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CFNS Seminar 2/16/2023

Searching for Wavelike Dark Matter with Dielectric and Superconducting Cavities

Raphael Cervantes

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Outline

Dark Matter
Searching for wavelike DM with microwave haloscopes
Orpheus Experiment.

Benefits of Dielectric Haloscopes
DM Search
Outlook

SERAPH Experiment

Benefits of SRF Cavities
DM Search
Upcoming Projects

SQMS Plugfest

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Who am I?

MSI student at Stony Brook.
Ph.D. Physics from University of Washington
Thesis Subject: ADMX-Orpheus developing high-mass dark matter axion search with dielectric microwave resonators.
Now at Fermilab/SQMS implementing SRF cavity and QIS technologies to push the limits of dark matter searches.

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The Dark Matter Problem

Non-luminous
Feebly interacting.
Stable on cosmological times scales.
Non-baryonic.
Non-relativistic.

But what is dark matter?

Credit: Jamarillo, Macias

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Evidence for Dark Matter

Gravitational Lensing

Bullet Cluster

CMB

Galactic Rotation Curves

Credit: JWST

Credit: NASA

Credit: Wayne Hu

Credit: �Mario de Leo

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What is dark matter?

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What are Axions?

Arise from solution to Strong CP problem: CP violation in strong force expected, but not observed.
Peccei-Quinn Solution:

New field with anomolous U(1) �symmetry → new particle (axion).
Axion oscillates around CP conserving minimum.

Produced copiously and cold in early universe, stable, non-baryonic, feebly interacting → excellent dark matter candidate!
Feebly interacts with photons in presence of magnetic field.

Credit: Daw

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Post-inflationary Axions

Lots of theoretical uncertainty

Parameter space much wider if PQ symmetry happened before inflation

Adapted from C. O’Hare

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What are Dark Photons?

Standard Model symmetries: SU(3)×SU(2)×U(1).
Simplest extension: additional U(1) symmetry
Results in dark photon.�

Dark photons oscillate with SM photons.

Credit: S. Ghosh

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The Explored Dark Photon Parameter Space

No preferred parameter space

Adapted from C. O’Hare

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Outline

Dark Matter
Searching for wavelike DM with microwave haloscopes
Orpheus Experiment.

Benefits of Dielectric Haloscopes
DM Search
Outlook

SERAPH Experiment

Benefits of SRF Cavities
DM Search
Upcoming Projects

SQMS Plugfest

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Searching for Wavelike DM with the Microwave Haloscope

Dark

Photons,

Axions

Dark Photons

Credit: C. Boutan

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The ADMX Haloscope at UW

Complicated because of unknown frequency.

Becomes undergrad lab when axion is discovered.

Works well for ∼ 1GHz when V ∼ 100L.

Credit: ADMX

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Outline

Dark Matter
Searching for wavelike DM with microwave haloscopes
Orpheus Experiment at UW

Benefits of Dielectric Haloscopes
DM Search
Outlook

SERAPH Experiment at Fermilab

Benefits of SRF Cavities
DM Search
Upcoming Projects

SQMS Plugfest

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Haloscope difficult to implement at higher frequencies

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Solution: Dielectric Haloscopes

Higher frequency with more volume and better axion sensitivity.

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ADMX-Orpheus Concept

Goal: Dielectrically-loaded Fabry-Perot Open Resonator in dipole magnet. Tunes with length. Search for axions around 16 GHz.

Challenges: Design optics, mechanics to maintain axion-coupling mode for over 1 GHz tuning range.

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The Growing Field of Dielectric Haloscopes

DBAS

MADMAX

LAMPOST

QUAX

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Orpheus Design

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Simulated TEM_00-18 Mode

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Measuring Orpheus Mode Structure

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Orpheus Mode Map

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Simulated vs Measured Transmission

General shape matches.�

Some discrepancy with plausible explanations.

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Orpheus Mode Map

TEM_00-18 mode clear

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The Orpheus Inaugural Dark Photon Search

No magnet yet. Do dark photon search.

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Orpheus Electronics

VNA measures f₀, Q_L in-situ.

Use cryogenic HEMT amplifier.

Superheterodyne receiver measures power.

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Data taking strategy

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The Orpheus Inaugural Dark Photon Search

Scan between 15.8 GHz and 16.8 GHz.

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The Orpheus Inaugural Dark Photon Search

Top dielectric plate motor stall. Had to adjust by hand.

Performed simulations with experimental run conditions.��Weirdly improved Q and V_eff.

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Measured and Simulated Quality Factor

Simulations account for misalignments and tuning errors.

Practical tuning bandwidth due to fixed dielectric thickness and mirror radius of curvature.

3x more than TM010 haloscope at similar frequency (ORGAN).

Also ~2x the tuning range with no mode crossing issues.

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V_eff from Simulation

Can’t be measured directly. Must be confident in simulation.

3x more than TM010 haloscope at similar frequency (ORGAN).

Plenty of room for optimization.

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Looking for dark matter in power spectra

Measured ~3000 power spectra at different cavity lengths.

Search for power excess over noise floor.

Not a dark photon

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Looking for dark matter in power spectra

Expected signal superimposed on data. �Follows Standard Halo Model lineshape and would be about 7 bins wide.

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The excluded DP parameter space

Follow standard haloscope analysis. Data consistent with Gaussian statistics.

No discovery. 90% CL limit.

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DP Limits in the context of other haloscope experiments.

Adapted from C. O’Hare

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Near Future Axion Search

1.5 T dipole magnet being constructed by hand.

KSVZ sensitivity: Veff = 120 mL, Tn ~ 1 K, B0 = 10 T, QL = 20000.

DFSZ sensitivity: Veff = 600 mL, Tn ~ 1 K, B0 = 10 T, QL = 20000.

Adapted from C. O’Hare

Credit: J. Sinnis

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ADMX Collaboration

This work was supported by the U.S. Department of Energy through Grants Nos. DESC0011665 and by the Heising-Simons Foundation.

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Outline

Dark Matter
Searching for wavelike DM with microwave haloscopes
Orpheus Experiment at UW

Benefits of Dielectric Haloscopes
DM Search
Outlook

SERAPH Experiment at Fermilab

Benefits of SRF Cavities
DM Search
Upcoming Projects

SQMS Plugfest

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SQMS and Fermilab

Credit: A. Grassellino

Partners include:

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SRF Cavity Search for Dark Photons

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4/12/22

SQMS

ADMX

High Q allows for larger signal and lower noise floor.

Possibly factor 10⁵ increase in scan rate.

Credit: N. Du

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More details: arXiv:2208.03183

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The scan rate is proportional to the quality factor. The larger the Q, the longer the coherence time, the larger the signal power that accumulates in your cavity.

But there is a nuance to this. This nuance comes from the dark matter halo velocity distribution. The quality factor of this dark matter signal is 10^6.

But it’s been common wisdom that higher Q’s beyond 10^6 you get diminishing returns because you are only sampling a smaller fraction of the dark matter halo.

This is true. But I’m going to argue that the scan rate is proportional to Q even when we are in the ultra-high Q regime.

So yes, the signal power levels off for ultra-high Q. But your signal is now much narrower, which means there is much less noise power within your signal bandwidth. The noise power reduces by a factor of QL and that increases your SNR.

Furthermore, you don’t have to in steps of the cavity bandwidth. Your tuning steps don’t have to be smaller the the dark matter bandwidth because a single cavity frequency is sensitive to a range of axion or dark photon rest masses.

However, with this tuning scheme, we would only be sensitive to virialized axions and we wouldn’t catch the cold streams. But I think I can live with that.

And if you are still skeptical, I’d encourage you to read the paper I posted on the arxiv and to also talk to me.

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SERAPHv1: Parasitic Search for Dark Photons

No DP signal. Just noise.

1000 seconds integration time

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Excluded Dark Photon Parameter Space

haloscope analysis

arXiv:2208.03183

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Deepest Exclusion to Wavelike DPDM

Low-hanging

fruit

Adapted from C. O’Hare

arXiv:2208.03183

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Developing Widely Tunable SRF Cavity (SERAPH v2)

“plunger” cavity

Adapted from C. O’Hare

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Tunable search with 1.3 GHz Cavity (Seraph v1.1)

Similar 1.3 GHz cavity in liquid helium bath.

Tunes by mechanical compression.

500 kHz tuning range.

Data analysis ongoing.

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Subverting SQL Noise with Qubit-based Photon Counting (Seraph v3)

Superconducting qubit in SRF cavity.

Quantum protocols counts photons non-destructively.

Credit: T. Nam

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If this would work in an 8T field

Adapted from C. O’Hare

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Progress towards high Q cavities for Axion Searches

With room for improvement

https://arxiv.org/abs/2201.10733v2

Also advances by ADMX, CAPP, INFN, LLNL, and U. Chicago

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Practical considerations for SRF haloscopes

Achieving higher Q despite TLS dissipation.
Microphonics can introduce modulation effect that spreads signal over greater bandwidth.
Tuning strategy may not capture non-virialized dark matter.

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Summarize

Wavelike dark matter candidates like axions and dark photons are compelling.
Search for wavelike DM with microwave cavities.
Dielectric cavities, superconducting cavities, photon counters can enhance DM search potential.

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This material is based upon work supported by the U.S. Department of Energy, Office of Science, National Quantum Information Science Research Centers, Superconducting Quantum Materials and Systems Center (SQMS) under contract number DE-AC02-07CH11359

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Charactering Cavity Properties

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Measured temperature for noise calibration

Stopped run when flat mirror warmed up.

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Hysteresis in Orpheus measurements

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Debugging Microphonics

Measured with self-excitation loop.
Creates modulation of dark matter signal. Power gets spread into sidebands.
Mitigated by turning off DR pulse tubes.
Quantifiable systematic

Not expected to be a problem in future runs.

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