Gravitational Lensing with Euclid

Transcription

1 Gravitational Lensing with Euclid Y. Mellier on behalf of the Euclid Consortium Gravitational Lensing with Euclid GravLens, Leiden, JUL

2 Euclid Top Level Science Requirements Sector Dark Energy Test Gravity Dark Matter Initial Conditions Euclid Targets Measure the cosmic expansion history to better than 10% in redshift bins 0.7 < z < 2. Look for deviations from w = 1, indicating a dynamical dark energy. Euclid alone to give FoM DE > 400 ( 1-sigma errors on w p, & w a of 0.02 and 0.1 respectively) Measure the growth index, γ, with a precision better than 0.02 Measure the growth rate to better than 0.05 in redshift bins between 0.5< z < 2. Separately constrain the two relativistic potentials Ψ, Φ. Test the cosmological principle Detect dark matter halos on a mass scale between 10 8 and >10 15 M Sun Measure the dark matter mass profiles on cluster and galactic scales Measure the sum of neutrino masses, the number of neutrino species and the neutrino hierarchy with an accuracy of a few hundredths of an ev Measure the matter power spectrum on a large range of scales in order to extract values for the parameters σ 8 and n to a 1-sigma accuracy of For extended models, improve constraints on n and α wrt to Planck alone by a factor 2. Measure a non-gaussianity parameter : f NL for local-type models with an error < +/-2. DE equation of state: P/ρ = w, and w(a) = w p + w a (a p -a) Growth rate of structure formation: f ~ Ω γ ; FoM=1/(Δw a x Δw p ) > 400à ~1% precision on w s. Euclid Consortium Annual Meeting, May 30-June

3 WL probe: Cosmic shear over 0<z<2 : 1.5 billion galaxies shapes, shear and phot-z (u,g, r,i,z,y,j,h) with 0.05 (1+z) accuracy over 15,000 deg2 GC; BAO, RSD probes: 3-D positions of galaxies over 0.7<z<1.8 : 35 million spectroscopic redshifts with (1+z) accuracy over 15,000 deg2 Colombi, Mellier 2001 Source plane z2 Source plane z1 BAO RSD

4 Top Level Requirements for Weak Lensing R-WL.1-1: The survey area shall be greater than 15,000 deg 2 of the extra-galactic sky. R-WL.1-2:The average density of galaxies over the survey area that are useful for weak gravitational lensing shall be > 30 galaxies per arcmin 2. R-WL.1-3:The redshift distribution of the lensed galaxies shall have a median redshift greater than 0.8. R-WL.1-4: The measurements need to be controlled to a level such that the variance of the additive systematic signal σ 2 sys <10-7 and such that the multiplicative bias m< R-WL.1-5: The statistical scatter (RMS) of the errors in the measured photometric redshifts, in the range 0.2<z<2.0 shall be σ(z)/(1+z)<0.05. R-WL.1-6: The catastrophic failure fraction (fcat), shall be less than 10%. R-WL.1-7: The mean of the redshift distribution n(z) in each tomographic redshift bin shall be known to a precision of σ(<z>)/(1+z)<0.002

5 Measuring shear in next generation wide field cosmic shear surveys

6 Euclid Survey Machine:15,000 deg deg 2 deep Photometric redshifts: : External Photometry Space Euclid VIS and NIR observer of stars and galaxies sources, WL galaxies, spectra Wide and VIS Imaging NIR Photometry NIR Spectroscopy External Spectroscopy I AB =24.5 ; 10σ Y,J,H=24.0 ; 5σ erg.cm -2.s -1 ; 3.5σ I AB =26.5 ; 10σ Y,J,H=26.0 ; 5σ erg.cm -2.s -1 ; 3.5σ Other Euclid probes Tomographic WL survey Galaxy Redshift survey Dark Matter + Galaxy Power Spectra as function of look back time Planck, erosita, Cosmo. Simul. Cosmological explorer of gravity, dark matter, dark energy and inflation Legacy Science

7 Overview Gravitational Lensing with Euclid GravLens, Leiden, JUL

8 PLM, flight hardware, scientific instruments From Thales Alenia Italy, Airbus DS, ESA Project office and Euclid Consortium M2 mirror M1 mirror Telescope baseplate Gravitational Lensing with Euclid GravLens, Leiden, JUL

9 Plan From G. Racca Gravitational Lensing with Euclid GravLens, Leiden, JUL

10 VIS Courtesy: S. Pottinger, M. Cropper and the VIS team Cropper et al 2016:SPIE Gravitational Lensing with Euclid GravLens, Leiden, JUL

11 VIS in pictures (from the VIS team) Courtesy: Euclid Consortium VIS team Gravitational Lensing with Euclid GravLens, Leiden, JUL

12 Euclid : VIS imaging instrument Courtesy Mark Cropper, Sami M. Niemi and the VIS team Euclid CEFCA, Teruel, 23 Feb 2016

13 VIS: Simulation of M51 From J. Brinchmann z=0.1 z=0.7 Euclid will get the resolution of SDSS but at z=1 instead of z=0.05. Euclid will be 3 magnitudes deeper à Euclid Legacy = Super-Sloan Survey

14 VIS: Simulation of M51 From J. Brinchmann 2.4m z=0.1 z=0.1 Euclid will get the resolution of SDSS but at z=1 instead of z=0.05. Euclid will be 3 magnitudes deeper à Euclid Legacy = Super-Sloan Survey

15 NISP Courtesy: T. Maciaszek and the NISP team FoV: 0.55 deg2 Mass : 159 kg Telemetry: < 290 Gbt/day Size: 1m x 0.5 m x 0.5 m 16 2kx2K H2GR detectors 0.3 arcsec pixel on sky Limiting mag, wide survey AB : 24 (5 σ ) 3 Filters: Y ( nm), J (1192, 1544nm), H (1544, 2000nm) 4 grisms: 1B ( ), 1 orientation 0 3R ( ), 3 orientations 0, 90, 180 Maciaszek et al 2016:SPIE

16 NISP in pictures GWA STM (from the NISP team)) FWA STM Grism DM NI Warm electronics DM Model OA Gravitational Lensing with Euclid GravLens, Leiden, JUL NI-DS intergation

17 NISP-spectroscopy for Euclid From P. Franzetti, B. Garilli, A. Ealet, N. Fourmanoit & J. zoubian Gravitational Lensing with Euclid GravLens, Leiden, JUL

18 VIS Courtesy: S. Pottinger, M. Cropper and the VIS team and NISP Courtesy: T. Maciaszek and the NISP team FoV: 0.54deg2 FoV: 0.55 deg2 Mass : 133 kg Mass : 159 kg Telemetry: < 520 Gbt/day Telemetry: < 290 Gbt/day 36 4kx4K E2V CCDs, 12 micron pixels Size: 1m x 0.5 m x 0.5 m 0.1 arcsec pixel on sky 16 2kx2K H2GR detectors Limiting mag, wide survey AB : 24.5 (10 σ ) 0.3 arcsec pixel on sky 1 Filter: Y(R+I+Y): band pass nm Limiting mag, wide survey AB : 24 (5 σ ) 3 Filters: Y, J, H 4 grisms: 1B ( ),3R ( )

19 Euclid and the DM-dominated / DEdominated transition period Euclid Euclid redshift survey Euclid WL survey Accelerating Decelerating Plot inspired by the BOSS collaboration

20 Euclid Wide and Deep Surveys Euclid Deep From J.-C. Cuillandre and the Survey WG

21 Gravitational lensing with Euclid Euclid is optimised for lensing surveys Image quality: space telescope à very high accuracy on shapes Wide field and large samples of many types of sources Deep NIR photometry Pixel size samples the VIS PSF CCD E2E very well known devices for shape measurements Solid experienced teams leading WL, SL and Photo-z Euclid can address all aspects of gravitational lenses/lensing Cosmic shear cosmic magnification (stability photometry) Superclusters Clusters and groups of galaxies, Galaxy galaxy lensing Arcs and rings Microlensing

22 Science Working Groups T. Kitching,, J. Brinchmann, W. Percival, H. Hoekstra, L. Guzzo, C. Conselice, J. Weller H. Hoekstra L. Moscardini M. Meneghetti P. Fosalba J. Brinchmann E. Tolstoy J.-P. Beaulieu T. Kitching J. Weller J.-P. Kneib R. Teyssier D. Elbaz A. Ferguson M. Zapatero-Osorio M. Kilbinger J. Bartlett R. Gavazzi A. Cimatti E. Kerins L. Guzzo N. Aghanim L. Amendola J.-G. Cuby B. Poggianti I. Hook W. Percival C. Baccigalupi M. Kunz S. Toft C. Conselice C. Tao Y. Wang M. Viel Position transiens B. Altieri C. Tao (EC)

23 Euclid WL Science Wrking Group From H. Hoekstra

24 Euclid Science Ground Segment and OUs From M. Sauvage and SGS PO

25 From G. Racca Plan

26 Technical Performance Measure Requirement CBE Image Quality FWHM 800nm) 180 mas 163 mas ellipticity 15.0% 5.9% R2 800 nm) VIS Channel NISP Channel ellipticity stability σ(εi) (with straylight+persistence+cosmics) 2.00E E- 04 R2 stability σ(r2)/<r2> 1.00E E- 03 Plate scale 0.10 " 0.10 " Out- of- band avg red side 1.00E E- 05 Out- of- band avg blue side 1.00E E- 04 Slope red side 35 nm 15 nm Slope blue side 25 nm 8 nm ree50 (@1486nm) 400 mas 217 mas ree80 (@1486nm) 700 mas 583 mas Plate scale 0.30 " 0.30 " Sensitivity VIS SNR (for mab = 24.5 sources) NISP- S SNR (@ 1.6um for 2xe- 16 erg cm- 2 s- 1 source) NISP- P SNR (for mab = 24 sources) NISP- S Performance Purity Completeness Survey Wide Survey Coverage Y- band J- band H- band % 72% 45% ,000 deg2 15,000 ESA Mission PDR October 2015 successful: Euclid performances meet the scientific and survey requirements Image quality of the system fully in line with needs. Ellipticity, R 2 stability and Non-convolutive errors performance dictated mainly by ground processing Purity not compliant with current data processing methods but expected to be recovered with Euclid specific algorithms (not yet installed at this stage). Survey length [years]

27 Euclid Weak Lensing Survey: from observational signatures to the dark universe What is the expansion rate of the Universe? What is the expansion rate of the Universe? Understanding Dark Energy WL Survey DM power spectrum, tomogr" DM power spectrum" How does structure form within this background? Understanding energy-density, gravity What are the neutrino masses, matter density? Understanding energy-density What is f nl, which quantifies non- Gaussianity? GR-horizon effects Understanding Inflation, GR Does the potential change along line-of-sight to CMB Understanding DE, GR

28 Euclid: combining WL and GC data Euclid : DM power spectrum Euclid: Galaxy power spectrum 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%. V eff 19 h - 3 Gpc 3 75x larger than SDSS RedshiPs 0.7<z<1.85 Percentage difference [expected measured] power spectrum: recovered to 1%.

29 Euclid Forecast (2015) Planck + Current BAO MCMC Chains w 0 w a Planck + BAO + Euclid Weak Lensing Planck + BAO + Euclid WL+ Euclid GC From T. Kitching & Euclid Forecast IST h σ 8 Ω B n Ω DE Ω M w 0 w a h σ 8 Ω B n Ω DE

30 Euclid Post-Planck Forecast for the Primary Program Ref: Euclid RB arxiv: Modified Gravity Dark Matter Initial Conditions Dark Energy Parameter γ m ν /ev f NL w p w a FoM = 1/(Δw 0 Δw a ) Euclid primary (WL+GC) EuclidAll (clusters,isw) Euclid+Planck Current (2009) ~10 Improvement Factor >10 >40 >400 DE equation of state: P/ρ = w, and w(a) = w p + w a (a p -a) From Euclid data alone, get FoM=1/(Δw a x Δw p ) > 400à ~1% precision on w s. Growth rate of structure formation: f ~ Ω γ ;. Notice neutrino constraints -> minimal mass possible ~ 0.05 ev

31 Euclid forecast: neutrinos and relativistics species Amendola et al 2013 Amendola et al 2016 If Σ >0.1 ev à Euclid spectroscopic survey will be able to determine the neutrino mass scale independently of the model cosmology assumed. If Σ <0.1 ev à the sum of neutrino masses, and in parkcular the minimum neutrino mass required by neutrino oscillakons, can be measured in the context of the Λ-CDM

32 Euclid and the next generation wide field VIS/NIR surveys Objects Euclid Before Euclid From J. Brinchmann 2013 Euclid in 5 yrs 15, 000 deg2 Galaxies at 1 < z < 3 with precise mass measurement ~2x10 8 ~5x Massive galaxies (1< z< 3) Few hundreds Few tens Hα Emitters with metal abundance measurements at z~2-3 ~ ? ~10 4? 100 Galaxies in clusters of galaxies at z > 1 ~1.8x10 4 ~10 3? 10 HST in 15 yrs <20 deg2 Active Galactic Nuclei galaxies (0.7 < z< 2 ) ~10 4 <10 3 Dwarf galaxies ~ Teff ~400K Y dwarfs ~few 10 2 <10 Lensing galaxies with arcs and rings ~150,000 ~ Quasars at z > 8 ~30 None Targets for JWST, E-ELT, TMT, Subaru, VLT, MSE, etc Synergy with LSST, erosita, Subaru/HSC, Planck, SKA

33 Simulations of gravitational arcs and Einstein rings with Euclid CFHTLS-w R+I+Z YJH CFHTLS-w R+I+Z YJH

34 Strong lenses seen with Euclid: Galaxy-galaxy lensing Galaxy-QSO lensing Gravitational arcs Probing haloes with strong lensing Compound lenses Multiple images in clusters Exotic lenses Giant arcs in clusters (Boldrin et al 2015) 1300 arcs wit L/w > arcs with L/w > 5 Galaxy-galaxy lensing (Collett 2015) 140,000 lenses in the wide survey 650 double source plane lenses

35 SLACS (~ HST) Galaxy-scale strong lensing with Euclid

36 SLACS Euclid VIS Legacy : after 2 months (66 months planned)

37 Clusters of galaxies with Euclid Probe of peaks in density distribution Nb density of high mass, high redshift clusters very sensitive to primordial non-gaussianity and deviations from standard DE models Euclid data will get for free: Λ-CDM: all clusters with M> Msol detected at 3-σ up to z=2 à 60,000 clusters with 0.2<z<2, à clusters at z > 1. ~ 5000 giant gravitational arcs à accurate masses for the whole sample of clusters à dark matter density profiles on scales >100 kpc à Synergy with Planck and erosita Max BCG erosita Euclid

38 Scaling relations with Euclid Clusters Expected precision on the mean mass of clusters with gravitational shear in bin of Δlog(M200)=0.2 and Δz=0.1 Survey of 15,000 deg 2 3.0x10 14 M sol 2.0x10 14 M sol 1.0x10 14 M sol Λ-CDM Planck cosmology Tinker mass function Shape noise of 0.3 Euclid has the potential to calibrate the mean mass, and hence the scaling relations, to 1% out to z=1.0 and to 10% out to z=1.6 Sartoris et al 2015

39 Cosmology with Euclid Clusters of Galaxies NC: Cluster Number counts ; PS: Cluster Power Spectrum, SR: Cluster Scaling Relation

40 3 fields observed every 17mn in H, every 12 hours in VIS, J and Y Microlensing survey? Mini-survey during commissioning (24h), then 4x1 months survey Measuring cold Earth abundance and mass function 35 planets/months (5 Earth/ month, 15 Neptune/month) Getting constraints on free-floating planets 15 free floating planets/month Euclid will complement the parameter space probed by RV and Kepler Measuring the cold planet mass function below 1 Earth mass From Beaulieu and Penny et al 2013 Possibility of simultaneous Euclid-WFIRST?

41 Summary

42 Euclid Wide and Deep and Lensing Surveys Euclid Wide: Euclid Deep: deg 2 outside the galactic and ecliptic planes 12 billion sources (3-σ) 1.5 billion galaxies with Very accurate morphometric information (WL) Visible photometry: (u), g, r, i, z, (R +I+Z) AB=24.5, 10.0 σ + NIR photometry : Y, J, H AB = 24.0, 5.0σ Photometric redshifts with 0.05(1+z) accuracy 35 million spectroscopic redshifts of emission line galaxies with accuracy Halpha galaxies within 0.7 < z < 1.85 Flux line: erg.cm -2.s -1 ; 3.5σ 1x10 deg 2 at North Ecliptic pole + 1x20 deg 2 at South Ecliptic pole + 1x10 deg 2 South Equatorial field 10 million sources (3-σ) 1.5 million galaxies with Very accurate morphometric information (WL) Visible photometry: (u), g, r, i, z, (R +I+Z) AB=26.5, 10.0 σ + NIR photometry : Y, J, H AB = 26.0, 5.0σ Photometric redshifts with 0.05(1+z) accuracy spectroscopic redshifts of emission line galaxies with accuracy Halpha galaxies within 0.7 < z < 1.85 Flux line: erg.cm -2.s -1 ; 3.5σ Euclid NL LSS Workshop IAP, 24 May 2016

43 Overview mission timeline End PLM FM Assembly 2008 Definition Implementation VIS FM NISP FM delivery delivery End S/C FM Integration 2020 Operations Proposal selection Mission adoption Launch End nominal mission Science with Euclid will start in 2022 with Q1 and in 2023 with DR1

44 Euclid: a space mission design for gravitational lensing surveys Euclid is progressing well and meet all the weak lensing requirements Use 5 cosmological probes, with at least 2 independent, and 3 power spectra Explore the dark universe: DE, DM (neutrinos), MG, inflation, biasing Explore the transition DM-to-DE-dominated universe periods Get the percent precision on w and the growth factor γ Complementarity with Planck: probes, data, cosmic periods -à CMB /Galaxies cross correlations Synergy with New Gen wide field surveys: LSST, WFIRST, e-rosita, SKA Provide 150,000 strong lenses à propoerties of DM haloes at dwarf galaxies, galaxies, groups, clusters of galaxies scales in the range of redshift 0. < z < 2 Euclid =12 billion sources, 35 million redshifts, 1.5 billion shapes/photo-z of galaxies; A mine of images and spectra for the community for years; A reservoir of strong lenses targets for JWST, E-ELT, TMT, ALMA, VLT Launch: 2020, releases: 2500 deg 2 public in 2023, 7500 deg 2 in 2025, final 2027