Lecture VIII: Cosmic Frontier Connections M.J. Ramsey-Musolf U Mass - - PowerPoint PPT Presentation

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Lecture VIII: Cosmic Frontier Connections M.J. Ramsey-Musolf U Mass Amherst http://www.physics.umass.edu/acfi/ ACFI NLDBD School 10/31-11/3 2017 1 Lecture VIII Goals Provide some background on leptogenesis in the broader context of

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Lecture VIII: Cosmic Frontier Connections

ACFI NLDBD School 10/31-11/3 2017

M.J. Ramsey-Musolf

U Mass Amherst

http://www.physics.umass.edu/acfi/

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Lecture VIII Goals

  • Provide some background on leptogenesis in the

broader context of baryogenesis

  • Discuss some implications of 0νββ-decay searches for

leptogenesis

  • Provide some background on cosmological probes of

neutrino mass**

  • Invite questions !

** Disclaimer: not my primary area of expertise

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Lecture VIII Outline

I. Origin of Matter: Leptogenesis II. Neutrino Mass from Cosmology

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  • I. Origin of Matter: Leptogenesis
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Symmetries & Cosmic History

Standard Model Universe EW Symmetry Breaking: Higgs QCD: n+p! nuclei QCD: q+g! n,p… Astro: stars, galaxies,..

10-35 s 10-11 s 10-5 s ~ 1 m 380k yr

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Symmetries & Cosmic History

Standard Model Universe EW Symmetry Breaking: Higgs BSM Physics? QCD: n+p! nuclei QCD: q+g! n,p… Astro: stars, galaxies,..

10-35 s 10-11 s 10-5 s ~ 1 m 380k yr

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The Origin of Matter

Explaining the origin, identity, and relative fractions of the cosmic energy budget is one of the most compelling motivations for physics beyond the Standard Model

Cosmic Energy Budget Dark Matter Dark Energy

68 % 27 % 5 %

Baryons Baryons

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The Origin of Matter

Explaining the origin, identity, and relative fractions of the cosmic energy budget is one of the most compelling motivations for physics beyond the Standard Model

Cosmic Energy Budget Dark Matter Dark Energy

68 % 27 % 5 %

Baryons Baryons

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Cosmic Baryon Asymmetry

Big Bang Nucleosynthesis: Light element abundances depend on YB Cosmic Microwave Bcknd: Shape of anisotropies depends on YB

YB = nB s = (8.59 ± 0.11) ⇥ 10−11

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Symmetries & Cosmic History

Standard Model Universe EW Symmetry Breaking: Higgs QCD: n+p! nuclei QCD: q+g! n,p… Astro: stars, galaxies,..

10-35 s 10-11 s 10-5 s ~ 1 m 380k yr

How did we go from nothing to something ?

BSM Physics?

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Ingredients for Baryogenesis

  • B violation (sphalerons)
  • C & CP violation
  • Out-of-equilibrium or

CPT violation

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Ingredients for Baryogenesis

  • B violation (sphalerons)
  • C & CP violation
  • Out-of-equilibrium or

CPT violation

Standard Model BSM

✔ ✖ ✖ ✔ ✔ ✔

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Ingredients for Baryogenesis

  • B violation (sphalerons)
  • C & CP violation
  • Out-of-equilibrium or

CPT violation

Standard Model BSM

✔ ✖ ✖ ✔ ✔ ✔ Scenarios: leptogenesis, EW baryogenesis, Afflek- Dine, asymmetric DM, cold baryogenesis, post- sphaleron baryogenesis…

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Symmetries & Cosmic History

Standard Model Universe EW Symmetry Breaking: Higgs QCD: n+p! nuclei QCD: q+g! n,p… Astro: stars, galaxies,..

?

Baryogenesis: When? CPV? SUSY? Neutrinos?

10-35 s 10-11 s 10-5 s ~ 1 m 380k yr

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Symmetries & Cosmic History

Standard Model Universe EW Symmetry Breaking: Higgs QCD: n+p! nuclei QCD: q+g! n,p… Astro: stars, galaxies,..

?

Baryogenesis: When? CPV? SUSY? Neutrinos?

EW Baryogenesis: testable w/ EDMs + colliders

10-35 s 10-11 s 10-5 s ~ 1 m 380k yr

Leptogenesis: look for ingred’s w/ νs: DBD, ν osc

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Baryogenesis Scenarios

Energy Scale (GeV) 1012

Affleck Dine

109 10 2 10-1

Standard thermal lepto Electroweak, resonant lepto, WIMPY baryo, ARS lepto… Post-sphaleron, cold…

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What Questions Does It Address ?

  • Is the neutrino its own antiparticle ?
  • Why is there more matter than antimatter ?
  • Why are neutrino masses so small?

New heavy neutrino-like particle = its own anti-particle “See saw mechanism” “Leptogenesis” Heavy neutrino decays in early universe generate baryon asym

ν = ν

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Neutrinos and the Origin of Matter

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Γ(N ! `H) 6= Γ(N ! ¯ `H∗) (

  • Heavy neutrinos decay out of equilibrium

in early universe

  • Majorana neutrinos can decay to particles

and antiparticles

  • Rates can be slightly different (CP violation)
  • Resulting excess of leptons over anti-leptons

partially converted into excess of quarks over anti-quarks by Standard Model sphalerons

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Neutrinos and the Origin of Matter

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Γ(N ! `H) 6= Γ(N ! ¯ `H∗) (

  • Heavy neutrinos decay out of equilibrium

in early universe

  • Majorana neutrinos can decay to particles

and antiparticles

  • Rates can be slightly different (CP violation)
  • Resulting excess of leptons over anti-leptons

partially converted into excess of quarks over anti-quarks by Standard Model sphalerons

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Neutrinos and the Origin of Matter

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  • Heavy neutrinos decay out of equilibrium

in early universe

ΓN ⌘ Γ(NR ! `H) + Γ(NR ! ¯ `H∗) = |h|2 8⇡ MN NR H l h

Hubble rate

H(T) ⇠ 1.66 g∗ T 2 MP

+

NR H* l h

_

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Neutrinos and the Origin of Matter

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  • Heavy neutrinos decay out of equilibrium

in early universe

Simple estimation

2 4 6 8 10 0.2 0.4 0.6 0.8

ΓN(z) = K1(z) K2(z) ΓN

ΓN (z) / ΓN z = MN / T

ΓN < H(T=MN )

~

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Neutrinos and the Origin of Matter

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  • Heavy neutrinos decay out of equilibrium

in early universe

Simple estimation

✓ ◆ ✓ m1 ⇡ m2

D

MN

m∗ = 8π ∗ (1.66g∗) v2 MP ~ few x 10-3 eV

m1 ≈ m∗

ΓN < H(T=MN )

~

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Neutrinos and the Origin of Matter

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  • Heavy neutrinos decay out of equilibrium

in early universe

Washout processes

NR H * H l l

_ ΔL = 2

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Neutrinos and the Origin of Matter

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  • Heavy neutrinos decay out of equilibrium

in early universe

Complete calculation: Boltzmann equations

di Bari ‘12 Non-Eq: T < mN Eq: T > mN

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Neutrinos and the Origin of Matter

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Γ(N ! `H) 6= Γ(N ! ¯ `H∗) (

  • Heavy neutrinos decay out of equilibrium

in early universe

  • Majorana neutrinos can decay to particles

and antiparticles

  • Rates can be slightly different (CP violation)
  • Resulting excess of leptons over anti-leptons

partially converted into excess of quarks over anti-quarks by Standard Model sphalerons

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Neutrinos and the Origin of Matter

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Γ(N ! `H) 6= Γ(N ! ¯ `H∗) (

  • Heavy neutrinos decay out of equilibrium

in early universe

  • Majorana neutrinos can decay to particles

and antiparticles

  • Rates can be slightly different (CP violation)
  • Resulting excess of leptons over anti-leptons

partially converted into excess of quarks over anti-quarks by Standard Model sphalerons

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Neutrinos and the Origin of Matter

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CPV Asymmetry

Tree-level CPV One-loop “absoprtive part” X

Buchmuller, Peccei, Yanagida ‘05

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Neutrinos and the Origin of Matter

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CPV Asymmetry

Tree-level CPV One-loop “absoprtive part” X

Buchmuller, Peccei, Yanagida ‘05

CPV phases but not same as φPMNS

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Neutrinos and the Origin of Matter

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Putting pieces together: B-L asymmetry

Buchmuller, Peccei, Yanagida ‘05

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Neutrinos and the Origin of Matter

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Γ(N ! `H) 6= Γ(N ! ¯ `H∗) (

  • Heavy neutrinos decay out of equilibrium

in early universe

  • Majorana neutrinos can decay to particles

and antiparticles

  • Rates can be slightly different (CP violation)
  • Resulting excess of leptons over anti-leptons

partially converted into excess of quarks over anti-quarks by Standard Model sphalerons

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Electroweak Sphalerons

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Aλ

Sphaleron Configuration

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Electroweak Sphalerons

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Aλ

Sphaleron Configuration Δ (B+L) / NF Anomaly

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Electroweak Sphalerons

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Aλ

Sphaleron Configuration Δ (B+L) / NF Anomaly

EW sphalerons convert B-L asymmetry to YB

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Davidson-Ibarra Bound

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|✏1| <

∼

3 8⇡ MN1mν3 hH0i2

MN1 > 109 GeV

~ Davidson, Ibarra ‘02

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TeV Scale LNV ?

e− e−

A Z,N

( )

A Z − 2,N + 2

( )

TeV LNV Mechanism

Dirac Majorana

Lmass = y ¯ L ˜ HνR + h.c. Lmass = y Λ ¯ LcHHTL + h.c.

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F B B O(1) for Λ ~ 1 TeV Implications

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TeV LNV & Leptogenesis

Energy Scale (GeV) 1012 10 3 10 2 10-1

Standard thermal lepto Fast ΔL = 2 int: erase L

36 Deppisch et al ‘14, ‘15

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TeV LNV & Leptogenesis

Energy Scale (GeV) 1012 10 3 10 2 10-1

Standard thermal lepto Electroweak, resonant lepto, WIMPY baryo, ARS lepto… Post-sphaleron, cold…

Baryogenesis alternatives

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Fast ΔL = 2 int: erase L

Deppisch et al ‘14, ‘15

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Low Scale “ARS” Leptogenesis

Akhmedov, Rubakov, Smirmov ‘98

  • 1. 3 Singlet RH neutrinos: NA , NB , NC
  • 2. LTOT = LSM + LA + LB + LC
  • 3. Nk oscillations + CPV ! LA = 0, LA = 0, LA = 0 but

LTOT =0

  • 4. Yukawa interactions: Lk , H + lk in equilibrium

above TEW for k=A,B but not for k=C

  • 5. Lepton number for lA,B converted to nB by EW

sphalerons

  • 6. Conditions 4 ! MNk can be ~ O( GeV )

/ / /

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Low Scale “ARS” Leptogenesis

  • M. Drewes
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  • II. Neutrino Mass from Cosmology
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ACFI Workshop

December 2015

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0νβ νββ-Decay: Standard Mechanism

Three active light neutrinos

Effective DBD neutrino mass (eV)

Inverted Normal

Lightest neutrino mass (eV) !

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0νβ νββ-Decay: Standard Mechanism

Three active light neutrinos

Effective DBD neutrino mass (eV)

Inverted Normal

Current generation Current generation Ton Scale Lightest neutrino mass (eV) !

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0νβ νββ-Decay: Standard Mechanism

Three active light neutrinos

Effective DBD neutrino mass (eV)

Inverted Normal

Ton Scale

Full implications require information on lightest mass & hierarchy

Lightest neutrino mass (eV) ! Current generation Current generation

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Interpreting a Positive Result

Three active light neutrinos

Effective DBD neutrino mass (eV)

Inverted Normal

Ton Scale

Positive result would be consistent with 3 light active ν’s & IH or quasi-deg regime, but not definitive as to mechanism

Lightest neutrino mass (eV) ! Current generation Current generation

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Interpreting a Null Result: St’d Mechanism

Three active light neutrinos

Effective DBD neutrino mass (eV)

Inverted Normal

Ton Scale

Full implications require information on lightest mass & hierarchy

Lightest neutrino mass (eV) ! Current generation Current generation

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Kinematic Neutrino Mass Measurements

KATRIN

3H ! 3He e- ν

_

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St’d Mech: What Would a Null Result Imply ?

Three active light neutrinos

Effective DBD neutrino mass (eV)

Inverted Normal

Ton Scale

3H decay cur gen

Null result in NLDBD & non-zero mν from

3H decay ! Neutrinos are (pseudo) Dirac

Lightest neutrino mass (eV) ! Current generation Current generation

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St’d Mech: What Would a Null Result Imply ?

Three active light neutrinos

Lightest neutrino mass (eV) ! Effective DBD neutrino mass (eV)

Inverted

Ton Scale

3H decay cur gen

Normal

3H decay next gen

Current generation Current generation

Null result in NLDBD & non-zero mν from

3H decay ! Neutrinos are (pseudo) Dirac

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St’d Mech: What Would a Null Result Imply ?

Three active light neutrinos

Lightest neutrino mass (eV) ! Effective DBD neutrino mass (eV)

Inverted

Ton Scale

Normal

Current generation Current generation

Null result in NLDBD & non-zero mν from

3H decay ! Neutrinos are (pseudo) Dirac

3H decay cur gen 3H decay next gen

  • P. Vogel
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Neutrino Mass & Cosmology

Matter Power Spectrum

Transition to non-rel ν matter

Massive neutrinos suppress power (relative to large scale power) at scales below free streaming scale

  • K. Abazajian ACFI neutrino mass workshop

Σ mv < 0.12 eV

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Neutrino Mass & Cosmology

Matter Power Spectrum

  • K. Abazajian ACFI neutrino mass workshop
  • J. Brau, U. Oregon

Later Earlier

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Neutrino Mass & Cosmology

Matter Power Spectrum

  • K. Abazajian ACFI neutrino mass workshop

Later Earlier

Neutrino Free Streaming

ΩM = Ων + ΩDM + ΩB

δρν δρDM Free Streaming Scale

Lfs / m−1/2

ν

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Neutrino Mass & Cosmology

Matter Power Spectrum

  • K. Abazajian ACFI neutrino mass workshop

Later Earlier

Neutrino Free Streaming

ΩM = Ων + ΩDM + ΩB

δρν δρDM Free Streaming Scale

Lfs / m−1/2

ν

δρν (power) suppressed for L < Lfs

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Neutrino Mass & Cosmology

Matter Power Spectrum

  • K. Abazajian ACFI neutrino mass workshop

Later Earlier

Neutrino Free Streaming

ΩM = Ων + ΩDM + ΩB

δρν δρDM Free Streaming Scale

Lfs / m−1/2

ν

δρν (power) suppressed for L < Lfs Suppression moves to smaller scales ! Larger k

Increase mν

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Neutrino Mass & Cosmology

Matter Power Spectrum

  • K. Abazajian ACFI neutrino mass workshop

Neutrino Free Streaming

ΩM = Ων + ΩDM + ΩB

δρν δρDM Free Streaming Scale

Lfs / m−1/2

ν

δρν (power) suppressed for L < Lfs Suppression moves to smaller scales ! Larger k

Increase mν Later Earlier Increase mν

Σ mv < 0.12 eV Palanque-Dalabrouille ‘15

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St’d Mech: What Would a Null Result Imply ?

Three active light neutrinos

Lightest neutrino mass (eV) ! Effective DBD neutrino mass (eV)

Inverted

Ton Scale

3H decay cur gen

Null result in NLDBD & non-zero mν from cosmology ! Conclusion depends on mlightest & hierarchy

Normal

3H decay next gen

Cosmo current Current generation Current generation

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St’d Mech: What Would a Null Result Imply ?

Three active light neutrinos

Lightest neutrino mass (eV) ! Effective DBD neutrino mass (eV)

Inverted

Ton Scale

3H decay cur gen

Null result in NLDBD & non-zero mν from cosmology ! Conclusion depends on mlightest & hierarchy

Normal

Current generation Current generation Cosmo current

3H decay next gen

  • P. Vogel
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Lecture VIII Summary

  • Simplest type I see-saw mechanism with Majorana 3 NR + CPV

provides ingredients for baryogenesis via thermal leptogenesis

  • “Standard leptogenesis” ! MN1 > 109 GeV
  • Observation of 0νββ-decay consistent with “standard mechanism”

would demonstrate existence of one key ingredient for thermal leptogenesis

  • Discovery of TeV scale (and below) LNV (0νββ-decay + LHC…)

would preclude high scale leptogenesis & point to alternate, low- scale scenarios (ARS lepto, EW baryo…)

  • Precision cosmology (large scale structure, CMB) places tight

constraints on Σmν for the three light active neutrinos, squeezing the viability of the IH region for mββ

  • Challenge for theory: are there any well-motivated loopholes to

cosmological constraints ?