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  • Open Access

Search for solar bosonic dark matter annual modulation with COSINE-100

G. Adhikari et al. (COSINE-100 Collaboration)
Phys. Rev. D 107, 122004 – Published 26 June 2023
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Abstract
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  • INTRODUCTION
  • EXPERIMENT
  • ANNUAL MODULATION
  • DARK PHOTONS
  • DFSZ AND KSVZ AXIONS
  • KALUZA-KLEIN AXIONS
  • DATA ANALYSIS
  • SENSITIVITY FOR COSINE-200
  • CONCLUSION
  • ACKNOWLEDGMENTS
    • References

    Abstract

    We present results from a search for solar bosonic dark matter using the annual modulation method with the COSINE-100 experiment. The results were interpreted considering three dark sector bosons models: solar dark photons, Dine-Fischler-Srednicki-Zhitnisky (DFSZ) and Kim-Shifman-Vainshtein-Zakharov (KSVZ) solar axions, and Kaluza-Klein solar axions. No modulation signal compatible with the expected from the models was found from a dataset of 2.82 yr, using 61.3 kg of NaI(Tl) crystals. Therefore, we set a 90% confidence level upper limits for each of the three models studied. For the solar dark photon model, the most stringent mixing parameter upper limit is 1.61×10−14 for dark photons with a mass of 215 eV. For the DFSZ and KSVZ solar axion, and the Kaluza-Klein axion models, the upper limits exclude axion-electron couplings, gae, above 1.61×10−11 for axion mass below 0.2 keV; and axion-photon couplings, gaγγ, above 1.83×10−11  GeV−1 for an axion number density of 4.07×1013  cm−3. This is the first experimental search for solar dark photons and DFSZ and KSVZ solar axions using the annual modulation method. The lower background, higher light yield and reduced threshold of NaI(Tl) crystals of the future COSINE-200 experiment are expected to enhance the sensitivity of the analysis shown in this paper. We show the sensitivities for the three models studied, considering the same search method with COSINE-200.

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    • Received 20 February 2023
    • Accepted 9 May 2023

    DOI:https://doi.org/10.1103/PhysRevD.107.122004

    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
    Dark matterParticle astrophysicsParticle dark matter
    1. Physical Systems
    Axion-like particles
    1. Techniques
    Dark matter detectors
    Gravitation, Cosmology & AstrophysicsParticles & Fields

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    Issue

    Vol. 107, Iss. 12 — 15 June 2023

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    Images

    • Figure 1
      Figure 1

      Schematic of COSINE-100 detector, showing the positioning of NaI(Tl) crystals, as well as the passive and active shields [39].

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    • Figure 2
      Figure 2

      Dark photon fluxes on Earth with longitudinal polarization (dashed lines) and transverse polarization (solid lines), for 100 eV (orange), 1 keV (green), 10 eV (purple), and 1 eV (blue) masses.

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    • Figure 3
      Figure 3

      Solar axion flux on Earth considering the axion-Bremsstrahlung process (orange), Compton (green), Primakoff (purple), and electronic recombination and deexcitation by axions (blue). Couplings of gae=5.11×10−11, ma=0.01  eV, and gaγγ=1.02×10−10  GeV−1 were considered, since these are typical values for axions from nonhadronic models. The flux for the Primakoff effect was multiplied by 103 for better visualization and has not been considered in the total flux (black).

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    • Figure 4
      Figure 4

      Expected solar KK axions in the COSINE-100 NaI(Tl) crystals when Earth is at aphelion (blue), and perihelion (red), assuming naphelion=3.81×1013  m−3, nperihelion=4.36×1013  m−3, and gaγγ=9.2×10−14  GeV−1.

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    • Figure 5
      Figure 5

      “BDT” event selection for crystal number 3. (a) Data from the detector calibration with a Co60 source. (b) Physics data taken for around three years. The “BDT” selection removes events to the left of the magenta solid line. In order to define the “BDT” cut, it is required that the purity of scintillation events to the right of the magenta line is at least 99.8%. The 1 keV threshold is represented by the black dashed line.

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    • Figure 6
      Figure 6

      Efficiencies for the “BDT” event selection in crystal 2 for energies from 1 to 6 keV. Above 6 keV, the detection efficiency is considered to be 100%.

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    • Figure 7
      Figure 7

      Event rate for all crystals analyzed (blue data points), considering 15 days time bin and 1–2 keV energy range. The fit (red curves) for this energy range resulted in an amplitude of −0.0250±0.0106 DRU. The vertical black dotted lines refer to the aphelion dates, and the dashed lines refer to the perihelion dates.

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    • Figure 8
      Figure 8

      Amplitudes for the expected modulations simultaneous fits for each energy interval. (a) Considering the R∝d−2 model. (b) Considering the R∝d−4 model. The dashed black line represents the null modulation hypothesis.

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    • Figure 9
      Figure 9

      Amplitudes for the expected annual modulation in the event rate for solar dark photons with mass of 100 eV and ε=6×10−14 (blue) and solar dark photons with mass of 4.4 keV and ε=1.5×10−12 (orange). The amplitudes above 12 keV are very small, and were not shown in the plot.

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    • Figure 10
      Figure 10

      Exclusion plot for solar dark photons, showing the 90% CL upper limits determined in this analysis. The black line is the upper limit derived from the COSINE-100 2.82 dataset analyzed. The red line shows the median of projected sensitivity. The 1σ and 2σ bands are shown by yellow and green shaded regions, respectively. Upper limits determined by Sun observations [52], red giants and horizontal branch stars studies [26], and from the XENON1T experiment [64] are also shown for comparison.

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    • Figure 11
      Figure 11

      Expected amplitudes for DFSZ and KSVZ solar axions in the COSINE-100 crystals for each 1 keV energy interval.

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    • Figure 12
      Figure 12

      Exclusion plot for DFSZ and KSVZ solar axions showing the 90% CL upper limits determined in this analysis. Limits from XMASS [28], XENON100 [27], LUX [29], and values theorized by DFSZ and KSVZ models are also shown for comparison. The projected sensitivity (red line) was gae=2.49×10−11, and the upper limit from the physics data analysis (black line) was gae=1.69×10−11.

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    • Figure 13
      Figure 13

      Expected amplitudes in the NaI(Tl) crystals, considering gaγγ=2×10−11  GeV−1, and n0=1010  m−3 (red), n0=3.35×1012  m−3 (blue), and n0=1015  m−3 (green).

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    • Figure 14
      Figure 14

      Upper limits with 90% CL determined for the solar KK axion model from this analysis. Projected sensitivity with its 1σ and 2σ bands are shown by the red line and yellow and green bands, respectively. Upper limits from XMASS [24] (magenta), NEWS [65] (cyan), and the gaγγ and n0 values that could explain the solar coronal heating problem (orange) are also shown for comparison.

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    • Figure 15
      Figure 15

      Background model for COSINE-200 crystals used for our sensitivity study, based on our expectation for COSINE-200. Contribution from each component is show in colored lines. Contribution from Te series and Sn113 are expected to be very small, and can be neglected.

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    • Figure 16
      Figure 16

      Projected sensitivity for the solar dark photon (left), DFSZ and KSVZ solar axion (center), and KK solar axion (right) models, considering future COSINE-200 experiment NaI(Tl) crystals.

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