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NEUTRINOS IN NUCLEOSYNTHESIS AND STRUCTURE FORMATION ne nm nt STEEN HANNESTAD UNIVERSITY OF SOUTHERN DENMARK NOW2004, 17 SEPTEMBER 2004 NEUTRINOS, THE MICROWAVE BACKGROUND, AND LARGE SCALE STRUCTURE WMAP 1-YEAR DATA 2dF Galaxy redshift survey 15 May 2002 SDSS SURVEY 2dF POWER SPECTRUM SDSS POWER SPECTRUM DATA FROM THE LYMAN-ALPHA FOREST PROVIDES AN INDEPENDENT MEASUREMENT OF POWER ON SMALL SCALES, BUT IN THE SEMI-LINEAR REGIME (CROFT ET AL. 2002, MCDONALD ET AL. 2003). THE RELIABILITY OF THE INFERRED MATTER SPECTRUM IS CONTROVERSIAL! CROFT ET AL. DATA SDSS EXPERIMENTAL QUESTIONS FROM NEUTRINO PHYSICS NEUTRINO MASS HIERARCHY AND MIXING MATRIX - solar & atmospheric neutrinos - supernovae ABSOLUTE NEUTRINO MASSES - cosmology: CMB and large scale structure - supernovae STERILE NEUTRINOS (LEPTOGENESIS) - cosmology, supernovae NUMBER OF RELIC NEUTRINOS / RELATIVISTIC ENERGY - cosmology STATUS OF 1-2 MIXING (SOLAR + KAMLAND) Araki et al. hep-ex/0406035 STATUS OF 2-3 MIXING (ATMOSPHERIC + K2K) Maltoni et al. hep-ph/0405172 If neutrino masses are hierarchical then oscillation experiments do not give information on the absolute value of neutrino masses ATMO. n K2K SOLAR n KAMLAND Normal hierarchy Inverted hierarchy TALKS BY FERUGLIO, GIUNTI However, if neutrino masses are degenerate m0 matmospheric no information can be gained from such experiments. Experiments which rely on the kinematics of neutrino mass are the most efficient for measuring m0 (or 0n2b decays) Tritium decay endpoint measurements have reached limits on the electron neutrino mass mn e U 2 ei 2 i m 1/ 2 2.3 eV (95%) Mainz experiment, final analysis (Kraus et al. 2003) This translates into a limit on the sum of the three mass eigenstates m 7 eV i TALKS BY GIUNTI, DREXLIN IF NEUTRINOS ARE MAJORANA PARTICLES, THEN 0n2b CAN OCCUR (TALKS BY FAESSLER, KLAPDOR-KLEINGROTHAUS) THE ABSOLUTE VALUES OF NEUTRINO MASSES FROM COSMOLOGY NEUTRINOS AFFECT STRUCTURE FORMATION BECAUSE THEY ARE A SOURCE OF DARK MATTER n h 2 mn 92.5 eV HOWEVER, eV NEUTRINOS ARE DIFFERENT FROM CDM BECAUSE THEY FREE STREAM 1 eV d FS ~ 1 Gpc m SCALES SMALLER THAN dFS DAMPED AWAY, LEADS TO SUPPRESSION OF POWER ON SMALL SCALES BY MEASURING THE MATTER POWER SPECTRUM P(k ) P0 (k )T (k ) 0 eV 0.3 eV T(k) = Transfer function IT IS POSSIBLE TO OBTAIN CONSTRAINTS ON mn ROUGHLY ONE FINDS THAT n P 8 P m EISENSTEIN, HU & TEGMARK ’99 1 eV mn 0 eV mn 1 eV mn 7 eV mn 4 eV Ma ’96 COMBINED ANALYSIS OF CMB, 2dF AND LY-ALPHA DATA BY THE WMAP TEAM (Spergel et al. 2003) HOWEVER, THIS MASS LIMIT IS EXTREMELY DEPENDENT ON DATA OTHER THAN CMB, AND ON PRIORS. Elgaroy & Lahav (astro-ph/0303089, JCAP) A SELECTION OF RECENT RESULTS ON Smn WMAP ONLY 13 eV @ 95% WMAP SPERGEL ET AL. (WMAP) 2003 0.69 eV @ 95% WMAP, CMB, 2dF, s8, H0 STH 2003 1.01 eV @ 95% WMAP, CMB, 2dF, H0 ALLEN, SMITH, BRIDLE 2003 0.56 00..326eV @ 68% WMAP, CMB, 2dF, s8, H0 TEGMARK ET AL 2003 1.8 eV @ 95% WMAP, SDSS BARGER ET AL 2003 0.65 eV @ 95% WMAP, CMB, 2dF, SDSS , H0 CROTTY ET AL. 2004 1.0 eV @ 95% WMAP, CMB, 2dF, SDSS , H0 ANALYSIS WITH RECENT DATA: WMAP CMB DATA SDSS LARGE SCALE STRUCTURE DATA RIESS ET AL. SNI-a ”gold” SAMPLE Lya DATA FROM KECK SAMPLE, NO PRIOR ON s8 (SMALL SCALE AMPLITUDE) mn 0.65 eV @ 95% C.L. S STH, HEP-PH/0409108 BOUND FROM SDSS + WMAP + BIAS + SDSS LYMAN ALPHA (SELJAK ET AL. ASTRO-PH/0407372) mn 0.42 eV @ 95% C.L. FOGLI ET AL. HEP-PH/0408045 FIND ~ 0.5 eV IN A SIMILAR STUDY BOTH RESULTS RELY ON THE ABILITY TO MEASURE THE EXACT MATTER FLUCTUATION AMPLITUDE ON SMALL SCALES Fogli et al., hep-ph/0408045 Normal hierarchy Inverted hierarchy mb U mbb 2 ei 2 i m 1/ 2 2 U ei mi Including the most recent Klapdor et al. constraint Klapdor-Kleingrothaus et al. Nucl. Inst. & Meth. A 522, 371 (2004) Phys. Lett. B 586, 198 (2004) leads to FINAL HEALTH WARNING!! A GENERIC PROBLEM WITH USING COSMOLOGICAL OBSERVATIONS TO PROBE PARTICLE PHYSICS: IN GENERAL, LIKELIHOOD ANALYSES ARE CARRIED OUT ON TOP OF THE MINIMAL COSMOLOGICAL STANDARD MODEL HOWEVER, THERE COULD BE MORE THAN ONE NON-STANDARD EFFECT, SEVERELY BIASING THE PARAMETER ESTIMATE A MODEL WITH BROKEN SCALE-INVARIANCE CAN ALLOW FOR A HIGH NEUTRINO MASS WHAT ABOUT TOPOLOGICAL DEFECTS? COULD WE EVEN BE LIVING IN A NEUTRINOLESS UNIVERSE? (BEACOM, BELL, DODELSON ASTRO-PH/0404585) ANY DERIVED LIMIT SHOULD BE TREATED WITH SOME CARE EXPERIMENTAL QUESTIONS FROM NEUTRINO PHYSICS NEUTRINO MASS HIERARCHY AND MIXING MATRIX - solar & atmospheric neutrinos - supernovae ABSOLUTE NEUTRINO MASSES - cosmology: CMB and large scale structure - supernovae STERILE NEUTRINOS (LEPTOGENESIS) - cosmology, supernovae NUMBER OF RELIC NEUTRINOS / RELATIVISTIC ENERGY - cosmology ANALYSIS OF PRESENT DATA GIVES A LIMIT ON Nn OF 2 Nn 7 (95% C.L.) NOTE THAT THIS MEANS A POSITIVE DETECTION OF THE COSMIC NEUTRINO BACKGROUND AT 3.5s! Crotty, Lesgourgues & Pastor ’03 Pierpaoli ’03, Barger et al. ’03 STH 2003 (JCAP 5, 004 (2003)) Because of the stringent bound from LEP on neutrinos lighter than about 45 GeV Nn 2.992 0.008 this bound is mainly of academic interest if all such light neutrinos couple to Z. However, sterile neutrinos can also contribute to Nn STERILE NEUTRINOS: WHAT ABOUT LSND? WMAP TAKEN AT FACE VALUE THE WMAP RESULT ON NEUTRINO MASS SEEMS TO RULE OUT LSND BECAUSE NO ALLOWED REGIONS EXIST FOR LOW m2. (Pierce & Murayama, hep-ph/0302131; Giunti hep-ph/0302173) HOWEVER, A DETAILED ANALYSIS SHOWS THAT INCREASING Nn, THE NEUTRINO MASS, AND THE MATTER DENSITY SIMULTANEOUSLY PRODUCES EXCELLENT FITS 0 = 1.0 M= 0.35 0.3 b= 0.05 H0 = 70 ns = 1.0 mn = 3eV 0 Nn = 8 3 STH, JCAP 0305, 004 (2003), STH & G RAFFELT JCAP 0404, 008 (2004) THE UPPER MASS LIMIT ON EACH INDIVIDUAL MASS EIGENSTATE IS ROUGHLY CONSTANT FOR ALL Nn IF ALL SPECIES CARRY EQUAL MASS STH & G RAFFELT (JCAP 0404, 008 (2004)) SEE ALSO CROTTY, LESGOURGUES & PASTOR HEP-PH/0402049 A GLOBAL ANALYSIS STILL LEAVES THE TWO LOWEST LYING ISLANDS IN PARAMETER SPACE FOR LSND! Maltoni, Schweitz, Tortola & Valle ’03 (hep-ph/0305312) ONLY IF LYMAN-ALPHA AND BIAS CONSTRAINTS ARE INCLUDED IS THE LSND SOLUTION EXCLUDED AT 95% C.L. (SELJAK ET AL. 2004) BIG BANG NUCLEOSYNTHESIS THE WMAP+LSS LIMIT ON THE BARYON DENSITY b h2 0.0226 0.0008 CAN BE COMBARED TO THE CONFIDENCE REGION FROM OBSERVATIONS OF PRIMORDIAL DEUTERIUM b h2 0.022 0.006 THERE IS COMPLETE CONSISTENCY WITH THE DEUTERIUM VALUE! HOWEVER.... CYBURT, FIELDS & OLIVE, astro-ph/0302431 THERE IS AN INCONSISTENCY AT ROUGHLY 2s WITH HELIUM AND LITHIUM OBSERVATIONS CYBURT, FIELDS & OLIVE, astro-ph/0302431 BOUND ON THE RELATIVISTIC ENERGY DENSITY (NUMBER OF NEUTRINO SPECIES) FROM BBN Helium-4 production is very sensitive to Nn Nn = 4 Nn = 3 Nn = 2 MOST RECENT RESULTS ON Nn FROM BBN 1.7 Nn 3.0 @ 95% C.L. BARGER ET AL. HEP-PH/0305075 Nn 2.510..19 CUOCO ET AL. ASTRO-PH/0307213 DIFFERENCES DUE TO ESTIMATED HELIUM UNCERTAINTY WHAT ABOUT NEUTRINO CHEMICAL POTENTIALS? 12-MIXING LEADS TO ALMOST COMPLETE FLAVOUR EQUILIBRATION BEFORE BBN AND SETS VERY STRINGENT BOUNDS ON THE MAGNITUDE OF THE CHEMICAL POTENTIAL e , m ,t 0.15 Dolgov et al. ’02 Lunardini & Smirnov, hep-ph/0012056 (PRD), Dolgov et al., hep-ph/0201287 Abazajian, Beacom & Bell, astro-ph/0203442, Wong hep-ph/0203180 COMBINING BBN, CMB AND LSS A GLOBAL FIT INCLUDING ALL DATA (BBN, WMAP, 2dF) YIELDS Nn 2.600..43 (95% C.L.) INDICATING THAT a) There seems to be a slight inconsistency between BBN and CMB, meaning that either YP is higher than usually believed, or Nn is lower than 3. b) There seem to be tight bounds on the presence of sterile neutrinos STH, JCAP 5, 004 (2003) ALMOST IDENTICAL RESULT FOUND BY BARGER ET AL. hep-ph/0305075 NEUTRINO THERMALIZATION ALSO PROVIDES A VERY ROBUST LOWER BOUND ON THE REHEATING TEMPERATURE AT THE END OF INFLATION TRH 4 MeV @ 95 C.L. STH, PRD 70, 043506 (2004) SEE ALSO: KAWASAKI ET AL. PRL 82, 4168 (1999) KAWASAKI ET AL. PRD 62, 023506 (2000) GIUDICE ET AL. PRD 64, 023508 (2001) GIUDICE ET AL. PRD 64, 043512 (2001) WHAT ABOUT OTHER LIGHT, THERMALLY PRODUCED PARTICLES? ........... RADIONS AXINOS MAJORONS GRAVITONS AXIONS NEUTRINOS FOR ANY THERMALLY PRODUCED PARTICLE IT IS STRAIGHTFORWARD TO CALCULATE THE DECOUPLING EPOCH ETC. THE ONLY IMPORTANT PARAMETERS ARE mX AND g*,X WHERE g* IS THE EFECTIVE NUMBER OF DEGREES OF FREEDOM WHEN X DECOUPLES. Density bound for a Majorana fermion Based on WMAP, SDSS, SNI-a and Lyman-a data, No assumptions about bias! EW transition (~ 100 GeV) g* = 106.75 MASS BOUND FOR SPECIES DECOUPLING AROUND EW TRANSITION m 5 eV Below QCD transition (~ 100 MeV) g* < 20 DECOUPLING AFTER QCD PHASE TRANSITION LEADS TO m 1 eV STH, hep-ph/0409108 (See also STH & G Raffelt, JCAP 0404, 008) WHAT IS IN STORE FOR THE FUTURE? BETTER CMBR TEMPERATURE MEASUREMENTS Satellites Balloons Interferometers WMAP (ongoing) Boomerang (ongoing) CBI (ongoing) Planck (2007) TopHat (ongoing)DASI (ongoing) CMBR POLARIZATION MEASUREMENTS Satellites Balloons WMAP (ongoing) Boomerang (2002-3) Planck (2007) LARGE SCALE STRUCTURE SURVEYS 2dF (completed) 250.000 galaxies SDSS (ongoing) 1.000.000 galaxies COSMOLOGICAL SUPERNOVA SURVEYS SNAP satellite (2012???) WEAK LENSING SURVEYS Ground Polatron (ongoing) DASI MEASURING mn USING CMB+LSS DATA SDSS-BRG SDSS-BRG PROSPECTS FOR FUTURE DETERMINATION OF Nn Lopez et al. 1998 Data from Planck may allow for very accurate determination of Nn Standard model prediction Nn =3.03-3.04 due to heating and finite temperature effect could perhaps be detected CONCLUSIONS ON NEUTRINOS THE PRESENT UPPER BOUND ON THE NEUTRINO MASS IS SOMEWHERE IN THE REGION OF 0.5-1 eV USING PLANCK, SDSS AND WEAK LENSING SURVEYS IT WILL BE POSSIBLE TO PROBE MASSES AS SMALL AS 0.1-0.2 eV (FOR THE SUM OF ALL MASS EIGENSTATES). IT WILL BE POSSIBLE TO DETERMINE WHETHER NEUTRINO MASSES ARE HIERARCHICAL SIGNIFICANTLY BETTER THAN DIRECT MEASUREMENTS LIKE KATRIN, BUT ALSO LESS ROBUST THE EFFECTIVE NUMBER OF NEUTRINO SPECIES CAN BE PROBED WITH A PRECISION APPROACHING Nn ~ 0.05, CLOSE TO THE STANDARD MODEL PREDICTION OF 0.04