Kinetic mixing as the origin of a light dark-gauge-group scale
Abstract
We propose a model in which supersymmetric weak scale dark matter is charged under a U(1)_d dark gauge symmetry. Kinetic mixing between U(1)_d and hypercharge generates the appropriate hierarchy of scales needed to explain PAMELA and ATIC with a GeV scale force carrier and DAMA (or INTEGRAL) using the proposals of inelastic (or, respectively, exciting) dark matter. Because of the extreme simplicity of this setup, observational constraints lead to unambiguous determination of the model parameters. In particular, the DAMA scattering cross section is directly related to the size of the hypercharge D-term vacuum expectation value. The known relic abundance of dark matter can be used to fix the ratio of the dark sector coupling to the dark matter mass. Finally, the recent observation of cosmic ray positron and electron excesses can be used to fix the mass of the dark matter through the observation of a shoulder in the spectrum and the size of the kinetic mixing by fitting to the rate. These parameters can be used to make further predictions, which can be checked at future direct detection, indirect detection, as well as collider experiments.
Additional Information
© 2009 American Physical Society. (Received 2 March 2009; published 12 August 2009) We would like to thank N. Arkani-Hamed, M. Popsleov, and N. Weiner for very useful discussions, especially in regard to the long lifetimes of the excited state discussed in the text. We would especially like to thank T. Slatyer for help in generating the Sommerfeld enhancement plot. L.-T. W. and I. Y. are supported by the National Science Foundation under grant PHY-0756966 and the Department of Energy under grant DE-FG02-90ER40542. J. T. R. is supported by the National Science Foundation.Attached Files
Published - PhysRevD.80.035008.pdf
Accepted Version - 0902.3246.pdf
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Additional details
- Alternative title
- Kinetic Mixing as the Origin of Light Dark Scales
- Eprint ID
- 96540
- Resolver ID
- CaltechAUTHORS:20190619-094159422
- PHY-0756966
- NSF
- DE-FG02-90ER40542
- Department of Energy (DOE)
- Created
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2019-06-19Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field