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Limits on Axion Couplings from the First 80 Days of Data of the PandaX-II Experiment

Changbo Fu et al. (PandaX-II Collaboration)
Phys. Rev. Lett. 119, 181806 – Published 1 November 2017
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    Abstract

    We report new searches for solar axions and galactic axionlike dark matter particles, using the first low-background data from the PandaX-II experiment at China Jinping Underground Laboratory, corresponding to a total exposure of about 2.7×104  kg day. No solar axion or galactic axionlike dark matter particle candidate has been identified. The upper limit on the axion-electron coupling (gAe) from the solar flux is found to be about 4.35×10−12 in the mass range from 10−5 to 1  keV/c2 with 90% confidence level, similar to the recent LUX result. We also report a new best limit from the Fe57 deexcitation. On the other hand, the upper limit from the galactic axions is on the order of 10−13 in the mass range from 1 to 10  keV/c2 with 90% confidence level, slightly improved compared with the LUX.

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    • Received 25 July 2017

    DOI:https://doi.org/10.1103/PhysRevLett.119.181806

    © 2017 American Physical Society

    Physics Subject Headings (PhySH)

    1. Research Areas
    AxionsParticle dark matter
    1. Techniques
    Dark matter detectors
    Particles & FieldsGeneral PhysicsGravitation, Cosmology & Astrophysics

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    Vol. 119, Iss. 18 — 3 November 2017

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    • Figure 1
      Figure 1

      Upper: Event distribution obtained in log10(S2/S1) vs Eee in the PandaX-II experiment; the ±2σ contours for CH3T calibration data are indicated as the green box, and the dark matter data are drawn as red crosses. Lower: The combined energy spectrum with data (histogram with uncertainties) compared to the best fit (red histogram), with individual background components indicated (see Ref. [29]). We also plot here the estimated 10−5  keV/c2 solar axion and 16  keV/c2 ALP spectra assuming that gAe equals 5×10−12 and 5×10−13, respectively. See the text for details.

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    • Figure 2
      Figure 2

      The expected solar-axion flux at Earth’s orbit deduced from theoretical models [19]. Five mechanisms are considered here: Compton-like scattering (C), axion bremsstrahlung (B), atomic recombination (R), and atomic deexcitation (D). See the text for details. The 14.4 keV line is generated by Fe57* deexcitation. In this plot, the corresponding axion parameters are set to be gAe=10−13 and gANeff=10−8.

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    • Figure 3
      Figure 3

      The 90% upper limits on a solar CBRD axion (solid red line) and 14.4 keV Fe57 solar axion in gAe vs mA. The constraints from other representative experiments are also shown, including those using solar neutrinos [41], data from a Si(Li) target [42], CDEX-1 [22], XMASS [23], EDELWEISS-II [19], KIMS [43], XENON100 [24], LUX [26], Majorana Demonstrator [44] (converted to gAe using the same benchmark DFSZ model values for gANeff as in this Letter), and observations of a red giant [45]. The benchmarks of the QCD axion models, DFSZ [19, 40] and Kim-Shifman-Vainstein-Zakharov (KSVZ) [19, 46], are also displayed.

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    • Figure 4
      Figure 4

      Constraints on gAe as a function of the MWDM ALP mass. PandaX’s 90% limit is shown as the red curve, with ±1σ and ±2σ sensitivity bands in green and yellow, respectively. The constraints from other representative experiments are also shown, including those from the solar neutrinos [41], data from CDEX-1 [22], CoGeNT [21], CDMS [20], EDELWEISS-II [19], XENON100 [25], LUX [26] and Majorana Demonstrator [44].

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