL SWG

GC SWG

OUs OUs OU...

SDC-IT SDC-UK SDC...

Euclid Data Processing

Science Ground Segment (SGS)

...

...

Science Working Groups set

Requirements

OperationalUnits define algorithms

Science DataCentres

Implement and run analysis

Science Working Groups coordinate

Science Exploitation

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Euclid Legacy Science

15DEXVIII

• Legacy SWGs Coordinated by Steve Warren (IC).

• High-redshift Universe: z>7 Galaxies and Quasars:

Detect Lyman Break Galaxies (LBG).

• Co-evolution of galaxies and AGN

• Near-field Cosmology and Astrophysics

• Strong Lensing



Prominent UK Roles in Euclid

• UK has major scientific leadership of Euclid Weak Lensing and a significant role in Galaxy Clustering.

•Euclid Consortium Board/ESA Science Team: - Mark Cropper (MSSL) - VIS Instrument Scientist, UK PI.

- Bob Nichol (Ports) - Galaxy Clustering Scientist.

• 3 of the 6 Science Working Group Coordinators:- Tom Kitching (UoE) - Weak Lensing- Will Percival (Ports) - Galaxy Clustering- Steve Warren (IC) - Legacy Science

• Euclid Science Ground Segment:- Andy Taylor (UoE) - Weak Lensing OU-SHE Lead, UK SGS Lead.- Filipe Adballa (UCL P&A) - LE3 Science-Ready Products co-deputy lead.- Neville Shane (MSSL) - VIS raw reduction deputy lead.

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17UK Space Agency Presentation – Jan 2012: page

Euclid Summary• Euclid will be the major optical/NIR mission for a generation.

• Need space for: Small, stable PSF, NIR photo-z channels for Weak Lensing. Large homogeneous volume for Galaxy Clustering.

• Survey optimised for primary, dark energy science.

• VIS and NISP Instruments for imaging, photometry and spectroscopy.

• UK has very prominent role in Weak Lensing: WL SWG, VIS Inst, VIS reduction, 3-D Shear Catalogue, 3-D Shear power spectra, 3-D mass maps.

and a significant role in Galaxy Clustering: GC SWG, Slitless corrections, Galaxy redshift-space power spectrum.

• Additional significant roles in Legacy Science.

• Euclid Red Book available online: Laureijs et al 2010.

DEXVIII



END

18DEXVIII



Overview of Euclid Data Handling

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Centre (MOC)

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Euclid Legacy Active

Euclid Mission Active

Euclid Science Ground Segment

19DEXVIII

ESA

Euclid Consortium



Euclid Science Ground Segment Structure

VIS INST VIS

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NISP

EXT

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SDCs...

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SWG

GC SWG

WL LE3

GC LE3

UK LeadDeputy-Lead

UK co-Lead

Science Ground Segment (SGS)

OUs

(Non-UKSAFunded)

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