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Exploring Very Weakly Interacting Slim Particles: WISP Searches in Theoretical and Astrophysical Contexts

This summary focuses on Very Weakly Interacting Slim Particles (WISPs), which emerge from theoretical, cosmological, and astrophysical motivations. It discusses candidates like Axions, Axion-Like Particles (ALPs), and hidden sector U(1)s (HPs). The role of these particles in Cold Dark Matter (CDM), their phenomena during cosmic events, and their potential to explain astrophysical anomalies like the transparency of the universe to TeV gamma rays are examined. ALPS II is highlighted as a promising experimental endeavor to probe relevant parameter ranges for WISP-based CDM hypotheses.

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Exploring Very Weakly Interacting Slim Particles: WISP Searches in Theoretical and Astrophysical Contexts

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  1. Physics Case for WISP Searches. Towards a comprehensive summary

  2. Summary of Physics Case • VeryWeaklyInteracting Slim Particles (WISPs) arestronglymotivatedfromtheory, cosmology, andastrophysics • Theory: • Axions • Axion-LikeParticles (ALPs) • hiddensector U(1)s (HPs) • Cosmology: • Axion, ALP, or HP Cold Dark Matter (CDM) • Extra, darkradiationduring CMB decoupling • Astrophysics: • Photon ALP oscillationsasexplanationofanomaloustransparencyoftheuniverseforTeVgammarays • Axionor ALP bremsstrahlungasexplanationof non-standard energylossofwhitedwarfs • ALPS II cansearchforthem in stronglymotivatedparameterregion

  3. WISPy Cold Dark Matter • Axions, ALPs and HPs can be born in the early universe non-thermally in the form of spatially homogeneous classical field oscillations (misalignment mechanism) • If sufficiently weakly coupled, this CDM component survives until today • Arias, Cadamuro, Goodsell, Jaeckel, Redondo, AR, in prep.

  4. WISPy Cold Dark Matter • ALPS II 2012 will reachtheparameterrangeofinterestfor HP CDM:

  5. WISPy Cold Dark Matter • ALPS II 2017 will reach the parameter range of interest for ALP CDM:

  6. HP Dark Radiation • Global fit to CMB angular power spectrum slightly prefers extra dark radiation beyond three light neutrinos:

  7. HP Dark Radiation • Global fit to CMB angular power spectrum slightly prefers extra dark radiation beyond three light neutrinos:

  8. HP Dark Radiation • FormeVscalemasses, photon -> HP conversionsoccurresonantly after BBN, but before CMB decoupling -> HP darkradiation • Jaeckel, Redondo, AR • ALPS II 2012 canprobe HP explanationof extra darkradiation:

  9. Light Shining through Cosmic Walls • Spectraofdistant VHE gamma-raysourcesshowno strong indicationsofabsorptionfeatures due to pair productionprocessesfromscattering off photonbath in intergalacticspace (ExtragalacticBackground Light) • Horns, Meyer, subm. to JCAP

  10. Light Shining through Cosmic Walls • Photon -> ALP conversions in cosmic magnetic fields may explain this observation, for ALP masses below neV and g ~ 10e-11/GeV • De Angelis, Roncadelli, Mansutti; …; Simet, Hooper, Serpico; …; Hochmuth, Sigl; …;Mirizzi, Montanino • M • Meyer

  11. Light Shining through Cosmic Walls • Photon -> ALP conversions in cosmic magnetic fields may explain this observation, for ALP masses below neV and g ~ 10e-11/GeV • De Angelis, Roncadelli, Mansutti; …; Simet, Hooper, Serpico; …; Hochmuth, Sigl; …;Mirizzi, Montanino • Meyer

  12. Non-Standard Energy Loss in White Dwarfs • Standard model does not fit to white dwarf luminosity function • Extra energy loss compatible with axion or ALP bremsstrahlung (mass below keV, decay constant ~ 1e9 GeV -> g ~ 1e-11/GeV) • Isern et al.

  13. Physics Reach of ALPS II 2017 • ALPS II 2017 will reach the parameter range of interest for VHE light shining through the EBL and WD energy loss (g ~ 10e-11/GeV ):

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