Constraints on dark matter-neutrino scattering from the Milky-Way satellites
and subhalo modeling for dark acoustic oscillations
Kensuke Akita 1 & Shin’ichiro Ando 2,3
1 Institute for Basic Science, CTPU, 2 GRAPPA Institute, Univer sity of Amsterdam, 3 Kavli IPMU, Univer sity of Tokyo

Dar k Matter (DM)・ We can test light DM scattering with neutrinos, baryons, photons
and dark radiations.
・ Even if DM is heavy (GeV-scale), asymmetric DM is not well constrained.

DM is gravitationally confirmed by cosmological observations.
DM properties :・ 27% of the total energy of the universe
・ Massive
・ Stable
We don’t know at (almost) all
・ Mass・ Interactions beyond gravity

Comparisons with N-body simulations

Why the Milky-Way satellites?

Our result(solid)DM does not annihilate today.
→Indirect searches by γ-rays would be ineffective.
https://map.gsfc.nasa.gov/media/121238/index.html

・ Large DM scattering may be achieved in asymmetric DM scenarios.

Constraints on DM-neutrino scattering

・ We may impose relatively strong constraints on DM scatteringwith the lepton sector.

We use the latest data of Milky-Way satellite galaxies
from Dark Energy Survey (DES) and PanSTARRS1 (PS1).

Muon, tau rapidly decay→DM could not scatter with mu, tau.
U (1)Lµ L⌧ symmetry→DM-electron interactions would be suppressed.

https://www.darkenergysurvey.org/supporting-science/large-scale-structure/

Neutrinos, photons,
baryons (coupled to photons), dark radiation
Gravity
If DM has interactions with relativistic particles,DM
DM fluctuations are suppressed by their pressure.
ScatterDM–⌫ (✓DM

DM velocity divergence✓⌫ )Additional term

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DM ⌫ /DM ⌫ nDM /DM ⌫DM gravitationally collapse
and then merge,
forming halos and subhalos.

Subhalo

DM evolution is non-linear.
Semi-analytical model is needed
for comprehensive parametersearch.

Time

Milky WayWe can test DM scattering from the MW satellites!

cm2 (mDM /GeV)DM–⌫,2 < 1043

cm2 (mDM /GeV)(E⌫ /E⌫0 )2

54
2
0 4
<
10
cm
(m
/GeV)(E/E
DM–⌫,4
DM⌫⌫)

DM–⌫,0 < 4 ⇥ 1034

DM–⌫,4 < 7 ⇥ 1059

<latexit sha1_base64="KMynP7GglSzehENOqgGaDcsiZlY=">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</latexit>

cm2 (mDM /GeV)

46
2
0 2
<
10
cm
(m
/GeV)(E/E
DM–⌫,2DM⌫⌫)

cm2 (mDM /GeV)(E⌫ /E⌫0 )4

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Cosmic neutrino momentum today One of uncertainties→Milky-Way halo mass

・We have developed a semi-analytical subhalo model for DAOs.

W

Subhalo32

We adopt the smooth-k filter:f smooth kSatellite
galaxyDM–⌫,0 < 10<latexit sha1_base64="aykzoSL9vJBuxuHocoyx1KhE9cM=">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</latexit>

Summar y

mDM Light DM→efficientMilky-Way satellite galaxies→Small-scale objects in the universe→DAOs would reduce
the number of the satellite galaxies.

Subhalo mass at accreation

DM collapse to halo:
DM linear fluctuations are spherical:<latexit sha1_base64="ZRarOpgzv52s0Qr+jYIbKP/Ultc=">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</latexit>

DM halo→

Constant DM-neutrino cross section

DM oscillates between gravity and pressure: DAOs.

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8
m
>
10
M
2. 270 satellites with a satellite forming condition aDM decouples with neutrinosin the linear region.

Dark acoustic oscillations

Linear matter
power spectrum<latexit sha1_base64="wFm72idkjv3wyzG9Gyyx9PJ49Bs=">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</latexit><latexit sha1_base64="ElH9wFBv/CuhJx4Krop2K52gnY8=">AAACnXichVFNLyxBFD3a9/BobCQWJibkxWJyW3zFQoRI3gLx8caQQae7FTr6K901kzDxB/wBCzZeQiLvJ7yljT9g4SeIJYnNW7jT04kguJWqOnXqnluncs3AsSNJdFej1NbVNzQ2NadaWn+0tasdnauRXwwtkbN8xw/XTCMSju2JnLSlI9aCUBiu6Yi8uT9Tuc+XRBjZvvdbHgRi0zV2PXvHtgzJlK6qrm5MarQ1np7XN/xtX+pqhrIUR/oj0BKQQRKLvvoPG9iGDwtFuBDwIBk7MBDxKEADIWBuE2XmQkZ2fC9whBRri5wlOMNgdp/XXT4VEtbjc6VmFKstfsXhGbIyjX66pSt6pBv6S/f0/9Na5bhGxcsB72ZVKwK9/bh75flblcu7xN6r6kvPEjsYj73a7D2ImcovrKq+dHjyuDKx3F8eoD/0wP7P6Y6u+Qde6cm6WBLLp1/4MdlLXGV9sJBHihulvW/LR7A6lNVGsyNLw5mp6aRlTehBH35yX8YwhV9YRI7fKeEMF7hUepVZZU5ZqKYqNYmmC29Cyb8A4DmXLg==</latexit>

HaloEx) DM-neutrino scattering

We use two data sets:
1. The kinematics data of 94 satellites with Vcirc > 4 km s 1→

Smooth component

DM play an important role in the structure formation.
→ DM is a seed of matter density contrast for galaxy formation.

Small-Scale[DES collaboration (2020)]

Subhalo modeling for DAOs

Dar k acoustic oscillations (DAOs)
and the Milky-Way (MW) satellites

H✓DM

Our model is very good agreement
within a factor of 1.8!

Why DM-neutrino scattering?

We would like to explore DM property broadly.

✓˙DM = k 2[M. Vogelsberger, et al. (2016)]

Simulations (dashed)<latexit sha1_base64="ASBGiTJxt21Pn6H/Ay4+8oyUgkw=">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</latexit>

In the linear region,

To confirm our model is variable,
we compare publicly available resultsof N-body simulations with DAOs.

1= 3.5 [M. Leo, et al. (2018)](kR) =
1 + (kR)
This filter is different from CDM and WDM cases.

・.Our model is very good agreement with N-body simulations
including DAOs within a factor of 1.8.

<latexit sha1_base64="LC3p+5eZ74nQBXY23CmijxstfxY=">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</latexit>

DM spherically collapse to halos with M ($ R) .
<latexit sha1_base64="cTnQTWTm+MBaNNwZiU2CRymwFmE=">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</latexit>

Distributions of halos and subhalos:
Extended Press-Schechter formalism, e.g., subhalo distribution at z = za<latexit sha1_base64="4qXFfmyz+gVUbdfndQ5+B7W12S4=">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</latexit><latexit sha1_base64="kEBDCqHE8z1W32Q0DqgqkzKzi4s=">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</latexit>

2

d Na
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exp
3/2
dma dza2⇡ (sa SM )

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M
SM )

m : subhalo mass M : host halo mass<latexit sha1_base64="WCc8UPhYVkTNbce9EOaDnCe0Zfk=">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</latexit><latexit sha1_base64="XJXu8t5csUGCf+43yjNJjrcFHEM=">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</latexit>

KASHIWA-DM 2023

・Using the latest data of Milky-Way satellite galaxies from DES
and PS1, we have obtained the most stringent constraints on
DM-neutrino scattering.

Reference
K. Akita and S. Ando, JCAP 11 (2023) 037.

kensuke8a1@ibs.re.kr