Light Dark Matter Kenji Kadota IBS Center for Theoretical Physics - - PowerPoint PPT Presentation

Kenji Kadota IBS Center for Theoretical Physics of the Universe (CTPU) Institute for Basic Science, Korea

Light Dark Matter Ø Two concrete examples

Kenji Kadota (IBS) YKIS workshop, Feb 2018

ü Sterile neutrino DM ü Axion(-like) Particle Ø Conclusion Production mechanism Radio (SKA-like) survey

Kenji Kadota (IBS) YKIS workshop, Feb 2018 Interaction strength Sin2(2θ)

Dark matter mass MDM [keV] 10-14 10-13 10-12 10-11 10-10 10-9 10-8 10-7 2 5 50 1 10 DM overproduction

Tremaine-Gunn / Lyman-α

Excluded by X-ray observations

Interaction strength Sin2(2θ)

Dark matter mass MDM [keV] 10-14 10-13 10-12 10-11 10-10 10-9 10-8 10-7 2 5 50 1 10 DM overproduction

Tremaine-Gunn / Lyman-α

Excluded by X-ray observations

Interaction strength Sin2(2θ)

Dark matter mass MDM [keV] 10-14 10-13 10-12 10-11 10-10 10-9 10-8 10-7 2 5 50 1 10 DM overproduction

Tremaine-Gunn / Lyman-α

Excluded by X-ray observations

Interaction strength Sin2(2θ)

Dark matter mass MDM [keV] 10-14 10-13 10-12 10-11 10-10 10-9 10-8 10-7 2 5 50 1 10 DM overproduction

Tremaine-Gunn / Lyman-α

Excluded by X-ray observations

Interaction strength Sin2(2θ)

Dark matter mass MDM [keV] 10-14 10-13 10-12 10-11 10-10 10-9 10-8 10-7 2 5 50 1 10 DM overproduction

Tremaine-Gunn / Lyman-α

Excluded by X-ray observations

Interaction strength Sin2(2θ)

Dark matter mass MDM [keV] 10-14 10-13 10-12 10-11 10-10 10-9 10-8 10-7 2 5 50 1 10 DM overproduction

Tremaine-Gunn / Lyman-α

Excluded by X-ray observations A concrete example for the warm dark matter: Sterile Neutrinos

Dodelson-Widrow mechanism: Thermal active neutrinos conversion to sterile neutrinos

L = −yNLH − 1 2 MNN θ = y H M

Drewes et al (2016)

X P P X

• W ±

γ νe e⌥ N Ue

Cherry,Horiuch(2017)

Kenji Kadota (IBS) YKIS workshop, Feb 2018

Production from (active-sterile) neutrino oscillation ΩN< ΩDM ΩN> ΩDM X-ray

DM constraints heavily depend on the production mechanism! 1) Active-Sterile neutrino oscillation (e.g. Dodelson-Widrow) 2) Active-Sterile neutrino oscillation with the resonance (e.g. Shi-Fuller) 3) Decay of a heavier particle, Thermal freeze-out, variable mixing angle, ... ( e.g. Kusenko, Petraki, Asaka, Shaposhnikov, Merle, Schneider ,Berlin, Hooper,.. ) 4) Sterile-sterile oscillation! (KK and Kaneta (2017)) Also the left-handed neutrino masses via the seesaw mechanism!

L = LSM + LN, LN = νRi/ ∂νR −  νc

R T yνLH − 1

2νc

R T MNνc R + h.c.

• Kenji Kadota (IBS)

YKIS workshop, Feb 2018

ΩN1h2 ∝sin2 2θNM1(yν yν

+)22

Kenji Kadota IBS Center for Theoretical Physics of the Universe (CTPU) Institute for Basic Science, Korea

Light Dark Matter Ø Two concrete examples

Kenji Kadota (IBS) YKIS workshop, Feb 2018

ü Sterile neutrino DM ü Axion(-like) Particle Ø Conclusion Production mechanism Radio (SKA-like) survey

Kenji Kadota (IBS) YKIS workshop, Feb 2018

Non-resonant conversion: Kelley and Quinn (2017), Sigl (2017) Resonant conversion: Huang, KK, Sekiguchi and Tashiro to appear

!"## $

𝑏𝐺𝐺 '=−𝑕*++𝑏𝑭 - 𝑪 𝑔~

1" 23 ~240 1" 789 MHz

Line-like radio signal for non-relativistic axion conversion:

10-16 10-14 10-12 10-10 10-8 10-6 10-10 10-8 10-6 10-4 10-2 100 Axion Coupling |GAγγ | (GeV-1) Axion Mass mA (eV) 10-16 10-14 10-12 10-10 10-8 10-6 10-10 10-8 10-6 10-4 10-2 100

LSW (OSQAR) Helioscopes (CAST) Haloscopes (ADMX and others) Telescopes

Horizontal Branch Stars K S V Z D F S Z

VMB (PVLAS)

SN 1987A HESS Fermi Sun

Figure 61.1: Exclusion plot for axion-like particles as described in the text.

PDG (2017) SKA 50MHz-14 GHz, S~𝜈Jy Previous work: Relativistic axion converted into photon in presence of B. Non-relativistic axion decay into two photons for CDM axion. , Axion mass: 0.2~60 𝜈𝑓𝑊

Kenji Kadota (IBS) YKIS workshop, Feb 2018

South Africa- Karoo Australia- Western Outback Construction 2019-2025, Early Science 2022-, Full Science 2025-2030 Cost: ~650 M Euros, Operation ~ 50 M Euros per year. Square Kilometer Array

CERN-SKA Big data co-operation agreement

Kenji Kadota (IBS) YKIS workshop, Feb 2018

Kelley, Quinn [ApJ Letter (2017)]

10-16 10-14 10-12 10-10 10-8 10-6 10-10 10-8 10-6 10-4 10-2 100 Axion Coupling |GAγγ | (GeV-1) Axion Mass mA (eV) 10-16 10-14 10-12 10-10 10-8 10-6 10-10 10-8 10-6 10-4 10-2 100

LSW (OSQAR) Helioscopes (CAST) Haloscopes (ADMX and others) Telescopes

Horizontal Branch Stars KSVZ DFSZ

VMB (PVLAS)

SN 1987A HESS Fermi Sun

Model: ALP (Axion-like particles) i.e. Ultra-light scalars

• Ultra-light mass :

DE (Barbieri et al (2005),…) Fuzzy DM (Hu (2000),…) String axiverse (Arvanitaki et al (2009),...)

mu ~ 10−22 eV mu ~ 10−22eV −10−10eV

mu ~ H 0 ~ 10−33eV

mu, fu = Ωu / Ωm ~ O(0.01) mu ≤ H (t) : ρu = const mu > H (t) : ρu ∝1 / a3

YKIS workshop, Feb 2018 Kenji Kadota (IBS)

100 1000 10000 0.001 0.01 0.1 1

P(k)[(Mpc/h)3] k [h/Mpc]

Linear: fu=0 fu=0.05 Nonlinear: fu=0 fu=0.05

KK, Mao, Ichiki, Silk (2014)

21 cm signals 1420 MHz

Kenji Kadota (IBS) YKIS workshop, Feb 2018

Brief History of Universe

Years since the Big Bang ~300000 (z~1000) ~100 million (z~20-40) ~1 billion (z~6) ~13 billion (z=0) ß Big Bang: the Universe is filled with ionized gas ß Recombination:The gas cools and becomes neutral ß The first structures begin to form. Reionization starts (z ~12) ß Reionization is complete ß Today’s structures

Dark Ages

Kenji Kadota (IBS) YKIS workshop, Feb 2018

Reionization

Kenji Kadota (IBS) YKIS workshop, Feb 2018

Kleban+(2007) What can we do with 21cm? High precision on small-scale power spectrum

ΔP / P ~ 1/ N

Oyama+(2013)

0.004 0.006 0.008 0.01 0.012 0.014 0.016 0.018 0.02 0.022 0.024 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18

fν fu

mu=1e3 mu=1e5 mu=1e7

KK, Mao, Ichiki, Silk (2014)

Kenji Kadota IBS Center for Theoretical Physics of the Universe (CTPU) Institute for Basic Science, Korea

Light Dark Matter Ø Two concrete examples

Kenji Kadota (IBS) YKIS workshop, Feb 2018

ü Sterile neutrino DM ü Axion(-like) Particle Ø Conclusion Production mechanism Radio (SKA-like) survey Let us be open minded. Complimentarity between particle physics and cosmology.