Detecting dark matter made in supernovae G u s t a v o Ma r - - PowerPoint PPT Presentation

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Detecting dark matter made in supernovae G u s t a v o Ma r - - PowerPoint PPT Presentation

Apr 20, 2023 194 likes •444 views

Detecting dark matter made in supernovae G u s t a v o Ma r q u e s - T a v a r e s , U n i v e r s i t y o f Ma r y l a n d In collaboration with W. DeRocco, P.W. Graham, D. Kasen and S. Rajendran

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SLIDE 1

Detecting dark matter made in supernovae

G u s t a v

  • Ma

r q u e s

  • T

a v a r e s , U n i v e r s i t y

  • f

Ma r y l a n d

In collaboration with W. DeRocco, P.W. Graham, D. Kasen and S. Rajendran (arxiv:1905.09284)

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SLIDE 2

Dark matter direct detection

?

arxiv: 1709.00688

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SLIDE 3

Challenges for sub-GeV DM

  • Galactic DM velocity: v ~ 10-3

– Kinetic energy ~ 10-6 mdm < keV

  • Backgrounds increase
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SLIDE 4

Challenges for sub-GeV DM

  • Galactic DM velocity: v ~ 10-3

– Kinetic energy ~ 10-6 mdm < keV

  • Backgrounds increase
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SLIDE 5

Astrophysical sources of DM

  • Look for astrophysical environments where T ~ mdm,

where DM can be produced

  • Supernovae are an ideal candidate, the central

region gets to ~ 50 MeV temperatures for timescales of O(10s)

  • Promising idea, but must check if the flux of dark

matter made in supernovae is sufficiently large.

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SLIDE 6

Focus on simplified model

  • Fermionic DM interacting via
  • UV inspiration
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SLIDE 7

Core-collapse supernovae

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SLIDE 8

Proto-neutron star

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SLIDE 9

Important effects

  • Dark matter is only mildly relativistic:

– delayed arrival – signal spread

  • In most of relevant parameter space dark

matter is diffusively trapped: not all DM that is produced will make it out

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SLIDE 10

Velocity effects

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SLIDE 11

Velocity effects

SN1987a was 55 kpc away (~ 150000 years)

F l u x d i l u t e d b y

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SLIDE 12

Diffuse background

  • CCSN occur at a rate of ~ 2 per century in our

galaxy

  • Each signal lasts for 1000s of years, signals

from many old supernovae overlap

  • Similar to SN neutrino background, except

that origin is galactic

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SLIDE 13

Trapped regime

We computed the flux with a Monte Carlo simulation, but many aspects can be understood analitically using a radial freeze-out approach (assuming static profile)

Rate vs Timescale e.g.

Freeze-out in time Freeze-out in radius

Mean free path vs Size e.g.

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SLIDE 14

Freeze-out radii

Number Sphere RN Energy Sphere RE Scattering Sphere RT

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SLIDE 15

Diffusion

Only one type of interaction Diffusion

The total distance traveled to move λann is enhanced by

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SLIDE 16

Effective mean free path

Freeze-out condition:

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SLIDE 17

Compare with Monte Carlo

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SLIDE 18

Flux on Earth

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SLIDE 19

Energy sphere

  • In the simulation we do not keep track of

momentum information since we are mostly interested in the tail of the distribution.

  • We set the spectrum using the temperature of

the energy sphere instead

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SLIDE 20

Signals

For most of the parameter space: For electron scattering: Large backgrounds from neutrinos

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SLIDE 21

Signals

For electron scattering: Large backgrounds from neutrinos For nuclear scattering: With Liquid Xenon targets: Bonus: For most of the parameter space:

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SLIDE 22

Projected sensitivity

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SLIDE 23

Projected sensitivity

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SLIDE 24

Conclusions

  • Supernovae can be sources of relativistic DM
  • Liquid Xe detectors are sensitive to sub-GeV dark

matter made in SN

  • Can be extended to your favorite sub-GeV DM, as

long as DM couples to electrons and/or nuclei