Dark SRF - Theory Roni Harnik (Theory Dept.) to be followed by Anna - - PowerPoint PPT Presentation

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Dark SRF - Theory Roni Harnik (Theory Dept.) to be followed by Anna - - PowerPoint PPT Presentation

Dec 05, 2022 372 likes •549 views

Dark SRF - Theory Roni Harnik (Theory Dept.) to be followed by Anna Grassellino (APSTD) For the DarkSRF group: APS-TD : Alex Romanenko, Sam Posen, Yuriy Pischalnikov, Roman Pilipenko, Alex Melnitchouk, Damon Bice, Timergali Khabiboulline, Sergey

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Roni Harnik (Theory Dept.) to be followed by Anna Grassellino (APSTD)

Dark SRF - Theory

For the DarkSRF group:

APS-TD: PPD: Alex Romanenko, Sam Posen, Yuriy Pischalnikov, Roman Pilipenko, Alex Melnitchouk, Damon Bice, Timergali Khabiboulline, Sergey Belomestnykh, Oleg Pronitchev, Valeri Poloubotko Aaron Chou (Astrophysics), Zhen Liu (Theory), Joshua Isaacson (Theory).

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  • Fermilab has a unique opportunity to launch a program of

exploring dark sectors that couple to EM radiation using SRF technology.

  • Leveraging existing Fermilab infrastructure and expertise.
  • We are asking the PAC to endorse the physics goals and the

effort to use SRF technology for fundamental discovery.

Opportunities to Explore Dark Sectors

Well motivated searches:

  • Light mediators
  • Dark matter

Well motivated theories:

  • Dark Photons
  • Axions and ALPs

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γ0

γ

  • Imagine another photon, with a

different mass.

  • Common in top-down frameworks.
  • Any heavy particle that is charged

both photons will generate mixing.

Dark Photons

γ0

dark photon

Nature has already ordered extra copies of fermions. Why not gauge bosons?

L = −1 4

  • FµνF µν + F 0

µνF 0µν − 2✏FµνF 0µν

+ . . . ⊃ ✏

⇣ ~ E · ~ E0 + ~ B · ~ B0⌘

An oscillating EM field is a source of dark photons, and vice versa.

(reminiscent of neutrino oscillations)

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⊗

B

  • Imagine an approximate symmetry broken at a high scale f.

→ a pseudo-Goldstone Boson ≃ an axion-like particle.

  • Common in top-down constructions, the axion is invoked to

solve the strong CP problem.

  • Loops of heavy charged particles can generate interaction:

Axion-like particles

Axions and photons mix in a magnetic field. An oscillating E⋅B is a source of dark photons.

L = ↵ f aFµν ˜ F µν = gaγγa ~ E · ~ B

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  • Both axion-like particles and dark photons are well motivated as

mediators of long range interactions that can be searched for.

Longer Range Interactions and Wave-like Dark Matter

L ⊃

  • Both axion-like particles and dark photons are dark matter

candidates with nice production mechanisms.

  • In the Wave-like DM category. Oscillating at ω = mDM.

dark photons? axions? dark photons? axions?

⊃

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  • Fermilab’s SRF Cavities are world’s highest quality

photon resonators, with Q as high as 1011:

  • Large coherent fields when excited → source dark fields.
  • Resonant response → amplify coherent feeble signals.

Searches with SRF Cavities

Emitter Receiver

Light Shining through wall:

Receiver

a search for a mediator.

A dark matter search:

the DM filled Universe is the emitter

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Dark Photon Search

Emitter Cavity Receiver Cavity

The first simple setup:

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Dark Photon Search

Emitter Cavity Receiver Cavity

Frequency of 1.3 GHz, excited to ~ 35 MV/m. Thats ~ 1025 Photons! The first simple setup:

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Dark Photon Search

Emitter Cavity Receiver Cavity

Frequency of 1.3 GHz, excited to ~ 35 MV/m. Thats ~ 1025 Photons! a dark photon field is radiated at 1.3 GHz. The first simple setup:

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Dark Photon Search

Emitter Cavity Receiver Cavity

Frequency of 1.3 GHz, excited to ~ 35 MV/m. Thats ~ 1025 Photons! Tuned to 1.3 GHz. Responds to dark field. Contains only thermal noise (T=1.4 K). a dark photon field is radiated at 1.3 GHz.

For correct cavity positioning

[see Graham, Mardon, Rajendran, Zhao 2014]

Prec ∼ G2 ✏4 ⇣mγ0 ! ⌘4 QrecQemPem

The first simple setup:

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Dark Photon Search

ω=1.3 GHz Q=1010 t= 2 weeks Runs: T= 1.4 K T= 10 mK

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Log10(mγ/eV) Log10(ϵ) Dark SRF @ FNAL

CMB CROWS (cavities) Coulomb

D a r k S R F @ F e r m i l a b

Preliminary

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Dark Photon Search

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A further search for dark photon DM can follow using a tunable receiver cavity.

Receiver Cavity

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Axion Searches (future directions)

Emitter Cavity Receiver Cavity Excite two modes, with a non-zero (oscillating) E1⋅B2 an axion field is radiated at (f1 ± f2). Several possibilities to explore:

  • One excited and one quiet

mode.

  • Inserting a region of static B

field.

  • .... R&D is required

search for cosmic DM.

  • r

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On to Anna...

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Deleted Scenes

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Light Shining through Wall versus a DM Search

Emitter Receiver DM detector

No need to scan. Need to scan. Need to tune cavities to one another. No need to tune.

Assumes the A’ or axion are the DM, but is often more sensitive. Independent of whether the A’ or axion are the DM.

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Graham et al, Phys.Rev. D90 (2014) no.7, 075017

  • S. R. Parker et al, Phys. Rev. D 88, 112004 (2013)
  • J. Hartnett et al, Phys. Lett. B 698 (2011) 346
  • J. Jaeckel and A. Ringwald, Phys. Lett. B 659, 509 (2008)

Some References LSTW

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