Dark photon

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The dark photon (also hidden, heavy, para-, or secluded photon) is a hypothetical hidden sector particle, proposed as a force carrier similar to the photon of electromagnetism but potentially connected to dark matter.[1] In a minimal scenario, this new force can be introduced by extending the gauge group of the Standard Model of Particle Physics with a new abelian U(1) gauge symmetry. The corresponding new spin-1 gauge boson (i.e., the dark photon) can then couple very weakly to electrically charged particles through kinetic mixing with the ordinary photon[2] and could thus be detected. The dark photon can also interact with the Standard Model if some of the fermions are charged under the new abelian group.[3] The possible charging arrangements are restricted by a number of consistency requirements such as anomaly cancellation and constraints coming from Yukawa matrices.

Motivation[edit]

Observations of gravitational effects that cannot be explained by visible matter alone imply the existence of matter which does not or does only very weakly couple to the known forces of nature. This dark matter dominates the matter density of the universe, but its particles (if there are any) have eluded direct and indirect detection so far. Given the rich interaction structure of the well-known Standard Model particles, which make up only the subdominant component of the universe, it is natural to think about a similarly interactive behaviour of dark sector particles. Dark photons could be part of these interactions among dark matter particles and provide a non-gravitational window (a so-called vector portal) into their existence by kinematically mixing with the Standard Model photon.[1][4] Further motivation for the search for dark photons comes from several observed anomalies in astrophysics (e.g., in cosmic rays) that could be related to dark matter interacting with a dark photon.[5][6] Arguably the most interesting application of dark photons arises in the explanation of the discrepancy between the measured and the calculated anomalous magnetic moment of the muon.[7][8][9] This discrepancy is usually thought of as a persisting hint for physics beyond the Standard Model and should be accounted for by general new physics models. Beside the effect on electromagnetism via kinetic mixing and possible interactions with dark matter particles, dark photons (if massive) can also play the role of a dark matter candidate themselves. This is theoretically possible through the misalignment mechanism.[10]

Theory[edit]

Adding a sector containing dark photons to the Lagrangian of the Standard Model can be done in a straightforward and minimal way by introducing a new U(1) gauge field.[2] The specifics of the interaction between this new field, potential new particle content (e.g., a Dirac fermion for dark matter) and the Standard Model particles are virtually only limited by the creativity of the theorist and the constraints that have already been put on certain kinds of couplings. The arguably most popular basic model involves a single new broken U(1) gauge symmetry and kinetic mixing between the corresponding dark photon field and the Standard Model hypercharge fields. The operator at play is , where is the field strength tensor of the dark photon field and denotes the field strength tensor of the Standard Model weak hypercharge fields. This term arises naturally by writing down all terms allowed by the gauge symmetry. After electroweak symmetry breaking and diagonalising the terms containing the field strength tensors (kinetic terms) by redefining the fields, the relevant terms in the Lagrangian are

where is the mass of the dark photon (in this case it can be thought of as being generated by the Higgs or Stueckelberg mechanism), is the parameter describing the kinetic mixing strength and denotes the electromagnetic current with its coupling . The fundamental parameters of this model are thus the mass of the dark photon and the strength of the kinetic mixing. Other models leave the new U(1) gauge symmetry unbroken, resulting in a massless dark photon carrying a long-range interaction.[11][12] A massless dark photon, however, will experimentally be hard to distinguish from the Standard Model photon. The incorporation of new Dirac fermions as dark matter particles in this theory is uncomplicated and can be achieved by simply adding the Dirac terms to the Lagrangian.[13]

Experiments[edit]

Constraints on the dark photon's kinetic mixing parameter


Direct Conversion[edit]

A massive dark photon candidate with kinetic mixing strength could spontaneously convert to a Standard Model photon. A cavity, with resonant frequency tuned to match the mass of a dark photon candidate , can be used to capture the resulting photon.

One technique to detect the presence of signal photon in the cavity is to amplify the cavity field with a quantum limited amplifier. This method is prevalent in the search for axion dark matter. With linear amplification, however, is difficult to overcome the effective noise imposed by the standard quantum limit and search for dark photon candidates that would produce a mean cavity population much less than 1 photon.

By counting the number of photons in the cavity, it is possible to subvert the quantum limit. This technique has been demonstrated by researchers at the University of Chicago in collaboration with Fermilab.[14] The experiment has excluded dark photon candidates with mass centered around 24.86 μeV and by using a superconducting qubit to repeatedly measure the same photon. This has enabled a search speed up of over 1,000 as compared to the conventional linear amplification technique.

See also[edit]

  • Dark radiation – Postulated type of radiation that mediates interactions of dark matter
  • Fifth force – Speculative fifth fundamental force
  • Dual photon – Hypothetical elementary particle that is a dual of the photon under electric–magnetic duality
  • Photino – Hypothetical superpartner of the photon

References[edit]

  1. ^ a b Essig, R.; Jaros, J. A.; Wester, W.; Adrian, P. Hansson; Andreas, S.; Averett, T.; Baker, O.; Batell, B.; Battaglieri, M. (2013-10-31). "Dark Sectors and New, Light, Weakly-Coupled Particles". arXiv:1311.0029 [hep-ph].
  2. ^ a b Holdom, Bob (1986-01-09). "Two U(1)'s and ϵ charge shifts". Physics Letters B. 166 (2): 196–198. Bibcode:1986PhLB..166..196H. doi:10.1016/0370-2693(86)91377-8. ISSN 0370-2693.
  3. ^ Galison, Peter; Manohar, Aneesh (1984-03-08). "Two Z's or not two Z's?". Physics Letters B. 136 (4): 279–283. Bibcode:1984PhLB..136..279G. doi:10.1016/0370-2693(84)91161-4. ISSN 0370-2693.
  4. ^ Battaglieri, Marco; Belloni, Alberto; Chou, Aaron; Cushman, Priscilla; Echenard, Bertrand; Essig, Rouven; Estrada, Juan; Feng, Jonathan L.; Flaugher, Brenna (2017-07-14). "US Cosmic Visions: New Ideas in Dark Matter 2017: Community Report". arXiv:1707.04591 [hep-ph].
  5. ^ Pospelov, Maxim; Ritz, Adam (January 2009). "Astrophysical Signatures of Secluded Dark Matter". Physics Letters B. 671 (3): 391–397. arXiv:0810.1502. Bibcode:2009PhLB..671..391P. doi:10.1016/j.physletb.2008.12.012. S2CID 14611829.
  6. ^ Arkani-Hamed, Nima; Finkbeiner, Douglas P.; Slatyer, Tracy R.; Weiner, Neal (2009-01-27). "A Theory of Dark Matter". Physical Review D. 79 (1): 015014. arXiv:0810.0713. Bibcode:2009PhRvD..79a5014A. doi:10.1103/PhysRevD.79.015014. ISSN 1550-7998. S2CID 17059718.
  7. ^ Pospelov, Maxim (2009-11-02). "Secluded U(1) below the weak scale". Physical Review D. 80 (9): 095002. arXiv:0811.1030. Bibcode:2009PhRvD..80i5002P. doi:10.1103/PhysRevD.80.095002. ISSN 1550-7998. S2CID 202294.
  8. ^ Endo, Motoi; Hamaguchi, Koichi; Mishima, Go (2012-11-27). "Constraints on Hidden Photon Models from Electron g-2 and Hydrogen Spectroscopy". Physical Review D. 86 (9): 095029. arXiv:1209.2558. Bibcode:2012PhRvD..86i5029E. doi:10.1103/PhysRevD.86.095029. ISSN 1550-7998. S2CID 118418557.
  9. ^ Giusti, D.; Lubicz, V.; Martinelli, G.; Sanfilippo, F.; Simula, S. (October 2017). "Strange and charm HVP contributions to the muon ($g - 2)$ including QED corrections with twisted-mass fermions". Journal of High Energy Physics. 2017 (10): 157. arXiv:1707.03019. Bibcode:2017JHEP...10..157G. doi:10.1007/JHEP10(2017)157. ISSN 1029-8479. S2CID 119060801.
  10. ^ Arias, Paola; Cadamuro, Davide; Goodsell, Mark; Jaeckel, Joerg; Redondo, Javier; Ringwald, Andreas (2012-06-08). "WISPy Cold Dark Matter". Journal of Cosmology and Astroparticle Physics. 2012 (6): 013. arXiv:1201.5902. Bibcode:2012JCAP...06..013A. doi:10.1088/1475-7516/2012/06/013. ISSN 1475-7516. S2CID 55566455.
  11. ^ Ackerman, Lotty; Buckley, Matthew R.; Carroll, Sean M.; Kamionkowski, Marc (2009-01-23). "Dark Matter and Dark Radiation". Physical Review D. 79 (2): 023519. arXiv:0810.5126. Bibcode:2009PhRvD..79b3519A. doi:10.1103/PhysRevD.79.023519. ISSN 1550-7998. S2CID 10056950.
  12. ^ Foot, Robert; Vagnozzi, Sunny (2015). "Dissipative hidden sector dark matter". Physical Review D. 91 (2): 023512. arXiv:1409.7174. Bibcode:2015PhRvD..91b3512F. doi:10.1103/PhysRevD.91.023512. S2CID 119288106.
  13. ^ Ilten, Philip; Soreq, Yotam; Williams, Mike; Xue, Wei (2018-01-15). "Serendipity in dark photon searches". Journal of High Energy Physics. 2018 (6): 4. arXiv:1801.04847. Bibcode:2018JHEP...06..004I. doi:10.1007/JHEP06(2018)004. S2CID 59408241.
  14. ^ Dixit, Akash; Chakram, Srivatsan; He, Kevin; Agrawal, Ankur; Naik, Ravi; Schuster, David; Chou, Aaron (2021). "Searching for Dark Matter with a Superconducting Qubit". Physical Review Letters. 126 (14): 141302. arXiv:2008.12231. Bibcode:2021PhRvL.126n1302D. doi:10.1103/PhysRevLett.126.141302. PMID 33891438. S2CID 221341034.