Fundamental Cosmology with EUCLID

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1 Fundmentl Cosmology with EUCLID Rphel, Euclid, The School of Athens, Rome Luc Amendol University of Heidelberg nd ESTEC INAF/Rom 009

2 The reconstruction of spce-time geometry with Euclid Drk mtter nd infltion with Euclid Synergy of Euclid with Plnk, LHC, Gi, EELT

3 Cosmic degenercy The bckground expnsion only probes H (z bckground The mtter clustering growth probes ( k, z perturbtions '' (1 H H ' 3 m 0

4 Wht bckground hides perturbtions revel The most generl (liner, sclr metric t first-order bckground ds [(1 dt (1 ( dx dy dz ] Full metric reconstruction t first order requires 3 functions H ( z ( k, z ( k, z perturbtions

5 Two free functions ds [(1 dt (1 ( dx dy dz ] At the liner perturbtion level nd sub-horizon scles modified Poisson s eqution k 4 G Q( k, m m non-zero nisotropic stress ( k,

6 Modified Grvity t the liner level sclr-tensor models,0 * ' ' ( ' 3 ' ( ( F F F F F F F FG G Q cv 0, ( 1, ( k k Q stndrd grvity DGP 1 3 ( 1 ; ( w Hr Q DE c f(r R k m R k m R k m R k m FG G Q cv,0 * 1 (, ( Lue et l. 004; Koym et l. 006 Ben et l. 006 Hu et l. 006 Tsujikw 007 coupled Guss-Bonnet see L. A., C. Chrmousis, S. Dvis (... ( Q Boisseu et l. 000 Acquviv et l. 004 Schimd et l. 004 L.A., Kunz &Spone 007

7 Reconstruction of the metric ds [(1 dt (1 ( dx dy dz ] mssive prticles respond to Ψ H ' k '' (1 H mssless prticles respond to Φ-Ψ perp ( dz

8 Reconstruction of the metric Correltion of glxy positions: glxy clustering P gl ( k, z, (1 ' b b ( k, z Correltion of glxy ellipticities: glxy wek lensing P ellipt ( k, z (

9 The Euclid theorem Observbles: Conservtion equtions: b P( k, z, trnsv ' P( k, z, rd / P( k, z, trnsv 1 b z Pellipt ( k, z dz' K( z'( 5 unknown vribles: 0 b( k, z, ( k, z, ( k, z, ( k, z, ( k, z We cn mesure 3 combintions nd we hve theoreticl reltions ' 3' H k ' H Theorem: lensing+glxy clustering llows to mesure ll (totl mtter perturbtion vribles t first order without ssuming ny specific grvity theory

10 The Euclid theorem Observbles: Conservtion equtions: b P( k, z, trnsv ' P( k, z, rd / P( k, z, trnsv 1 b z Pellipt ( k, z dz' K( z'( 5 unknown vribles: 0 b( k, z, ( k, z, ( k, z, ( k, z, ( k, z We cn mesure 3 combintions nd we hve theoreticl reltions ' 3' H k ' H Theorem: lensing+glxy clustering llows to mesure ll (totl mtter perturbtion vribles t first order without ssuming ny specific grvity theory

11 L = crossover scle: r r L L S V V An exmple: DGP d 1 r 1 r (Dvli, Gbddze, Porrti x g H (5 R 5D grvity domintes t low energy/lte times/lrge scles 4D grvity recovered t high energy/erly times/smll scles (5 8 3 H G L L brne d 4 x g R 5D Minkowski bulk: infinite volume extr dimension grvity lekge

Modified Grvity predictions 3 1 1 0, ( 3 ' ' (1 '' m k m k k Q Q k H H 0.70 0.65 (1 (1 1 1 ( m s w Q 0.

12 Modified Grvity predictions , ( 3 ' ' (1 '' m k m k k Q Q k H H (1 (1 1 1 ( m s w Q (1 ( log log w w d d s m ( 1 ( k f M k s DGP f(r m s w s H c k w w w (1 (1 1 clustered DE

13 Euclid vs. gmm current DGP Euclid LCDM tomogrphic wek lensing glxy power spectrum (redshift distortions

14 ncient questions for Euclid wht wht is the is the nture sky of drk mde mtter of? which re the infltionry where do we initil come conditions from?

15 Euclid vs. drk mtter drk mtter hlos from wek lensing mps of clusters drk mtter bundnce from power spectrum shpe drk mtter clustering from cluster bundnce neutrino mss from power spectrum shpe

16 Euclid cosmologicl bounty Neutrino mss error error m N 0.03 ev 0.3 Infltionry spectrum error error n s Primordil non gussinity error f NL 5

17 Euro-Synergy Plnck 009 LHC 009 Gi 011 EELT 00

18 LHC (beyond the Higgs Stndrd model is complete but... no unifiction of forces nd prticles no consistent inclusion of grvity Answer: supersymmetry Answer: string theory Consequence for cosmology: the lightest supersymmetric prticle is perfect cold drk mtter cndidte Consequence for cosmology: the grvity lekge into the extr-dimensions required by strings could explin ccelertion

19 EELT

20 010 EELT tody......ten yers lter sec / 1 1 ( (1 ( ( ( ( cm z z c v H z H z t H z t t t t t t z yr s s s Sndge effect

21 CODEX t EELT 350 S / N Liske et l N QSO 1/ 5 1 z 1.8 cm / s lrge colleting re high resolution spetrogrphs stble, low-peculir motion trgets: Lymn-lph lines

22 Euclid rnge Blbi & Quercellini 007

23 Gi: Complete, Fint, Accurte Hipprcos Gi Mgnitude limit 1 0 mg Completeness mg Bright limit 0 6 mg Number of objects million to V = million to V = million to V = 0 Effective distnce 1 kpc 50 kpc Qusrs None 5 x 10 5 Glxies None Accurcy 1 millircsec 7 µrcsec t V = µrcsec t V = µrcsec t V = 0 Photometry -colour (B nd V Low-res. spectr to V = 0 Rdil velocity None 15 km/s to V = Observing Pre-selected Complete nd unbised

24 The cosmic reference frme (t Binchi I 1 b(t c(t

25 Anisotropic drk energy Mot & Koivisto 008, Brrow, Sh, Bruni, Rodrigues nd mny others.. DE C. Quercellini, P. Cbell, L.A., M. Qurtin, A. Blbi 009 H R 10 4, H t ny z

26 A Europen Drem Tem The combintion of wek lensing nd clustering llows the full recostruction of the spce-time geometry In ddition, Euclid will provide unique new constrints on drk mtter nd initil conditions Togther with Plnck, LHC, Gi, EELT, Euclid will drw new 3D tls of the universe Euclid LHC EELT Gi

27 Cosmic Degenercy 3 Tomit 001 Celerier 001 Alnes & Amrzguioi 006,07 Bssett et l. 07 Clifton et l. 08 Notri et l Mrr et l. 08 Grci-Bellido & Hugbolle 008 Grci-Bellido & Hugbolle 008 void model

28 One null cone time H 0 H 0 comoving dist. now z 0 H ( z 1 z z 1

29 One null cone One null cone time H out H in com. dist. now z 0 H ( z, r 1 z z 1 VOID

30 Two null cones re better thn one! time H out H in t now t com. dist. now z 0 H ( z, r 1 z H (z VOID z 1 Mshhoon & Prtovi 1985 Uzn, Clrkson & Ellis 007 Qurtin, Quercellini, L.A. 009

31 Cosmology nd modified grvity in lbortory in the solr system }very limited time/spce/energy scles; only bryons t strophysicl scles complicted by non-liner/nongrvittionl effects t cosmologicl scles unlimited scles; mostly liner processes; bryons, drk mtter, drk energy!

yer cm v sec/ / 1 ( 1 z H ( z H sec / 1 1 ( (1 ( ( ( ( 1

32 yer cm v sec/ / 1 ( 1 z H ( z H sec / 1 1 ( (1 ( ( ( ( cm z z c v H z H z t H z t t t t t t z yr s s s

34 sec / 1 1 ( (1 ( ( ( ( cm z z c v H z H z t H z t t t t t t z yr s s s Corsniti, Huterer, Melchiorri 007 Blbi & Quercellini 007 sec / ( cm c yrs t H

36 CODEX t EELT 010 tody......ten yers lter

37 CODEX t EELT 350 S / N Liske et l N QSO 1/ 5 1 z 1.8 cm / s lrge colleting re high resolution spetrogrphs stble, low-peculir motion trgets: Lymn-lph lines

38 Two null cones re better thn one! time H out H in t now t com. dist. now z 0 z 1 VOID M. Qurtin & L. A. 009

39 Evolution Rest of the Universe Rest of the Universe Us Us Ptolemic system, I century LTB void model, XXI century

40 Cosmic Prllx H 10 0 t 9 10 rd 9 00s strometric stellites GAIA, SIM, Jsmine etc: µs LTB void model Quercellini, Qurtin & LA, Phys. Rev. Lett. 009 rxiv

42 LTB models Grci-Bellido & Hugbolle 008 LTB void model

44 Grci-Bellido & Hugbolle 008 Quercellini, Qurtin & LA, rxiv

45 Cosmic Prllx Quercellini, Qurtin & LA, rxiv

Gi: Complete, Fint, Accurte Hipprcos Gi Mgnitude limit 1 0 mg Completeness 7.3 9.

46 Gi: Complete, Fint, Accurte Hipprcos Gi Mgnitude limit 1 0 mg Completeness mg Bright limit 0 6 mg Number of objects million to V = million to V = million to V = 0 Effective distnce 1 kpc 50 kpc Qusrs None 5 x 10 5 Glxies None Accurcy 1 millircsec 7 µrcsec t V = µrcsec t V = µrcsec t V = 0 Photometry -colour (B nd V Low-res. spectr to V = 0 Rdil velocity None 15 km/s to V = Observing Pre-selected Complete nd unbised

47 Grci-Bellido & Hugbolle 008 Quercellini, Qurtin & LA, rxiv

48 Grci-Bellido & Hugbolle 008 Quercellini, Qurtin & LA, rxiv

49 Not only LTB (t Binchi I 1 b(t c(t

50 Current limits on nisotropy H R 10 4 t z = 1000 H H H H H 10 8? t z = 0 in ΛCDM universe t z = 0 in nisotropic drk energy

51 Anisotropic drk energy Mot & Koivisto 008, Brrow, Sh, Bruni, Rodrigues nd mny others.. DE C. Quercellini, P. Cbell, L.A., M. Qurtin, A. Blbi 009 H R 10 4, H t ny z

52 WERBUNG DARK ENERGY theory nd observtions L. A. nd S. Tsujikw Cmbridge University Press mid 010

53 Breking the degenercies The tsk of understnding the nture of Drk energy is plgued by severl cosmic degenercies We need to combine wek lensing nd clustering to reconstruct the metric t first order We need to use rel-time observbles to distinguish between rel nd pprent ccelertion Together with the Cosmic Prllx we cn reconstruct the full 3D picture of cosmic kinemtics! Euclid EELT Gi

54 rdil trnsverse globl locl Sndge effect Peculir ccelertion Cosmic prllx Proper ccelertion

55 Rel-time Cosmology rdil trnsverse globl Expnsion rte nisotropy locl Grvity t glctic scles: eg Newton vs Modif. Grv.

56 ToDo figur redshiftdrift void figur cover book

57 Peculir Accelertion pec GM ( r sin r The PA is direct probe of the grvittionl potentil: it does not ssume viriliztion or hydrosttic equilibrium.

58 Peculir Accelertion s( v cm t M v sin 14 sec 10yr 10 M cc NFW ( r, rs rv / c r r 1 r s r s rs 0.5Mpc log(1 C ( r / rs r r s r r s 1 (1 r r s r R c / cos Mss r s Andromed Virgo Com kpc 0.55 Mpc 0.9 Mpc

59 s Peculir Accelertion cm T M v v sin 14 sec 10yr 10 M rs 0.5Mpc r log(1 rs C ( r / rs r 1 r (1 r ( r s s different lines of sight L.A., A. Blbi, C. Quercellini, stro-ph rxiv/ Phys.Lett.B660:81,008

60 PA versus Sndge effect LCDM Cluster Mss

61 Peculir ccelertion in the Glxy Cn we use the peculir ccelertion to discriminte mong competing grvity theories? Steps: model the glxy s disc+cdm hlo nd derive the peculir ccelertion signl model the glxy s disc in modified grvity (MOND nlyse the different morphology of the signl in the Milky wy

62 Spirl glxy: Newton test prticle outside the disc, where the presence/bsence of CDM hlo is more influent. Disc: Kuzmin potentil, K MG R z h 1/ K MG R z h CDM hlo: logrithmic L 1 v o logr c R z q The totl line of sight ccelertion: MG s,k sin R g 1 tn h R g v 0 R g 1 tn q s,l sin R c R g 1 tn q C. Quercellini, L.A., A. Blbi 008 rxiv: v s,k s,l t

63 Spirl glxy: MOND Beckenstein-Milgrom modified Poisson eqution 4G 0 peculir ccelertion in MOND: s,m MG M G R 4 g 4 1 tn h R g R g 1 tn h R g 1/ sin

64 Most ccelerted globulr clusters v 1.5cm / sec/ yr

65 Newton vs. MOND

Memo for the future The Sndge-Loeb effect is direct mesure of the expnsion/ccelertion of the Universe The Cosmic Prllx is direct test of nisotropy The Peculir/Proper Accelertion is direct mesure of

66 Memo for the future The Sndge-Loeb effect is direct mesure of the expnsion/ccelertion of the Universe The Cosmic Prllx is direct test of nisotropy The Peculir/Proper Accelertion is direct mesure of the grvittionl potentil Full 3D picture of cosmic nd locl kinemtics! A sensitivity of 1 cm/sec could be chieved with the next genertion of ELTs A sensitivity of 1-10 mu rcsec will be chieved by plnned strometric missions like GAIA, SIM, Jsmine New observbles for DE, cosmology nd grvity theories!

Outline. I. The Why and What of Inflation II. Gauge fields and inflation, generic setup III. Models within Isotropic BG

Outline. I. The Why and What of Inflation II. Gauge fields and inflation, generic setup III. Models within Isotropic BG Outline I. The Why nd Wht of Infltion II. Guge fields nd infltion, generic setup III. Models within Isotropic BG Guge-fltion model Chromo-nturl model IV. Model within Anisotropic BG Infltion with nisotropic