Non-Minimal Kaluza Klein Dark Matter
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1 Non-Minimal Kaluza Klein Dark Matter Henrik Melbéus Royal Institute of Technology, Stockholm, Sweden EPS-HEP 2011 Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
2 Introduction Outline 1 Kaluza Klein Dark Matter 2 Phenomenology Collaborators: Johan Bonnevier Mattias Blennow Alexander Merle Tommy Ohlsson Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
3 Kaluza Klein Dark Matter Universal Extra Dimensions One of the most popular extra-dimensional extensions of the SM One or more flat extra dimensions All SM fields promoted to higher-dimensional fields Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
4 Kaluza Klein Dark Matter Universal Extra Dimensions One of the most popular extra-dimensional extensions of the SM One or more flat extra dimensions All SM fields promoted to higher-dimensional fields Remnant of translational invariance Conservation of KK parity ( 1) n Lower bound: R 1 > 300 GeV Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
5 Kaluza Klein Dark Matter Kaluza Klein Dark Matter KK parity the Lightest Kaluza Klein Particle (LKP) is stable Analogous to the LSP in SUSY models with R parity Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
6 Kaluza Klein Dark Matter Kaluza Klein Dark Matter KK parity the Lightest Kaluza Klein Particle (LKP) is stable Analogous to the LSP in SUSY models with R parity m LKP R 1 = O(1 TeV) Possible WIMP DM candidate Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
7 Kaluza Klein Dark Matter The LKP The identity of the LKP depends on the UED mass spectrum Minimal UED: B 1 is the LKP (Cheng, Matchev, Schmaltz [hep-ph/ ]) Compare to assumptions regarding SUSY breaking terms Non-minimal UEDs could give other LKPs (Flacke, Menon, Phalen [ ]) Possible WIMP DM candidates: B 1 Z 1 H 1 ν 1 Excluded by direct detection (Servant, Tait [hep-ph/ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
8 Kaluza Klein Dark Matter The LKP The identity of the LKP depends on the UED mass spectrum Minimal UED: B 1 is the LKP (Cheng, Matchev, Schmaltz [hep-ph/ ]) Compare to assumptions regarding SUSY breaking terms Non-minimal UEDs could give other LKPs (Flacke, Menon, Phalen [ ]) Possible WIMP DM candidates: B 1 Z 1 H 1 ν 1 Excluded by direct detection (Servant, Tait [hep-ph/ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
9 Relic abundance The masses giving the correct relic abundance have been calculated to different levels of precision: Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
10 Relic abundance The masses giving the correct relic abundance have been calculated to different levels of precision: B 1 Coannihilations with all level-1 KK particles: mb GeV (Burnell, Kribs [hep-ph/ ], Kong, Matchev [hep-ph/ ]) Adding resonances from second KK-level shifts the preferred mass to a somewhat higher value (Belanger, Kakizaki, Pukhov [ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
11 Z 1 Coannihilations with all level-1 KK particles: mz GeV Relic abundance The masses giving the correct relic abundance have been calculated to different levels of precision: B 1 Coannihilations with all level-1 KK particles: mb GeV (Burnell, Kribs [hep-ph/ ], Kong, Matchev [hep-ph/ ]) Adding resonances from second KK-level shifts the preferred mass to a somewhat higher value (Belanger, Kakizaki, Pukhov [ ]) (Arrenberg, Baudis, Kong, Matchev, Yoo [ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
12 Z 1 Coannihilations with all level-1 KK particles: mz GeV h 1 Without coannihilations: mh 1 3 TeV (preliminary) Relic abundance The masses giving the correct relic abundance have been calculated to different levels of precision: B 1 Coannihilations with all level-1 KK particles: mb GeV (Burnell, Kribs [hep-ph/ ], Kong, Matchev [hep-ph/ ]) Adding resonances from second KK-level shifts the preferred mass to a somewhat higher value (Belanger, Kakizaki, Pukhov [ ]) (Arrenberg, Baudis, Kong, Matchev, Yoo [ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
13 Direct Detection B 1 : σb 1,p 10 6 pb for m B 1 = 1 TeV (Cheng, Feng, Matchev [hep-ph/ ]) Possibly detectable, depending on the KK mass spectrum Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
14 Direct Detection B 1 : Z 1 : σb 1,p 10 6 pb for m B 1 = 1 TeV (Cheng, Feng, Matchev [hep-ph/ ]) Possibly detectable, depending on the KK mass spectrum σz1,p 10 8 pb for m B 1 = 2 TeV (Arrenberg, Baudis, Kong, Matchev, Yoo [ ]) Much more difficult to detect Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
15 Direct Detection B 1 : Z 1 : H 1 : σb 1,p 10 6 pb for m B 1 = 1 TeV (Cheng, Feng, Matchev [hep-ph/ ]) Possibly detectable, depending on the KK mass spectrum σz1,p 10 8 pb for m B 1 = 2 TeV (Arrenberg, Baudis, Kong, Matchev, Yoo [ ]) Much more difficult to detect Unknown, but presumably small due to the large preferred mass Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
16 Neutrinos From the Sun Detection of neutrinos from the annihilation of WIMPs trapped in the Solar core Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
17 Neutrinos From the Sun Detection of neutrinos from the annihilation of WIMPs trapped in the Solar core B 1 : Large branching ratios into leptons Possibly observable at IceCube (Hooper, Kribs [hep-ph/ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
18 Neutrinos From the Sun Detection of neutrinos from the annihilation of WIMPs trapped in the Solar core B 1 : Large branching ratios into leptons Z 1 : Possibly observable at IceCube (Hooper, Kribs [hep-ph/ ]) Large branching ratio into W + W Not observable, due to suppression of the rate by its high mass (Flacke, Menon, Hooper, Dan, Freese [ ], Blennow, H. M., Ohlsson [ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
19 Neutrinos From the Sun Detection of neutrinos from the annihilation of WIMPs trapped in the Solar core B 1 : Large branching ratios into leptons Z 1 : H 1 : Possibly observable at IceCube (Hooper, Kribs [hep-ph/ ]) Large branching ratio into W + W Not observable, due to suppression of the rate by its high mass (Flacke, Menon, Hooper, Dan, Freese [ ], Blennow, H. M., Ohlsson [ ]) Scalar, too strongly constrained by direct detection to be observable in indirect neutrino signals Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
20 Neutrinos From the Sun B 1 Muon-antimuon flux [km -2 yr -1 ] r q = 0.01 r q = 0.05 r q = 0.1 r q = 0.5 IceCube m LKP [GeV] (M. Blennow, H. M., T. Ohlsson [ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
21 Neutrinos from the Sun Z 1 Muon-antimuon flux [km -2 yr -1 ] r q = 0.01 r q = 0.05 r q = 0.1 r q = 0.5 IceCube m LKP [GeV] (M. Blennow, H. M., T. Ohlsson [ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
22 Monoenergetic Gamma-Rays Monoenergetic peak on top of the continuous spectrum Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
23 Monoenergetic Gamma-Rays Monoenergetic peak on top of the continuous spectrum B 1 : Potentially observable by future high-resolution Air Cherenkov Telescopes (Bergström, Bringmann, Eriksson, Gustafsson [hep-ph/ ]) Additional contribution from Zγ and ZH is small (Bertone, Jackson, Shaughnessy, Tait, Vallinotto [ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
24 Monoenergetic Gamma-Rays Monoenergetic peak on top of the continuous spectrum B 1 : Potentially observable by future high-resolution Air Cherenkov Telescopes (Bergström, Bringmann, Eriksson, Gustafsson [hep-ph/ ]) Z 1 : Additional contribution from Zγ and ZH is small (Bertone, Jackson, Shaughnessy, Tait, Vallinotto [ ]) Similar conclusions as for B 1, even though Z 1 is twice as massive (J. Bonnevier, H. M., A. Merle, T. Ohlsson [ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
25 Monoenergetic Gamma-Rays 10 5 Σ v 10 6 pb B 1 Z m LKP GeV (J. Bonnevier, H. M., A. Merle, T. Ohlsson [ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
26 Monoenergetic Gamma-Rays EΓ cm 2 s FERMI H.E.S.S. I & II Σ 50 Σ 1 B 1 BF 100 CTA Z 1 BF 300 Z 1 BF E Γ GeV Integrated Flux MAGIC I & II (J. Bonnevier, H. M., A. Merle, T. Ohlsson [ ]) Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
27 Summary Possible non-minimal KKDM candidates are the B 1, Z 1 and H 1 B 1 : Possibly detectable in direct detection experiments, as well as indirect neutrino and gamma-ray searches Z 1 : Heavier than B 1, and hence harder to detect, but perhaps possible in gamma-ray searches H 1 : Even heavier, and more difficult to detect Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
28 The End The End! Thank you for listening! Henrik Melbéus (KTH) Non-Minimal Kaluza Klein Dark Matter July 21, / 15
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