\begin{document}$ S_A $\end{document} and \begin{document}$ S_B $\end{document}, to interpret the XENON1T keV excess via boosted \begin{document}$ S_B $\end{document}. A small mass splitting \begin{document}$ m_{S_A}-m_{S_B}>0 $\end{document} is introduced, and the boosted \begin{document}$ S_B $\end{document} can be produced using the dark annihilation process of \begin{document}$ S_A S_A^\dagger \to \phi \to S_B S_B^\dagger $\end{document} via a resonant scalar ϕ. \begin{document}$ S_B- $\end{document}electron scattering is intermediated by a vector boson X. Although the constraints from Big Bang nucleosynthesis, cosmic microwave background (CMB), and low-energy experiments set the \begin{document}$ X- $\end{document}mediated \begin{document}$ S_B- $\end{document}electron scattering cross section to be \begin{document}$ \lesssim 10^{-35} \mathrm{cm}^2 $\end{document}, the MeV scale DM with a resonance enhanced dark annihilation today can still provide sufficient boosted \begin{document}$ S_B $\end{document} and induce the XENON1T keV excess. The relic density of \begin{document}$ S_B $\end{document} is significantly reduced by the s-wave process \begin{document}$ S_B S_B^\dagger \to X X $\end{document}, which is permitted by the constraints from CMB and 21-cm absorption. A very small relic fraction of \begin{document}$ S_B $\end{document} is compatible with the stringent bounds on un-boosted \begin{document}$ S_B $\end{document}-electron scattering in DM direct detection, and the \begin{document}$ S_A $\end{document}-electron scattering is also allowed."> Interpretation of XENON1T excess with MeV boosted dark matter -
  • [1]

    E. Aprileet al. (XENON), Phys. Rev. D102(7), 072004 (2020), arXiv:2006.09721[hep-ex

  • [2]

    K. Kannike, M. Raidal, H. Veermäeet al., Phys. Rev. D102(9), 095002 (2020), arXiv:2006.10735[hep-ph

  • [3]

    B. Fornal, P. Sandick, J. Shuet al., Phys. Rev. Lett.125(16), 161804 (2020), arXiv:2006.11264[hep-ph

  • [4]

    M. Du, J. Liang, Z. Liuet al., Chin. Phys. C45(1), 013114 (2021), arXiv:2006.11949[hep-ph

  • [5]

    L. Delle Rose, G. Hütsi, C. Marzoet al., JCAP02, 031 (2021), arXiv:2006.16078[hep-ph

  • [6]

    H. Alhazmi, D. Kim, K. Konget al., JHEP05, 055 (2021), arXiv:2006.16252[hep-ph

  • [7]

    H. Davoudiasl, P. B. Denton, and J. Gehrlein, Phys. Rev. D102(9), 091701 (2020), arXiv:2007.04989[hep-ph

  • [8]

    P. Van Dong, C. H. Nam, and D. Van Loi, Phys. Rev. D103, 095016 (2021), arXiv:2007.08957[hep-ph

  • [9]

    J. Cao, X. Du, Z. Liet al., arXiv: 2007.09981[hep-ph]

  • [10]

    J. Angleet al. (XENON10), Phys. Rev. Lett.107, 051301 (2011), arXiv:1104.3088[astro-ph.CO

  • [11]

    R. Essig, T. Volansky, and T. T. Yu, Phys. Rev. D96(4), 043017 (2017), arXiv:1703.00910[hep-ph

  • [12]

    P. Agneset al. (DarkSide), Phys. Rev. Lett.121(11), 111303 (2018), arXiv:1802.06998[astro-ph.CO

  • [13]

    E. Aprileet al. (XENON), Phys. Rev. Lett.123(25), 251801 (2019), arXiv:1907.11485[hep-ex

  • [14]

    L. Baraket al. (SENSEI), Phys. Rev. Lett.125(17), 171802 (2020), arXiv:2004.11378[astro-ph.CO

  • [15]

    T. R. Slatyer and C. L. Wu, Phys. Rev. D95(2), 023010 (2017), arXiv:1610.06933[astro-ph.CO

  • [16]

    M. Kawasaki, K. Kohri, T. Moroiet al., JCAP12, 048 (2020), arXiv:2006.14803[hep-ph

  • [17]

    C. M. Ho and R. J. Scherrer, Phys. Rev. D87(2), 023505 (2013), arXiv:1208.4347[astro-ph.CO

  • [18]

    C. Boehm, M. J. Dolan, and C. McCabe, JCAP08, 041 (2013), arXiv:1303.6270[hep-ph

  • [19]

    L. B. Jia and X. Q. Li, Eur. Phys. J. C76(12), 706 (2016), arXiv:1608.05443[hep-ph

  • [20]

    A. Berlin, D. Hooper, G. Krnjaicet al., Phys. Rev. Lett.121(1), 011102 (2018), arXiv:1803.02804[hep-ph

  • [21]

    J. R. Batleyet al. (NA48/2), Phys. Lett. B746, 178-185 (2015), arXiv:1504.00607[hep-ex

  • [22]

    D. Banerjeeet al. (NA64), Phys. Rev. D101(7), 071101 (2020), arXiv:1912.11389[hep-ex

  • [23]

    J. L. Feng, B. Fornal, I. Galonet al., Phys. Rev. Lett.117(7), 071803 (2016), arXiv:1604.07411[hep-ph

  • [24]

    J. L. Feng, T. M. P. Taitet al., Phys. Rev. D102(3), 036016 (2020), arXiv:2006.01151[hep-ph

  • [25]

    A. J. Krasznahorkay, M. Csatlós, L. Csigeet al., Phys. Rev. Lett.116(4), 042501 (2016), arXiv:1504.01527[nucl-ex

  • [26]

    A. J. Krasznahorkay, M. Csatlós, L. Csigeet al.,arXiv: 1910.10459[nucl-ex]

  • [27]

    L. B. Jia, Phys. Rev. D94(9), 095028 (2016), arXiv:1607.00737[hep-ph

  • [28]

    K. Agashe, Y. Cui, L. Necibet al., JCAP10, 062 (2014), arXiv:1405.7370[hep-ph

  • [29]

    P. Gondolo and G. Gelmini, Nucl. Phys. B360, 145-179 (1991)

  • [30]

    E. W. Kolb and M. S. Turner, Front. Phys.69, 1-547 (1990)

  • [31]

    K. Griest and D. Seckel, Phys. Rev. D43, 3191-3203 (1991)

  • [32]

    N. Aghanimet al. (Planck), Astron. Astrophys.641, A6 (2020), arXiv:1807.06209[astro-ph.CO

  • [33]

    G. Steigman, B. Dasgupta, and J. F. Beacom, Phys. Rev. D86, 023506 (2012), arXiv:1204.3622[hep-ph

  • [34]

    L. B. Jia and T. Li, Chin. Phys. C45(6), 063101 (2021), arXiv:2006.13357[hep-ph

  • [35]

    T. R. Slatyer, Phys. Rev. D93(2), 023527 (2016), arXiv:1506.03811[hep-ph

  • [36]

    H. Liu and T. R. Slatyer, Phys. Rev. D98(2), 023501 (2018), arXiv:1803.09739[astro-ph.CO

  • [37]

    J. Billard, L. Strigari, and E. Figueroa-Feliciano, Phys. Rev. D89(2), 023524 (2014), arXiv:1307.5458[hep-ph

  • [38]

    D. M. Mei, G. J. Wang, H. Meiet al., Eur. Phys. J. C78(3), 187 (2018), arXiv:1708.06594[physics.ins-det

  • [39]

    R. Essig, J. Mardon, and T. Volansky, Phys. Rev. D85, 076007 (2012), arXiv:1108.5383[hep-ph

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