Dark Matter Axion Searches Gray Rybka University of Washington - - PowerPoint PPT Presentation

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Dark Matter Axion Searches Gray Rybka University of Washington - - PowerPoint PPT Presentation

Apr 13, 2023 239 likes •540 views

Dark Matter Axion Searches Gray Rybka University of Washington TAUP 2019, Toyama Rybka - TAUP 2019 Why Axions? The Strong CP Problem Lack of neutron electron dipole moment edm<310 -26 e-cm Baker et al. indicates strong force is CP

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Dark Matter Axion Searches

Gray Rybka University of Washington

Rybka - TAUP 2019

TAUP 2019, Toyama

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Lack of neutron electron dipole moment indicates strong force is CP invariant How can the weak force be CP violating but the strong force remains CP invariant? O(10-10) cancellation required The Strong CP Problem The Peccei-Quinn Solution Add a dynamic field, spontaneously broken, which cancels any strong CP violation This results in a new pseudoscalar particle, the Axion

  • Weinberg, Wilczek

edm<3∙10-26 e-cm Baker et al. PRL 97 2006

Why Axions?

  • Peccei, Quinn
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The Axion

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The Axion has the same quantum numbers as, and mixes with, the π0. This gives a fairly clear picture of how the axion couplings scale with axion mass.

gagg

a

In the QCD axion particular the axion-photon coupling has very little model dependence. Benchmark models: “KSVZ”: Ad hoc “hadronic” axion couplings. “DFSZ”: Grand unification. “DFSZ” is so compelling that a search needs sensitivity to DFSZ axions in order to be credible. Unfortunately, DFSZ couplings are almost x10 weaker than KSVZ.

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Axions as Dark Matter

As the Universe cools and the temperature falls below the Peccei-Quinn symmetry breaking scale, the axion field begins

  • scillating about the new minimum.

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The classical simple assumption that Peccei-Quinn symmetry is broken after inflation yield a range of axions 1-100 ueV that could produce 100% dark matter.

Oscillation about the QCD minimum – Daniel Grin

A pre-inflationary Peccei-Quinn symmetry breaking combined with anthropic or preferred energy scales can relax this mass constraint.

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Axion Landscape

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Source: PDG

The classic axion-like particle experiments are: Light Shining Through Walls: Laser photon-axion mixing E.g. old: OSQAR, ALPS future: ALPS-II Helioscopes: Axions from the sun E.g. old: CAST, Sumico future: IAXO Haloscopes: Axion dark matter E.g. old: ADMX, RBF future: ADMX G2

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A Wide World of Axion-Like Particles (ALPs)

  • The classic view of axion production in the early universe suggests QCD

axions must be more than micro-eV to accommodate how much dark matter we see

  • However, recently, there has been a lot of exciting work that permits

axions to be much lighter or more strongly coupled

  • Removing the strong-CP requirement
  • Anthropic arguments
  • Preferred energy scales
  • Ties to inflation
  • Ties to dark energy
  • Other new physics
  • This is a very active field

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A Wide World of ALP Searches

  • Black hole superradiance (using LIGO) ~10-20 eV
  • Time varying nuclear EDM (e.g. CASPER) 10-15-10-8 eV
  • Lumped circuit haloscopes (ABRACADABRA, DM Radio) 10-8 – 10-6 eV
  • Ring Resonators, Axion Radar, Atomic Interferometers etc.

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There has been an explosion of search techniques being explored These are in too early development to have sensitivity to the QCD axion, but the community is hopeful

DOE Dark Matter BRN Report 2019

Potential reach

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The QCD Axion Dark Matter Sweet-Spot

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10-17 10-16 10-15 10-14 10-13 10-12 10-11 10-10 10-9 1 10 100 1 10 Axion Coupling |gaγγ | (GeV-1) Axion Mass µeV Cavity Frequency (GHz) Ringwald (2018) Borsanyi (2016) Bonati (2016) di Cortona (2016) Petreczky (2016) Berkowitz (2015) Klaer (2017) Ballesteros (2016) KSVZ DFSZ

ADMX (2018)

Adapted from G.R, J. Phys. G (2017)

Other axion experiments: RBF, HAYSTAC, ORGAN, etc. Astrophysical bounds

ADMX G2 Range

Analytic and Lattice predictions for the “classical” QCD (PQWW) axion mass making 100% dark matter when created post-inflation

*String/Domain Wall contributions can push these masses up/down, see T. Sekiguchi’s talk

*See also Iwazaki arXiv:1810.07270 For a 7 ueV mass prediction

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Axion Haloscope for my Intro Physics Class

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Axion Haloscope for my Intro Physics Class

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Axion Dark Matter Electromagnetic Cavity Resonance Axion-Photon Coupling

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Axion Haloscope: How to search for Dark Matter Axions

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Dark Matter Axions will convert to photons in a magnetic field. The conversion rate is enhanced if the photon’s frequency corresponds to a cavity’s resonant frequency. Signal Proportional to

Cavity Volume Magnetic Field Cavity Q

Noise Proportional to

Cavity Blackbody Radiation Amplifier Noise

Sikivie PRL 51:1415 (1983)

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Power in an Axion Haloscope

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Form Factor Magnetic Field Resonator Volume Model Coupling Dark Matter Density Frequency Resonator Quality Power in haloscope

Make These Large

Cavity Volume Magnetic Field Cavity Q

Make These Small

Cavity Blackbody Radiation Amplifier Noise The better your signal to noise, the faster you can explore axion mass space

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The Axion Haloscope

Digitize Amplify

Power Frequency

Photon Virtual Photon

B- Field

Unknown axion mass requires a tunable resonator This axion lineshape has been

  • exaggerated. A real

signal would hide beneath the noise in a single digitization. An axion detection requires a very cold experiment and an ultra low noise receiver-chain.

B- Field

Axion to photon production E • B

Power Spectrum

FFT Tuning Rod

  • C. Boutan
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Collaborating Institutions: UW, UFL, LLNL FNAL, UCB, PNNL LANL, NRAO, WU, UWA, Sheffield

The ADMX collaboration gratefully acknowledges support from the US Dept. of Energy, High Energy Physics DE-SC0011665 & DE-SC0010280 & DE-AC52-07NA27344 Also support from LLNL and PNNL LDRD programs and R&D support the Heising-Simons institute

ADMX collaboration meeting, UW, December 2018

ADMX “G2” Dark Matter Search Goal: Find Dark Matter Axions

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Key technologies:

  • millikelvin cryogenics
  • ultralow noise

quantum amplifiers

ADMX Design

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Scanning Technique

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The cavity is scanned in few kHz steps with 100 seconds integration ime over the frequency range. The power spectra are filtered for expected axion lineshapes Multiple spectra are combined to reach our sensitivity. Candidate excesses are rescanned. Transient candidates or candidates that do not follow cavity lineshape (RFI) can be vetoed.

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ADMX Cryogenics

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Temperature for example weeks, 2017 vs 2018

We had a significantly lower temperature, and better noise in 2018. Expect even better in 2019

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Scan Speed and Noise Temperature

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Scan speed is proportional to (noise temperature)-2 The limiting factor in our noise temperature is amplifier noise Transistor Amplifiers: 2K SQUID, JPA Quantum Amplifiers: 50 mK

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Quantum Amplifiers

  • Enabling Technology!
  • Superconducting Interference Device

(SQUID) amplifiers

  • Josephson Parametric Amplifiers (JPA)

Rybka - TAUP 2019 19 Sean O’Kelley, Clarke Group, UC Berkeley Yanjie Qiu, Siddiqi Group, UC Berkeley

ADMX Tunable MSA ADMX JPA

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Synthetic Axion Signal Injection

Axion-shaped RF signal are periodically injected into the cavity, blind to the analysis. Most signals are unblinded at the time of rescan to verify our detection efficiency. Some (like this one) are not unblinded until the decision to ramp the magnet down. Note much more data is required in a rescan than during the initial scan.

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Preliminary Sensitivity from 2018 Run

We estimate sensitivity to DFSZ dark matter axions between 2.8 and 3.3 ueV This is four times as much mass range with much more even DFSZ coverage. 3 Gaps from mode crossings in cavity. Paper in preparation!

Dark: Maxwell-Boltzmann Lineshape, Light: N-Body Lineshape Rybka - TAUP 2019 21

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Moving to Higher Frequencies

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Previous experiments

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Why are higher frequencies more challenging?

  • Smaller resonator volume decreases signal
  • Resonator Q worse at high frequencies
  • Standard quantum limit increases noise

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  • More sophisticated, large volume resonators
  • Sub-quantum limited amplifiers
  • Bigger magnets
  • Field tolerant high-Q resonators

How will future Axion Experiments counter these?

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ADMX G2 – Multicavity Systems

Multicavity system 1-2 GHz Prototype fabricated, tested

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Maintain detection volume at higher frequencies

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Higher Frequency Proof-of-Principles

100 101 102 103 104 105 5 10 15 20 25 30 35 gAγ / gAγ DFSZ Axion Mass mA (µeV) 100 101 102 103 104 105 5 10 15 20 25 30 35

ADMX A B C

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29.65 29.7 29.75 29.8 Axion Mass mA (µeV) 29.65 29.7 29.75 29.8

C

10-13 10-12 10-11 10-10 17.35 17.4 17.45 17.5 17.55 17.6 Axion Coupling gAγ (GeV-1) Axion Mass mA (µeV) 10-13 10-12 10-11 10-10 17.35 17.4 17.45 17.5 17.55 17.6

A

20 21 22 23 24 25 Axion Mass mA (µeV) 20 21 22 23 24 25

B

2017 Operations

  • Small-volume ‘sidecar’ demonstrator
  • Demonstration of higher-frequency technology
  • Piezoelectric Tuning
  • Higher-order modes
  • Traditional Quantum Amplifiers
  • New ALP Exclusion Limits at 17, 22, and 30 ueV
  • Boutan et al. Phys. Rev. Lett. 121, 261302

2018 Determinations

  • Found that the 2017 piezo design worked

better 2019 Explorations

  • Wideband Quantum Amplifiers
  • Feedback systems
  • Sensitivity to new frequency ranges
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Selected Axion Progress seen at TAUP 2019

  • Advances in Lumped-Element searches (Abracadabra, DM Radio)
  • Successful squeezing in the HAYSTAC haloscope
  • Field-Tolerant Superconducting High-Q cavities from CAPP Korea
  • Progress on MADMAX dielectric haloscope towards a 100𝛎eV+ search
  • Novel searches for axion-induced polarization rotation

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  • J. Oullet’s talk
  • A. Leder’s talk
  • Y. Semertzidis’s talk
  • X. Li’s talk
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More Exciting Haloscope R&D: Sub-quantum limited detection

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Quantum sensor research is pushing towards single microwave photon counting using bolometers or quantum non-demolition measurements, allowing for much more sensitive detectors

Source: Akash Dixit,

  • U. Chicago

Axion Cavity Workshop 2019

Counting single photons with a Josephson Qbit

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Conclusions

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The axion is a compelling dark matter candidate ADMX Gen 2 shows haloscopes are finally sensitive to the most compelling DFSZ axion model in the ideal dark matter axion mass range We are scanning up in mass, more quickly each year. New technologies are being developed worldwide, enabling access to higher and lower axion masses. Discovery could come at any time!