Neutrinos in Cosmology (IV)

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1 Neutrinos in Cosmology (IV) Sergio Pastor (IFIC Valencia) Cinvestav 8-12 June 2015

2 Outline Prologue: the physics of (massive) neutrinos IntroducBon: neutrinos and the history of the Universe Basics of Cosmology 1st ProducBon and decoupling of relic neutrinos 2nd

3 Outline The radiabon content of the Universe (N eff ) Neutrinos and Primordial Nucleosynthesis Neutrino oscillabons in the Early Universe 2nd Massive neutrinos as Dark MaNer 3rd

4 Outline Effects of neutrino masses and N eff on cosmological observables Present bounds on neutrino properbes from cosmology 3rd Future sensibvibes on neutrino physics from cosmology

5 Present bounds on neutrino properbes from cosmology

6 Neutrino masses Data on flavour oscilla/ons do not fix the absolute scale of neutrino masses ev 3 1 NH IH solar! (ev) 0.3 atm NORMAL atm INVERTED 0.1 solar m 0 (ev)

7 Neutrinos as Dark Ma<er Neutrinos are natural DM candidates h 2 = i m i 93.2 ev < 1 i m i 46 ev < m 0.3 m i 15 ev i They stream freely un/l non- rela/vis/c (collisionless phase mixing) Neutrinos are HOT Dark MaNer (large thermal mo/on) First structures to be formed when Universe became ma<er dominated are very large Ruled out by structure forma/on CDM Massive Neutrinos can s/ll be subdominant DM: limits on m from Structure Forma/on (combined with other cosmological data)

8 How to get a bound (measurement) of neutrino masses from Cosmology Fiducial cosmological model: (Ω b h 2, Ω m h 2, h, n s, τ, Σm ) DATA PARAMETER ESTIMATES

9 Cosmological Observables Recombination Hubble constant H0 & cosmic distances measurements: SN Ia and Baryon Acoustic Oscillations (BAO) matter density fluctuations Large-Scale Structures [ galaxy / cosmic shear / Lyα ] LSS spectrum Photon momentum after decoupling CMB secondary anisotropy spectrum from J. Lesgourgues Photon density fluctuations before decoupling CMB primary anisotropy spectrum (temp+pol)

10 Cosmological Data CMB Temperature: Planck plus data from other experiments at large mul/poles (ACT, SPT ) CMB Polariza/on and lensing: Planck, Large Scale Structure: * Galaxy Clustering * Bias (Galaxy, ): Amplitude of the Ma<er P(k) * Lyman- α forest: independent measurement of power on small scales * Baryon acous/c oscilla/ons (BAO) Bounds on parameters from other data: SNIa (Ω m ), HST (h),

11 Cosmological Parameters: example SDSS Coll, PRD 69 (2004)

12 Cosmological bounds on neutrino mass(es) A unique cosmological bound on m DOES NOT exist! Different analyses have found upper bounds on neutrino masses, since they depend on The combina/on of cosmological data used The assumed cosmological model: number of parameters (problem of parameter degeneracies) The proper/es of relic neutrinos

13 The minimal ΛCDM model fits very well Planck data

14 1- parameter extensions of the ΛCDM model 95% CL limits Ext =BAO + JLA + H 0

15 1- parameter extensions of the ΛCDM model 68+95% Conf regions 0.06 ev Planck TT + lowp Planck TT,TE,EE + lowp Planck TT,TE,EE + lowp + BAO

16 Measuring N eff Indirect detec/on of CNB at 10-17σ All 68%CL

17 CMB alone (Planck TT+lowP): Σm < 0.72 ev + TE,EE+ lensing: Σm < 0.59 ev Planck TT+lowP+lensing+ext: Σm < 0.23 ev Measuring m with Planck All 95% CL.

18 Measuring m with Planck Cosmological upper limits on the sum of neutrino masses 3 NH IH 1 Planck TT+lowP! (ev) 0.3 Planck TT+lowP+ TE,EE+ lensing Planck TT+lowP+lensing+ext m 0 (ev)

19 Measuring m & N eff with Planck Results are prac/cally unchanged (example from Planck 2013) CMB alone (Planck+WP+HighL): Σm < 0.60 ev N e = With BAO: Σm < 0.28 ev N e = All 95% CL All 95% CL

20 Probing Direct the laboratory absolute neutrino bounds mass on scale m Searching for non- zero neutrino mass in laboratory experiments Tritium beta decay: measurements of endpoint energy 3 H! 3 He + e + e m β < 2.2 ev (95% CL) Mainz Future experiments (KATRIN) m( e ) ~ ev Neutrinoless double beta decay: if Majorana neutrinos (A, Z)! (A, Z + 2) + 2e experiments with 76 Ge, 130 Te and other isotopes: m ββ < ev, depending on NME

21 Probing the absolute neutrino mass scale Absolute mass scale searches Tri/um β decay m = U ei 2 m 2 i i 1/2 2.2 ev Neutrinoless double beta decay m = i U 2 eim i < ev Cosmology i m i < ev

22 TriBum β decay, 02β and Cosmology KATRIN CURRENT 02β Planck TT+lowP +lensing+ext Planck TT+lowP +lensing+ext Σm Σm

23 Future sensibvibes on neutrino physics from cosmology

24 Future cosmological data Hannestad & Wong, JCAP 07 (2007) cm H Takada et al, PRD 73 line (2006) surveys Wang et al, PRL 95 (2005) Hannestad et al, JCAP 06 (2006) 025 Song & Knox, PRD 70 (2004) Galaxy Cluster Perotto et al, JCAP 10 Surveys (2006) 013 Lesgourgues et al, PRD 73 (2006) CMB PolarizaBon (beyond Planck) Forecasts indicate mev sensibvibes to Σm are possible!! CMB lensing Cosmic Shear Surveys Loeb & Wyithe, PRL 100 (2008) Lyman- α Pritchard & Pierpaoli, PRD 78 (2008)

25 Future sensibvibes to Σm : weak gravitabonal lensing Distant faint galaxies Frieman, Dodelson

26 Future sensibvibes to Σm : weak gravitabonal lensing Foreground mass No bias uncertainty Small scales much closer to linear regime Tomography: 3D reconstruc/on Weak lensing of faint galaxies Frieman, Dodelson Measure a large number of ellip/cally shaped galaxies

27 Future sensibvibes to Σm : weak gravitabonal lensing lensing of the CMB signal sensi/vity of CMB (primary + lensing) to m σ(m ) = 0.15 ev (Planck) σ(m ) = ev (CMBpol) Makes CMB sensi/ve to smaller neutrino masses Kaplinghat, Knox & Song PRL 91 (2003)

Future sensi/vi/es to N eff and Σm Example of forecast: PLANCK + Euclid- like photometric galaxy cluster survey Hannestad & Wong, JCAP 07 (2007) 004 Takada et al, PRD 73 (2006) 083520 Wang et al, PRL

28 Future sensi/vi/es to N eff and Σm Example of forecast: PLANCK + Euclid- like photometric galaxy cluster survey Hannestad & Wong, JCAP 07 (2007) 004 Takada et al, PRD 73 (2006) Wang et al, PRL 95 (2005) Hannestad et al, JCAP 06 (2006) 025 Song & Knox, PRD 70 (2004) Perotto et al, JCAP 10 (2006) 013 Lesgourgues et al, PRD 73 (2006) M.C.A. Cerbolini et al, JCAP 06 (2013) 020 [arxiv: ]

29 Measuring even m =0.05 ev? New cosmological observable as a potential probe of fluctuations at intermediate redshifts (6<z<20) study of fluctuations in the 21cm line emitted by neutral H Karttunen et al. 2007

21cm line emitted by neutral H accélération acceleration décélération fast deceleration rqpide décélération slow deceleration

30 Measuring even m =0.05 ev? New cosmological observable as a potential probe of fluctuations at intermediate redshifts (6<z<20) study of fluctuations in the 21cm line emitted by neutral H accélération acceleration décélération fast deceleration rqpide décélération slow deceleration lente accélération acceleration 20>z>6 inflation RD (radiation domination) MD matière (matter domination) énergie dark energy noire domination Redshifted line: 2.1 m at redshift 10 power spectrum of 21 cm brightness fluctuations P 21 (k)

31 Future sensibvibes on Σm from 21cm observabons Future Low- radio telescopes Pritchard & Pierpaoli, PRD 78 (2008) [also Loeb & Wyithe, PRL 100 (2008) ; Mao et al, PRD 78 (2008) ]

32 Future sensi/vi/es on neutrino masses Abazajian et al, Astrop. Phys. 35 (2011) 177

33 For more details

34 End of 4th lecture

Neutrinos in Cosmology

Neutrinos in Cosmology ν ν ν ν ν ν ν ν ν ν ν ν ν ν ν ν ν ν ν ν ν ν ν ν Olga Mena & Sergio Pastor (IFIC Valencia) Cosmology School in the Canary Islands, Fuerteventura, 18-22 Sep 2017 History of the Universe