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  • Open Access

Inverse Primakoff scattering for axionlike particle couplings

C.-P. Wu, C.-P. Liu, Greeshma C., L. Singh, J.-W. Chen, H.-C. Chi, M. K. Pandey, and H. T. Wong
Phys. Rev. D 108, 043029 – Published 25 August 2023
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  • INTRODUCTION
  • FORMALISM
  • SOURCE-SPECIFIC EVENT RATES
  • EXPERIMENTAL CONSTRAINTS
  • SUMMARY AND PROSPECTS
  • ACKNOWLEDGMENTS
    • References

    Abstract

    Axionlike particles (ALPs) can be produced in the Sun and are considered viable candidates for the cosmological dark matter (DM). It can decay into two photons or interact with matter. We identify new inelastic channels of inverse Primakoff processes due to atomic excitation and ionization. Their cross sections are derived by incorporating full electromagnetic fields of atomic charge and current densities, and computed by well-benchmarked atomic many-body methods. Complementing data from the underground XENONnT and surface TEXONO experiments are analyzed. Event rates and sensitivity reaches are evaluated with respect to solar- and DM-ALPs. New parameter space in ALP couplings with the photons versus ALP masses in (1 eV–10 keV) not previously accessible to laboratory experiments are probed and excluded with solar-ALPs. However, at regions where DM-ALPs have already decayed, there would be no ALP-flux and hence, no interactions at the detectors in direct search experiments. No physics constraints can be derived. Future projects would be able to evade the stability bound and open new observable windows in (100 eV–1 MeV) for DM-ALPs.

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    • Received 14 June 2022
    • Revised 29 June 2023
    • Accepted 3 August 2023

    DOI:https://doi.org/10.1103/PhysRevD.108.043029

    Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. Funded by SCOAP3.

    Published by the American Physical Society

    Physics Subject Headings (PhySH)

    1. Research Areas
    AxionsDark matterMany-body techniquesParticle dark matterParticle detection signaturesParticle interactions
    1. Physical Systems
    Axion-like particles
    Gravitation, Cosmology & AstrophysicsParticles & Fields

    Authors & Affiliations

    C.-P. Wu1, C.-P. Liu2,3,*, Greeshma C.4,5, L. Singh4,5, J.-W. Chen6,3,†, H.-C. Chi2, M. K. Pandey2,6, and H. T. Wong4,‡

    • 1Département de Physique, Université de Montréal, Montréal H3C 3J7, Canada
    • 2Department of Physics, National Dong Hwa University, Shoufeng, Hualien 97401, Taiwan
    • 3Physics Division, National Center for Theoretical Sciences, National Taiwan University, Taipei 10617, Taiwan
    • 4Institute of Physics, Academia Sinica, Taipei 11529, Taiwan
    • 5Department of Physics, School of Physical and Chemical Sciences, Central University of South Bihar, Gaya 824236, India
    • 6Department of Physics, CTP and LeCosPA, National Taiwan University, Taipei 10617, Taiwan

    • *cpliu@mail.ndhu.edu.tw
    • †jwc@phys.ntu.edu.tw
    • ‡htwong@phys.sinica.edu.tw

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    Issue

    Vol. 108, Iss. 4 — 15 August 2023

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    Images

    • Figure 1
      Figure 1

      Schematic diagrams of ALP two-photons decay in vacuum (TPD) and the three IP scattering channels in matter, where kinematics allows one of the photons to be virtual.

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    • Figure 2
      Figure 2

      Contours of Q2=0 in the IP processes traced by the ALP scattering angle cosθ and fraction of energy transfer (T/Ea) for selected values of va.

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    • Figure 3
      Figure 3

      Total cross sections for the three IP detection channels for the case of a massless ALP scattering off a xenon atom with gaγγ=10−10  GeV−1.

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    • Figure 4
      Figure 4

      Total cross sections for massive ALPs scattering off a xenon atom in the (a) elastic IPel and (b) ionization IPion channels, at gaγγ=10−10  GeV−1.

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    • Figure 5
      Figure 5

      Comparison between the full calculation and EPA for the IPion process in xenon: (a) the differential cross section with ma=1  keV and (b) total cross section with ma=100  eV, with gaγγ=10−10  GeV−1 in both cases.

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    • Figure 6
      Figure 6

      The differential spectrum for solar-ALPs, following Ref. [37] and taking gaγγ=10−10  GeV−1 and several ma as illustration.

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    • Figure 7
      Figure 7

      Differential event rates per ton-year of exposure for solar-ALPs with the four detection channels in liquid xenon, at gaγγ=10−10  GeV−1 with (a) ma=100  eV and (b) ma=5  keV.

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    • Figure 8
      Figure 8

      Differential event rates per ton-year of exposure for DM-ALPs with the four detection channels in liquid xenon, at gaγγ=10−10  GeV−1 and ma=100  eV as illustration. The x axis is in va≃2(Ea−ma)/ma, which is suitable for NR kinematics. The fractional deviation Δ between the Full and EPA calculations of IPion is shown at the upper panel.

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    • Figure 9
      Figure 9

      Signal detection efficiency for DM-ALPs for the leading TPD and IPion channels as function of Ea in XENONnT [44, 45] and TEXONO [42, 43] (inset) experiments. Efficiencies due to full absorption (FA) are applicable to both experiments, while single-hit (SH) selection applies in addition to XENONnT. Signatures for solar-ALPs are below 20  keVee, and the efficiency is close to unity.

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    • Figure 10
      Figure 10

      (a) Standalone sensitivity regions at 90% CL in (ma,gaγγ) from the TEXONO [42, 43] and XENONnT [44, 45] experiments with solar-ALPs. Contributions from the leading channels of IPel and IPion are displayed. Upper reaches of the sensitivity regions due to survival from the Sun is shown. (b) Exclusion plot in (ma,gaγγ) at 90% CL, showing the solar-ALP limits from TEXONO and XENONnT experiments. The astrophysical and cosmological bounds [11, 46, 47, 48] are the light shaded regions. The predicted band for QCD axions [49] is in yellow. Superimposed are the current constraints from solar-ALPs with Bragg scattering [19, 20] and helioscope [41] experiments, as well as the sensitivity reaches of the DARWIN project [50] at standard SH-selection and zero-background scenarios.

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    • Figure 11
      Figure 11

      (a) Standalone sensitivity regions at 90% CL in (ma,gaγγ) from the TEXONO [42, 43] and XENONnT [44, 45] experiments with DM-ALPs. Contributions from the leading channels of IPion and TPD are displayed. Upper reaches of the sensitivity regions due to survival of terrestrial attenuation effects are shown. The cosmological stability bound [46, 51, 52] is denoted by the bold black line. (b) Exclusion plot in (ma,gaγγ) at 90% CL, which results from the scenario of DM-ALPs. The stability bound (black) dictates that only a small region (red) is excluded by XENONnT [44, 45]. The astrophysical and cosmological constraints [11, 52], which are consequences of DM-ALPs, are included. The predictions from QCD axions [49] are displayed as the yellow band. Superimposed are the sensitivity reaches of the DARWIN project [50] at standard SH-selection and zero-background scenarios, indicating that a new detection window is opened and substantial region can be probed.

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    • Figure 12
      Figure 12

      Summary plot of existing constraints on gaγγ versus ma in ALPs. Those in dotted lines only apply under the assumption that ALPs are the cosmological DM [52]. The yellow band are predictions from QCD axion models [49].

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