Not So Weakly Interacting Dark Matter Bonding with Sterile Neutrinos - - PowerPoint PPT Presentation

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Not So Weakly Interacting Dark Matter Bonding with Sterile Neutrinos - - PowerPoint PPT Presentation

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Not So Weakly Interacting Dark Matter Bonding with Sterile Neutrinos Jrn Kersten Based on Torsten Bringmann, Jasper Hasenkamp, JK, JCAP 07 (2014) [arXiv:1312.4947] Outline Introduction 1 Self-Interacting Dark Matter 2 Dark Matter

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SLIDE 1

Not So Weakly Interacting Dark Matter Bonding with Sterile Neutrinos

Jörn Kersten

Based on Torsten Bringmann, Jasper Hasenkamp, JK, JCAP 07 (2014) [arXiv:1312.4947]

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SLIDE 2
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SLIDE 3

Outline

1

Introduction

2

Self-Interacting Dark Matter

3

Dark Matter Interacting with Neutrinos

3 / 21

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SLIDE 4

1

Introduction

2

Self-Interacting Dark Matter

3

Dark Matter Interacting with Neutrinos

4 / 21

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SLIDE 5

The Universe after Planck

Flat ΛCDM cosmology fits data perfectly Planck, arXiv:1303.5062

5 / 21

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SLIDE 6

The Universe after Planck

Flat ΛCDM cosmology fits data perfectly Planck, arXiv:1303.5062 Or does it? Tensions in ΛCDM cosmology

5 / 21

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SLIDE 7

Hints for Dark Radiation

Dark radiation: relativistic particles = γ, νSM Parameterized via radiation energy density ρrad ≡

  • 1 + Neff

7 8 Tν T 4 ργ T ≡ Tγ Neff: effective number of neutrino species Standard Model: Neff = 3.046 Existence of dark radiation ⇔ ∆Neff ≡ Neff − 3.046 > 0

6 / 21

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SLIDE 8

Hints for Dark Radiation

Dark radiation: relativistic particles = γ, νSM Parameterized via radiation energy density ρrad ≡

  • 1 + Neff

7 8 Tν T 4 ργ T ≡ Tγ Neff: effective number of neutrino species Standard Model: Neff = 3.046 Existence of dark radiation ⇔ ∆Neff ≡ Neff − 3.046 > 0 Measurements of Cosmic Microwave Background (CMB): ∆Neff = 1.51 ± 0.75 at 68% CL ACT, ApJ 739 (2011) ∆Neff = 0.81 ± 0.42 at 68% CL SPT, ApJ 743 (2011) ∆Neff = 0.31+0.68

−0.64 at 95% CL Planck, arXiv:1303.5076

6 / 21

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SLIDE 9

Hints for Hot Dark Matter

2 . . . 3 σ tension: CMB (z > 1000) vs. local (z < 10) observations Expansion rate Planck: H0 = (67.3 ± 1.2) km

s Mpc arXiv:1303.5076

Hubble: H0 = (73.8 ± 2.4) km

s Mpc Riess et al., ApJ 730 (2011)

Magnitude of matter density fluctuations (σ8)

7 / 21

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SLIDE 10

Hints for Hot Dark Matter

2 . . . 3 σ tension: CMB (z > 1000) vs. local (z < 10) observations Expansion rate Planck: H0 = (67.3 ± 1.2) km

s Mpc arXiv:1303.5076

Hubble: H0 = (73.8 ± 2.4) km

s Mpc Riess et al., ApJ 730 (2011)

Magnitude of matter density fluctuations (σ8) Resolved by hot dark matter component ≃ dark radiation Best fit: ∆Neff = 0.61 meff

s ≡

  • Ts

Tν

3 ms = 0.41 eV

Hamann, Hasenkamp, JCAP 10 (2013) Wyman, Rudd, Vanderveld, Hu, PRL 112 (2014) Battye, Moss, PRL 112 (2014) Gariazzo, Giunti, Laveder, JHEP 11 (2013)

7 / 21

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SLIDE 11

Small-Scale Problems of Structure Formation

Numerical simulations of structure formation with cold dark matter

Springel, Frenk, White, Nature 440 (2006)

Excellent agreement with observations

8 / 21

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SLIDE 12

Small-Scale Problems of Structure Formation

Numerical simulations of structure formation with cold dark matter

Springel, Frenk, White, Nature 440 (2006)

Excellent agreement with observations on large scales

8 / 21

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Small-Scale Problems of Structure Formation

Missing satellites

Kravtsov, Adv. Astron. (2010) Klypin et al., ApJ 522 (1999)

More galactic satellites predicted than observed Cusp-core

De Blok et al., ApJ 552 (2001)

More cuspy density profiles predicted than observed Too big to fail

Boylan-Kolchin et al., MNRAS 422 (2011)

Most massive satellites predicted denser than observed

8 / 21

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SLIDE 14

Small-Scale Problems of Structure Formation

Missing satellites

Kravtsov, Adv. Astron. (2010) Klypin et al., ApJ 522 (1999)

More galactic satellites predicted than observed Cusp-core

De Blok et al., ApJ 552 (2001)

More cuspy density profiles predicted than observed Too big to fail

Boylan-Kolchin et al., MNRAS 422 (2011)

Most massive satellites predicted denser than observed Astrophysics solutions or new particle physics?

8 / 21

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SLIDE 15

1

Introduction

2

Self-Interacting Dark Matter

3

Dark Matter Interacting with Neutrinos

9 / 21

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Not-so-WIMPy Dark Matter

Dark matter χ Standard Model singlet Charged under U(1)X gauge interaction Mass mχ ∼ TeV Light gauge boson V, mV ∼ MeV Long-range, velocity-dependent interaction . . . χ ¯ χ ¯ χ χ V Less cuspy density profiles Cusp-core and too big to fail solved

Feng, Kaplinghat, Yu, PRL 104 (2010) Loeb, Weiner, PRL 106 (2011) Vogelsberger, Zavala, Loeb, MNRAS 423 (2012)

10 / 21

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SLIDE 17

Velocity-Dependent Self-Interactions

Described by Yukawa potential V(r) = ± αX

r e−mV r

Desired scattering cross section σT: Large in dwarf galaxies Small on larger scales to satisfy experimental limits Very different behavior depending on model parameters

  • dwarf

Milky Way cluster

Born r e s

  • n

a n t classical

10 100 1000 105 104 103 102 0.1 1 10 100 v kms ΣTmX cm2g attractive only

mX200 GeV ΑX102 v10 kms

Classical Resonant Born 0.001 0.01 0.1 1 108 105 0.01 10 104 107 mΦ GeV ΣTmX cm2g

Tulin, Yu, Zurek, PRL 110, PRD 87 (2013)

11 / 21

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SLIDE 18

Velocity-Dependent Self-Interactions

Described by Yukawa potential V(r) = ± αX

r e−mV r

Desired scattering cross section σT: Large in dwarf galaxies Small on larger scales to satisfy experimental limits Very different behavior depending on model parameters

  • dwarf

Milky Way cluster

Born r e s

  • n

a n t classical

10 100 1000 105 104 103 102 0.1 1 10 100 v kms ΣTmX cm2g attractive only

mX200 GeV ΑX102 v10 kms

Classical Resonant Born 0.001 0.01 0.1 1 108 105 0.01 10 104 107 mΦ GeV ΣTmX cm2g

Tulin, Yu, Zurek, PRL 110, PRD 87 (2013)

Here: mχv mV ∼ TeV MeV 10 km/s 3 · 105 km/s ∼ 30 ≫ 1 classical regime analytical approximations exist

11 / 21

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Simulating Self-Interacting Dark Matter

Simulation: formation of dwarf galaxy with dark matter + baryons

dA: SIDM10

1 1 2

log[ρ/(M ⊙kpc−3 )]

200 400 600 1000 3000

r [pc]

106 107 108 109

ρ [M ⊙kpc−3 ] dA

DM:CDM-B DM:SIDM1-B DM:SIDM10-B DM:vdSIDMa-B DM:vdSIDMb-B stars:CDM-B stars:SIDM1-B stars:SIDM10-B stars:vdSIDMa-B stars:vdSIDMb-B

Vogelsberger, Zavala, Simpson, Jenkins, MNRAS 444 (2014)

Core, size depends on strength of self-interactions

12 / 21

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SLIDE 20

1

Introduction

2

Self-Interacting Dark Matter

3

Dark Matter Interacting with Neutrinos

13 / 21

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SLIDE 21

Late Kinetic Decoupling

Standard Model neutrinos coupled to V Dark matter scatters off neutrinos Tχ = Tν until kinetic decoupling at T ∼ 100 eV χ χ V ν ν Formation of smaller structures suppressed Missing satellites solved

Van den Aarssen, Bringmann, Pfrommer, PRL 109 (2012)

  • 20

70 60 50 40 30 10 0.5 1 2 5 10 20

ruled out by astrophysics not enough flattening

  • f cuspy profiles

Υmax km s1 Σmax mΧ cm2 g1

1 10 0.05 0.1 0.5 1 5 1 5 1 5

van den Aarssen, Bringmann & Pfrommer 2012

mΧ TeV mV MeV

1

11

M

  • 1

8

M

  • 1

7

M

  • 1

9

M

  • 1

10

M

  • cutoff too small to

address abundance problem LyΑ excluded

mΧ 500 GeV mΧ 10 TeV

105 104 103 102 101 0.05 0.1 0.5 1 5

van den Aarssen, Bringmann & Pfrommer 2012

gΝ mV MeV

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SLIDE 22

Late Kinetic Decoupling

Standard Model neutrinos coupled to V Dark matter scatters off neutrinos Tχ = Tν until kinetic decoupling at T ∼ 100 eV χ χ V ν ν Formation of smaller structures suppressed Missing satellites solved

Van den Aarssen, Bringmann, Pfrommer, PRL 109 (2012)

Problem: explicit breaking of SU(2)L

  • 20

70 60 50 40 30 10 0.5 1 2 5 10 20

ruled out by astrophysics not enough flattening

  • f cuspy profiles

Υmax km s1 Σmax mΧ cm2 g1

1 10 0.05 0.1 0.5 1 5 1 5 1 5

van den Aarssen, Bringmann & Pfrommer 2012

mΧ TeV mV MeV

1

11

M

  • 1

8

M

  • 1

7

M

  • 1

9

M

  • 1

10

M

  • cutoff too small to

address abundance problem LyΑ excluded

mΧ 500 GeV mΧ 10 TeV

105 104 103 102 101 0.05 0.1 0.5 1 5

van den Aarssen, Bringmann & Pfrommer 2012

gΝ mV MeV

14 / 21

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SLIDE 23

Enter the Sterile Neutrino

Sterile neutrino N Mass mN ∼ eV Standard Model singlet Charged under U(1)X

N χ χ V N

Forms hot dark matter Dark matter scatters off sterile neutrinos

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Enter the Sterile Neutrino

Sterile neutrino N Mass mN ∼ eV Standard Model singlet Charged under U(1)X

N χ χ V N

Forms hot dark matter Dark matter scatters off sterile neutrinos Everything solved All small-scale problems of structure formation Hot dark matter hint (CMB-local tension) Neutrino oscillation anomalies

Bringmann, Hasenkamp, JK, JCAP 07 (2014)

15 / 21

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Dark Matter Production

High temperatures: U(1)X sector thermalized via Higgs portal LHiggs ⊃ κ|H|2|Θ|2 Θ ∼ MeV breaks U(1)X

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Dark Matter Production

High temperatures: U(1)X sector thermalized via Higgs portal LHiggs ⊃ κ|H|2|Θ|2 Θ ∼ MeV breaks U(1)X Tχ ∼ mχ/25: freeze-out (chemical decoupling) of dark matter ΩCDMh2 ∼ 0.11 0.67 gX 4 mχ TeV 2

V V . . . χ ¯ χ V ν ¯ ν ν ¯ ν

. . . . . . 16 / 21

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Cold Dark Matter Parameter Space

  • ruled out by

astrophysics not enough flattening

  • f cuspy profiles

M

c u t

  • 1

9

M

  • Mcut
  • 5
  • 1

010 M

cored profiles m i s s i n g s a t e l l i t e s O K 0.1 1 10 1 10

mΧ TeV mV MeV

Bringmann, Hasenkamp & Kersten 2013

Blue band can be moved vertically by changing sterile neutrino charge and temperature Crosses: simulations show that too big to fail solved

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Sterile Neutrino Abundance

T ↓ Higgs portal no longer effective U(1)X sector decouples at T dpl

x

(depending on κ) SM particles becoming non-relativistic afterwards heat SM bath, not U(1)X bath TN < Tν (depending on number of d.o.f. g∗) ∆Neff(T) = TN Tν 4 = g∗,ν g∗,N 4

3

  • T

g∗,N g∗,ν 4

3

  • T dpl

x 18 / 21

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Sterile Neutrino Abundance

T ↓ Higgs portal no longer effective U(1)X sector decouples at T dpl

x

(depending on κ) SM particles becoming non-relativistic afterwards heat SM bath, not U(1)X bath TN < Tν (depending on number of d.o.f. g∗) ∆Neff(T) = TN Tν 4 = g∗,ν g∗,N 4

3

  • T

g∗,N g∗,ν 4

3

  • T dpl

x

∆Neff|BBN <

  • 58.4

g∗,ν(T dpl

x )

4

3

!

1 BBN bounds satisfied for T dpl

x

1 GeV Correct order of magnitude for hot dark matter hint

18 / 21

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Hot Dark Matter Parameter Space

Ν anomalies HDM signal

T

x dpl mt

not possible with SM d.o.f.

m Χ0.1 TeV m Χ0.5 TeV m Χ1TeV

0.2 0.4 0.6 0.8 1.0 0.0 0.5 1.0 1.5 2.0

100 200 g,ΝTx

dpl

Neff cmb mN1eV

Bringmann, Hasenkamp & Kersten 2013

∆Neff|CMB =

  • 58.4

g∗,ν(T dpl

x )

4

3 19 / 21

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Sterile Neutrino Production by Oscillations

Standard scenario: mixing between active and sterile neutrinos

  • scillations ∆Neff ≃ 1

U(1)X interactions effective matter potential suppresses mixing no production by oscillations for T MeV

Hannestad, Hansen, Tram, PRL 112 (2014); Dasgupta, Kopp, PRL 112 (2014)

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Sterile Neutrino Production by Oscillations

Standard scenario: mixing between active and sterile neutrinos

  • scillations ∆Neff ≃ 1

U(1)X interactions effective matter potential suppresses mixing no production by oscillations for T MeV

Hannestad, Hansen, Tram, PRL 112 (2014); Dasgupta, Kopp, PRL 112 (2014)

T < MeV: mixing unsuppressed Oscillations + U(1)X interactions N re-thermalize TN = Tν

Mirizzi, Mangano, Pisanti, Saviano, arXiv:1410.1385

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Sterile Neutrino Production by Oscillations

Standard scenario: mixing between active and sterile neutrinos

  • scillations ∆Neff ≃ 1

U(1)X interactions effective matter potential suppresses mixing no production by oscillations for T MeV

Hannestad, Hansen, Tram, PRL 112 (2014); Dasgupta, Kopp, PRL 112 (2014)

T < MeV: mixing unsuppressed Oscillations + U(1)X interactions N re-thermalize TN = Tν

Mirizzi, Mangano, Pisanti, Saviano, arXiv:1410.1385

With full re-thermalization: ∆Neff|CMB ≃ const. mN = 2 √ 2 Neff|

3/4 CMB

meff

s ≃ 2

√ 2 3.63/4 0.4 eV < 1 eV Cosmology still fine but neutrino anomalies not explained

20 / 21

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Conclusions

Particle physics solution for tensions in standard ΛCDM cosmology: Sterile neutrinos N with mass eV + self-interacting dark matter N small hot DM component, oscillation anomalies solved (?) New interaction mediated by gauge boson with mass ∼ MeV DM-DM scatterings cusp-core, too big to fail solved DM-N scattering missing satellites solved

21 / 21

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Conclusions

Particle physics solution for tensions in standard ΛCDM cosmology: Sterile neutrinos N with mass eV + self-interacting dark matter N small hot DM component, oscillation anomalies solved (?) New interaction mediated by gauge boson with mass ∼ MeV DM-DM scatterings cusp-core, too big to fail solved DM-N scattering missing satellites solved Outlook Interaction by scalar exchange possible and favorable? Further options for model building Connection to 3.5 keV X-ray line? Re-thermalization Improved treatment of scattering in Yukawa potential

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Timeline

t

T

B B N

C M B

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Dark Radiation and Big Bang Nucleosynthesis

T ∼ 1 MeV: freeze-out of n ↔ p n/p ratio fixed T ∼ 0.1 MeV: p + n → D Afterwards formation of 3He, 4He, 7Li ρrad ↑ faster expansion more n available for D fusion more 4He Neff = 3.8+0.8

−0.7 at 2σ CL Izotov, Thuan, arXiv:1001.4440

∆Neff ≤ 1 at 2σ CL

Mangano, Serpico, arXiv:1103.1261

23 / 21

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SLIDE 38

Dark Radiation Effects on the CMB

ρrad ↑ later matter-radiation equality 1st/3rd peak ratio no change ρm ↑ teq unchanged ρrad ↑ sound horizon rs ∝ 1/H ↓ Peak positions no change of angular size θs = rs

DA DA ∝ 1/H ↓

(by ρΛ ↑) Remaining effect: increased Silk damping reduced power on small scales

Hou et al., arXiv:1104.2333

24 / 21

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2 3 4 5 6 7 Neff W7+SPT+BAO+H0+Union21 W7+CMB+LRG+SN+H02 W7+CMB+BAO+SN+H03 W7+CMB+LRG+H04 W7+CMB+BAO+H05 W7+H0+WL+BAO+H(z)+Union26 W7+SPT+WiggleZ+H(z)+BAO+SNLS7 W9+SPT+WiggleZ+H(z)+BAO+SNLS8 W7+SPT+BAO+H09 W7+SPT+BAO+H0+Union210 W7+ACT+SPT+BAO+H011 W7+ACT+SPT+BAO+H012 W7+BAO+H013 W7+ACT14 W7+ACT+BAO+H015 W7+SPT+WiggleZ+H(z)+BAO+SNLS16 W7+CMB+LRG+H017 W7+CMB+BAO+H018 W7+ACT+SPT+LRG+H019 W7+SPTSZ+BAO+H020 W7+SDSS+H021 W7+SDSS+H0+Union222 W7+SDSS+H0+Union2+4He+D/H23 W7+H0+WL+BAO+H(z)+Union224 W7+SPT+BAO+H025 W7+SNLS+BAO+BOSS26 W7+SPT+BAO+H027 W9+STP+H028 W9+STP+H0+BAO29 W9+ACT+H030 W9+ACT+H0+BAO31 Pl+WP+SPT+ACT+BAO32

4He33

D/H34 D/H+4He35 W7+D/H36 W7+SPT(agnostic)37 W7+SPT38 W7+ACT+SPT+BAO+H039 W7+ACT+SPT+LRG+H040 W7+SPT+BAO+H041 W7+SPT42 W7+ACT+BAO+H043 W7+ACT44 W7+LRG+H045 W7+BAO+H046 W5+LRG+maxBGC+H047 W5+CMB+BAO+fgas+H048 W5+LRG+H049 W5+BAO+SN+H050 W7+H0+SDSS+SN+CHFTLS51 W7+SPT+H(z)+H052 W7+H0+WL+BAO+H(z)+Union253 W7+ACBAR+BAO+H0+ACT54 W7+ACBAR+ACT+SPT+SDSS+H055 W7+ACBAR+ACT+SPT+SDSS+MSH056 W7+SPT+BAO+H057 W7+SPT58 W7+H059 W7+SPT+BAO+H060 W7+SPT61 W7+SPT+BAO+H062 W9+ACT+SPT+BAO+H063 W9+ACT64 W9+SPT65 W9+ACT+SPT66 W9+ACT+SPT+lensing67 Pl+WP68 Pl+WP+SPT+ACT+BAO69

Measurements

CDM+Neff+k+f+ns CDM+Neff+k+f+w CDM+Neff+f+w CDM+Neff+k+f CDM+Neff+k

CDM+Neff+Yp CDM+Neff+f CDM+Neff

Modified from Riemer-Sørensen et al. (2013 review) arXiv:1301.7102

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SLIDE 40

Meet the Dark Side

Dirac fermion χ (dark matter) Gauge boson V Light sterile neutrino N Heavier sterile neutrino N2 with mN2 ∼ 1 MeV to cancel anomalies Scalar Θ breaking U(1)X with portal interaction Scalar ξ to enable active-sterile neutrino mixing (vξ < vΘ)

26 / 21