Euclid space mission
Y. Mellier on behalf of the Euclid Collaboration ESA M-class mission Euclid primary objectives • Understand the origin of the Universe’s accelerating expansion • Probe the properties and nature of dark energy, dark matter, gravity, and • Distinguish their effects by: • Using at least 2 independent but complementary probes • Tracking their (very weak) observational signatures on the • geometry of the universe: Weak Lensing (WL) and Galaxy Clustering (GC) • cosmic history of structure formation: WL, Redshift-Space Distortion (RSD), clusters of galaxies (CL) • Controling systematic residuals to an unprecedented level of accuracy.
Euclid Q2C6 Nice, 17 October 2013 DE and Planck
The Planck collaboration. Ade et al 2013
• If w = P/ρ = cte à After Planck: à w still compatible with -1
But Planck data leave open that w may not be -1 or may vary with time ... - à Euclid can probe its effects and explore its very nature.
Euclid Q2C6 Nice, 17 October 2013 BOSS: transition DM-DE
The BOSS collaboration • The Universe experienced a DM-DE transition period likely over the past 10 billion years.
z ~0.5 Transition very late, can be • Redshift range [0.; 2.5] à explored with visible+NIR telescopes à Euclid
Euclid Q2C6 Nice, 17 October 2013 Euclid primary probes BAO, RSD and WL over 15,000 deg2 50 million galaxies with redshifts 1.5 billion sources with shapes,Colombi, 10 Mellier slices 2001
BAO
Source plane z2
Source plane z1 RSD
Euclid Q2C6 Nice, 17 October 2013 Photo-z: Visible + NIR data needed for Euclid 9 • Weak Lensing : redshifts of 2 x10 HST/ACS credit NASA/ESA HST/ACS; credit NASA/ESA sources to o Slice the universe o Control contamination by intrinsic alignments of galaxies
• Redshifts of Euclid clusters: Galaxy halos Clusters of galaxies (60,000 clusters, 5,000 giant arcs)
à synergy with Planck and eROSITA Dietrich et al 2012 Colombi/Mellier
• Redshifts of sources and lenses needed at least in the range 0.2 à Photo-z necessary, but with both Filaments between clusters Cosmic shear Optical+NIR data Euclid Q2C6 Nice, 17 October 2013 Euclid: mission implementation Euclid mission baseline: Launch in 2020 Photo-z: Ground based Photometry and Spectroscopy In ~6 years 15,000 deg2 40 deg2 Shapes + Photo-z of n = 1.5 x109 galaxies z of n=5x107 galaxies Possibility other surveys: SN and/or µ-lens surveys, Milky Way ? Ref: Euclid RB Laureijs et al arXiv:1110.3193 Euclid Q2C6 Nice, 17 October 2013 Euclid main sub-systems PLM and scientific instruments Courtesy: Astrium and ESA Project office Euclid Consortium • Stabilisation: Pointing error along the x,y axes= 25mas over a period 700 s. • FoV: Common visible and NIR Fov = 0.54 deg2 Euclid Q2C6 Nice, 17 October 2013 VIS scientific instrument Courtesy: S. Pottinger, M. Cropper and the VIS team (wide band channel) Euclid Q2C6 Nice, 17 October 2013 NISP scientific instrument Courtesy: T. Maciaszek and the NISP team - 16 2kx2K H2GR NIR detectors - 0.3 arcsec pixel on sky - 3 Filters: Y, J, H - 4 grims: 2B, 2R - Limiting magAB: 24 (5 σ point like) Euclid Q2C6 Nice, 17 October 2013 Science Ground Segment Courtesy: F. Pasian, M. Sauvage, J. Hoar, C. Dabin EC SGS and ESAC • Complex organisation: • 10 Organisation Units • 7 Science Data Centers • Data: huge volumes, heterogeneous data sets • imagery and morphometry, photometry , spectroscopy Euclid Consortium • data from ground and space • 20-30 Pbytes SDCs • > 1010 sources (>3-sigmas) • 1st release Level-3: 26 months OUs after the begining of the survey. • SGS = 50% of Euclid Consortium contributions. Euclid Q2C6 Nice, 17 October 201313 Euclid: performances VIS performance:imaging A 4kx4k view of the Euclid sky VIS image: cuts made to highlight artefacts VIS PSF Cosmic rays Courtesy Mark Cropper, Sami M. Niemi and the VIS team Euclid Q2C6 Nice, 17 October 2013 Simulation of M51 with VIS (Courtesy J. Brinchmann and S. Warren ) SDSS @ z=0.1 Euclid @ z=0.1 Euclid @ z=0.7 Messier 51 galaxy at z~0.1 and 0.7: Euclid will get the resolution of Sloan Digital Sky Survey but at z=1 instead of z=0.05. Euclid will be 3 magnitudes deeper à Euclid Legacy = Super-Sloan Survey Euclid Simulation: Vis+NISP YJH image z~0.3 cluster of galaxies Ground Based Data: photo-z for Euclid Courtesy Euclid SWG Photo-z and OU-PHZ Requirements: accuracy = 0.05x(1+z) NIR images from NIR data Euclid à 4 optical band needed à u-band not needed. . Visible data obtained from ground based telescopes Euclid Q2C6 Nice, 17 October 2013 Euclid: sky coverage Euclid Q2C6 Nice, 17 October 2013 Data release: ground based + Euclid Year -3 T-3 start ground based observations (<2017) Yr -1 Ground DR1 All Euclid pointings set ready (2500 deg2) T-0 start Euclid nominal mission (2020) Yr+1 Ground DR2 ready (7500 deg2) Yr +3 Ground DR3 ready (15000 deg2) Euclid Q2C6 Nice, 17 October 2013 Dark Matter: reconstructed P(k) from wide survey Laureijs et al 2011, Euclid RB arXiv:1110.3193 . Courtesy H. Hoekstra, T. Kitching and the WL SWG Relevant scales for cosmic shear Input P(k) B-modes - Tomographic WL shear cross-power spectrum for 0.5 < z < 1.0 and 1.0 < z < 1.5 bins. - Percentage difference [expected – measured] power spectrum: recovered to 1% . Euclid Q2C6 Nice, 17 October 2013 NISP Performance: images/spectra/redshifts Courtesy A. Ealet, B. Garilli, W. Percival, L. Guzzo and the NISP and SWG GC, and Baugh and Merson True vs. measured redshift Euclid Q2C6 Nice, 17 October 2013 Galaxy Clustering: constraints on dark energy models Euclid: combined RSD and amplitude of GC Coupled model with βc=0.2 DGP Majoretto et al 2012 Euclid Q2C6 Nice, 17 October 2013 Forecasts for the primary cosmology programme DE constraints from Euclid: Constraints on γ and ns. Errors marginalised The Planck Collaboration. Ade et al 2013 over all other parameters. 68% confidence contours in (wp, wa). Modified Dark Matter Initial Conditions Dark Energy Gravity Parameter γ m ν /eV fNL wp wa FoM Euclid primary (WL+GC) 0.010 0.027 5.5 0.015 0.150 430 Euclid All 0.009 0.020 2.0 0.013 0.048 1540 Euclid+Planck 0.007 0.019 2.0 0.007 0.035 4020 Current (2009) 0.200 0.580 100 0.100 1.500 ~10 Improvement Factor 30 30 50 >10 >40 >400 Ref: Euclid RB arXiv:1110.3193 Assume systematic errors are under control Euclid Q2C6 Nice, 17 October 2013 Euclid Legacy Before • 12 billion sources ,3- Objects Euclid σ Euclid Galaxies at 1 Massive galaxies (1 decades; Galaxies in clusters of ~2x104 ~103 ? galaxies at z>1 Active Galactic Nuclei ~104 <103 • A reservoir of targets for JWST, galaxies (0.7 Lensing galaxies with arc and • Synergy with LSST, e-ROSITA, ~300,000 ~10-100 SKA rings Quasars at z > 8 ~30 None Euclid Q2C6 Nice, 17 October 2013 SimulationsAn Euclid/EIC of gravitational view arcs onand Einstein rings ringswith Euclid CFHTLS-w R+I+Z YJH CFHTLS-w R+I+Z YJH R+I+Z : great promises for detection SLACS (~2010 - HST) Galaxy-scale strong lensing with Euclid SLACS Euclid Legacy : after 2 months (66 months planned) Euclid: organisation and schedule Euclid Collaboration Euclid Euclid Project Science ESA EC Space Ground Segment Segment Launcher ESA ESA ESA/AE Ground OUs SDCs SVM PLM Instruments Observations MOC SOC ESA/Thales ESA/Astrium EC EC EC ESA/ESOC ESA/ESAC SWG: Science Euclid Consortium (EC): VIS NISP Products - 1200 members, EC EC EC - 120 Labs in 14 countries: Austria, Denmark, France, Finland,, Germany, Italy, The CCD SCS Netherlands, Norway, Portugal, Romania, Spain, ESA/e2v ESA/NASA/TIS Switzerland, UK + US/NASA and Berkeley labs. Euclid Q2C6 Nice, 17 October 2013 Schedule SGS Pipeline Model0 SGS Pipeline Model1 PDR VIS/NISP Delivery VIS/NISP Euclid Q2C6 Nice, 17 October 2013 Challenges for Euclid • Data processing: huge volume, heterogeneuous data, 10 SDCs • Shape measurements/systematics • Control of both multiplicative and additive biases • Photometric redshifts: • Ground based photometry in 4 bands : 15,000 deg2 (i.e. north and south) • Numerical simulations with power spectrum to a 1% accuracy : • Underlying physics: e.g. numerical simulations with baryons • Numerical simulations of a large number of DE, GR models • 103 to 105 simulations to estimate covariance matrices • Spectroscopic surveys to: • Calibrate deep photo-z and • Understand BAO and RSD samples Euclid Q2C6 Nice, 17 October 2013 Summary • The Euclid mission is now in implementation phase; • Euclid = 5 cosmological probes: WL, RSD, BAO, CL, ISW • Europe is leading one of the most fascinating and challenging question of modern physics and cosmology • Euclid Legacy = 12 billion sources, 50 million redshifts; – A mine of images and spectra for the community for several decades; – Synergy with LSST and e-ROSITA – A reservoir of targets for JWST, E-ELT, TMT, ALMA, VLT, SKA Euclid Q2C6 Nice, 17 October 2013