Euclid and MSE Y. Mellier IAP and CEA/SAp www.euclid-ec.org Euclid and MSE CFHT Users Meeting, Nice 02 May, 2016
Euclid Primary Objectives: the Dark Universe Understand The origin of the Universe s accelerating expansion The properties and nature of Dark Energy and Gravity, Probe the effects of Dark Energy, Dark Matter and Gravity by: Using at least 2 independent but complementary probes (5) Tracking their observational signatures on the o Geometry of the universe: Weak Lensing (WL), Galaxy Clustering (GC) o Cosmic history of structure formation: WL, Redshift-Space Distortion (RSD), Clusters of Galaxies (CL) Controling systematics to an unprecedented level of accuracy.
The ESA Euclid space mission PLM+SVM: 2010-2020 VIS imaging: La mission Euclid de l ESA: objectifs scientifiques 2010-2020 Launch date: Dec 2020? (VIS team) Soyuz@Kourou NIR spectro-imaging 2010-2020 (NISP team) Surveys: 2010-2028 (Survey WG) SGS: 2010-2028 Survey : 6 yrs, 15,000 deg2 Commisionning SV SWG: Ground data 2019-2028 Euclid opération: 5.5 yrs:euclid Wide+Deep +: SNIa, mu-lens, MW? ~100 PB data processing (EC-SGS team) Science analyses
Ground Observation: Imaging (From J.-C. Cuillandre) Euclid and MSE CFHT Users Meeting, Nice 02 May, 2016
Euclid Survey Euclid Wide: 15000 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 0.001 accuracy Halpha galaxies within 0.7 < z < 1.85 Flux line: 2. 10-16 erg.cm -2.s -1 ; 3.5σ
Euclid deep and calibration fields VVDS Deep CDFS EDFN EDFS GOODS North COSMOS
Euclid Survey Euclid Deep: 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 150 000 spectroscopic redshifts of emission line galaxies with 0.001 accuracy Halpha galaxies within 0.7 < z < 1.85 Flux line: 5. 10-17 erg.cm -2.s -1 ; 3.5σ
Euclid Legacy 12 billion sources, 3-σ Objects Euclid Before Euclid 35 million redshifts; Galaxies at 1<z<3 with precise mass measurement ~2x10 8 ~5x10 6 Huge samples: large numbers, large diversity of sources and samples, rare objects Reservoir of targets for JWST, E-ELT, TMT, Subaru, VLT, MSE, etc Synergy with LSST, e- ROSITA, Subaru/HSC, Planck, SKA Massive galaxies (1<z<3)) Few hundreds Few tens Hα Emitters with metal abundance measurements at z~2-3 Galaxies in clusters of galaxies at z>1 Active Galactic Nuclei galaxies (0.7<z<2) Dwarf galaxies ~ 4 10 7? ~10 4? ~1.8x10 4 ~10 3? ~10 4 <10 3 ~10 5 Teff ~400K Y dwarfs ~few 10 2 <10 Lensing galaxies with arc and rings ~150,000 ~10-1000 Quasars at z > 8 ~30 None
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>2.10 14 Msol detected at 3-σ up to z=2 à 60,000 clusters with 0.2<z<2, Max BCG erosita Euclid à 1.8 10 4 clusters at z>1. ~ 5000 giant gravitational arcs à very accurate masses for the whole sample of clusters (WL) à dark matter density profiles on scales >100 kpc à Synergy with Planck and erosita
SLACS (~2010 - HST) Galaxy-scale strong lensing with Euclid
SLACS Euclid VIS Legacy : after 2 months (66 months planned)
Prospect for detecting high-z Ly-a emitters From Matthee et al (2015)
Clustering redshifts V.Scottez Scottez, thesis 2015 etphd al 2016: VIPERS+CFHTLS ß Uses 10 109 galaxy position and photometric data of Euclid ß Uses 35 106 galaxy redshifts of Euclid Euclid and MSE CFHT Users Meeting, Nice 02 May, 2016
Clustering redshifts V.Scottez Scottez, thesis 2015 etphd al 2016: VIPERS+CFHTLS ß Uses 10 109 galaxy position and photometric data of Euclid BUT Euclid will only observe emission line galaxies NOT all WL galaxies (needed for clustering) ß Uses 35 106 galaxy redshifts of Euclid Euclid and MSE CFHT Users Meeting, Nice 02 May, 2016
MSE and Euclid
MSE: Euclid North Spectroscopic follow up Large very deep spectroscopic sample to calibrate photo-z in Euclid Deep Fields (I=26.5 extended, 10-σ): 5000 redshifts over 20 deg 2 Very deep spectroscopic sample to measure clustering redshifts in Euclid Deep Fields (emission and absorption line galaxies): 100, 000 redshifts Euclid Wide Survey (absorption line galaxies): 100,000 1 million redshifts Spectroscopy of arcs/rings in the Euclid Wide and Deep Field: 75000 redshifts Spectroscopic survey of Euclid clusters of galaxies (redshifts, velocity dispersion, substructures): 30000 clusters, 5000 at z>1 Spectroscopic surveys of z > 8 QSOs and z>7 Ly emitter galaxies: 10-10000 Spectroscopic survey of the Euclid dwarf galaxies sample: 50, 000 Spectroscopic survey of Euclid T 400K Y dwarfs: few 100
Euclid and MSE: time needed (from Côté et al : Feasibility Study Report)
Euclid and MSE: time needed (from Côté et al : Feasibility Study Report)
MSE: Euclid North Spectroscopic follow up Large very deep spectroscopic sample to calibrate photo-z in Euclid Deep Fields (I=26.5 extended, 10-σ): 5000 redshifts over 20 deg 2 Very deep spectroscopic sample to measure clustering redshifts in Euclid Deep Fields (emission and absorption line galaxies): 100, 000 redshifts Euclid Wide Survey (absorption line galaxies): 100,000 1 million redshifts Spectroscopy of arcs/rings in the Euclid Wide and Deep fields: 75000 redshifts Spectroscopic survey of Euclid clusters of galaxies (redshifts, velocity dispersion, substructures): 30000 clusters, 5000 at z>1, Spectroscopic surveys of z > 8 QSOs and z>7 Ly emitter galaxies: 10-10000 Spectroscopic survey of the Euclid dwarf galaxies sample: 50, 000 Spectroscopic survey of Euclid T 400K Y dwarfs: few 100 à Considerable amount of targets (nb of spectra, nb of fields) and exposure times: Between 100 to 1000 nights with MSE. Huge gain in deep fields.
Euclid releases and MSE operation Launch in Q4 2020, survey starting about 3 months after Wide survey (ground +space data) 2500 deg 2 public in 2023, 7500 deg 2 public in 2025, 15000 deg 2 public and final 2027 Deep Survey (ground + space date) 40 deg 2 public in 2023-2027 10 deg 2 North Ecliptic Pole within the erosita North deep 10 deg 2 South approaching Equatorial (exact field TBD) 20 deg 2 close to South Ecliptic Pole (exact position TBD) + several calibration fields (including COSMOS) à MSE may be too late for calibration of photo-z of wide fields but on time for spectroscopic follow up of Euclid targets, calibration of photo-z of deep fields and spectroscopic samples for clustering redshifts in deep and wide fields