Euclid and MSE. Y. Mellier IAP and CEA/SAp.

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Euclid and MSE Y. Mellier IAP and CEA/SAp www.euclid-ec.

1 Euclid and MSE Y. Mellier IAP and CEA/SAp Euclid and MSE CFHT Users Meeting, Nice 02 May, 2016

2 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.

3 The ESA Euclid space mission PLM+SVM: VIS imaging: La mission Euclid de l ESA: objectifs scientifiques Launch date: Dec 2020? (VIS team) Soyuz@Kourou NIR spectro-imaging (NISP team) Surveys: (Survey WG) SGS: Survey : 6 yrs, 15,000 deg2 Commisionning SV SWG: Ground data Euclid opération: 5.5 yrs:euclid Wide+Deep +: SNIa, mu-lens, MW? ~100 PB data processing (EC-SGS team) Science analyses

4 Ground Observation: Imaging (From J.-C. Cuillandre) Euclid and MSE CFHT Users Meeting, Nice 02 May, 2016

5 Euclid Survey Euclid Wide: 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

6 Euclid deep and calibration fields VVDS Deep CDFS EDFN EDFS GOODS North COSMOS

7 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 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

8 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 ~ ? ~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 ~ 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

9 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, Max BCG erosita Euclid à 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

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

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

12 Prospect for detecting high-z Ly-a emitters From Matthee et al (2015)

13 Clustering redshifts V.Scottez Scottez, thesis 2015 etphd al 2016: VIPERS+CFHTLS ß Uses galaxy position and photometric data of Euclid ß Uses galaxy redshifts of Euclid Euclid and MSE CFHT Users Meeting, Nice 02 May, 2016

14 Clustering redshifts V.Scottez Scottez, thesis 2015 etphd al 2016: VIPERS+CFHTLS ß Uses galaxy position and photometric data of Euclid BUT Euclid will only observe emission line galaxies NOT all WL galaxies (needed for clustering) ß Uses galaxy redshifts of Euclid Euclid and MSE CFHT Users Meeting, Nice 02 May, 2016

15 MSE and Euclid

16 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: redshifts Spectroscopic survey of Euclid clusters of galaxies (redshifts, velocity dispersion, substructures): clusters, 5000 at z>1 Spectroscopic surveys of z > 8 QSOs and z>7 Ly emitter galaxies: Spectroscopic survey of the Euclid dwarf galaxies sample: 50, 000 Spectroscopic survey of Euclid T 400K Y dwarfs: few 100

17 Euclid and MSE: time needed (from Côté et al : Feasibility Study Report)

18 Euclid and MSE: time needed (from Côté et al : Feasibility Study Report)

19 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: redshifts Spectroscopic survey of Euclid clusters of galaxies (redshifts, velocity dispersion, substructures): clusters, 5000 at z>1, Spectroscopic surveys of z > 8 QSOs and z>7 Ly emitter galaxies: 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.

20 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, deg 2 public and final 2027 Deep Survey (ground + space date) 40 deg 2 public in 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

Euclid. Mapping the Geometry of the Dark Universe. Y. Mellier on behalf of the. Euclid Consortium.

Euclid. Mapping the Geometry of the Dark Universe. Y. Mellier on behalf of the. Euclid Consortium. Mapping the Geometry of the Dark Universe Y. Mellier on behalf of the http://www.euclid-ec.org Instrument Overall WP Breakdown VG :1 The ESA mission: scientific objectives Understand the origin of the