Aside: anti-deuterium The signals from heavy, non-leptons-only DM are interesting! __ TOA d � flux: from ΧΧ � bb : best and worst cases 10 � 3 current BESS limit dashed: best case: NFW, prop.: max 10 � 4 dotted: worst case: isothermal, prop.: min projected AMS � 02 GAPS projected 5 TeV � in � m 2 sr s GeV � n � � 1 10 � 5 10 TeV 10 � 6 20 TeV 5 TeV 10 � 7 10 TeV 20 TeV 10 � 8 � Σ ann. v �� 5 TeV � � 3 � 10 � 22 cm 3 s � 1 10 � 9 � Σ ann. v �� 10 TeV � � 7 � 10 � 22 cm 3 s � 1 � Σ ann. v �� 20 TeV � � 2 � 10 � 21 cm 3 s � 1 10 � 10 10 � 1 10 0 10 1 T in GeV � n
Data sets Electrons + positrons from ATIC, PPB-BETS and HESS: HESS 2008 e + + e − - an excess 10 � 1 ATIC � 2 � Nature 2008 � (2008) PPB � BETS at 700 GeV? ∼ EC AMS HEAT � CAPRICE94 � � � � � � � � E 3 � e � � e � � GeV 2 � cm 2 sec � � � Tang et al. 1984 � � � � � � � � � � � � � � � � � � � ���� � � � � � � � � � � � � � � � � � � � � 10 � 2 � � � � � � � � � � background ? � � � � � � HESS: � very interesting (independent!) but difficult analysis (particle ID: contamination 10 � 3 from gamma & hadronic showers): 10 2 10 3 10 4 10 are these upper limits? energy in GeV [future data from GLAST]
Results Which DM spectra can fit the data? A DM with: -mass M DM = 1 TeV -annihilation DM DM → µ + µ −
Results Which DM spectra can fit the data? A DM with: -mass M DM = 1 TeV -annihilation DM DM → µ + µ − Electrons + Positrons: Positrons: Anti-protons: Yes! Yes! ! s e Y
Results Which DM spectra can fit the data? A DM with: -mass M DM = 1 TeV -annihilation DM DM → µ + µ − Electrons + Positrons: Positrons: Anti-protons: Yes! Yes! ! s e Y Have we identified the DM for the first time?
Results Which DM can fit the data? M.Pospelov and A.Ritz, 0810.1502: Secluded DM - A.Nelson and C.Spitzer, 0810.5167: Slightly Non-Minimal DM - Y.Nomura and J.Thaler, 0810.5397: DM through the Axion Portal - R.Harnik and G.Kribs, 0810.5557: Dirac DM - D.Feldman, Z.Liu, P.Nath, 0810.5762: Hidden Sector - T.Hambye, 0811.0172: Hidden Vector - Yin, Yuan, Liu, Zhang, Bi, Zhu, 0811.0176: Leptonically decaying DM - K.Ishiwata, S.Matsumoto, T.Moroi, 0811.0250: Superparticle DM - Y.Bai and Z.Han, 0811.0387: sUED DM - P.Fox, E.Poppitz, 0811.0399: Leptophilic DM - C.Chen, F.Takahashi, T.T.Yanagida, 0811.0477: Hidden-Gauge-Boson DM - K.Hamaguchi, E.Nakamura, S.Shirai, T.T.Yanagida, 0811.0737: Decaying DM in Composite Messenger - E.Ponton, L.Randall, 0811.1029: Singlet DM - A.Ibarra, D.Tran, 0811.1555: Decaying DM - S.Baek, P.Ko, 0811.1646: U(1) Lmu-Ltau DM - C.Chen, F.Takahashi, T.T.Yanagida, 0811.3357: Decaying Hidden-Gauge-Boson DM - I.Cholis, G.Dobler, D.Finkbeiner, L.Goodenough, N.Weiner, 0811.3641: 700+ GeV WIMP - E.Nardi, F.Sannino, A.Strumia, 0811.4153: Decaying DM in TechniColor - K.Zurek, 0811.4429: Multicomponent DM - M.Ibe, H.Murayama, T.T.Yanagida, 0812.0072: Breit-Wigner enhancement of DM annihilation - E.Chun, J.-C.Park, 0812.0308: sub-GeV hidden U(1) in GMSB - M.Lattanzi, J.Silk, 0812.0360: Sommerfeld enhancement in cold substructures - M.Pospelov, M.Trott, 0812.0432: super-WIMPs decays DM - Zhang, Bi, Liu, Liu, Yin, Yuan, Zhu, 0812.0522: Discrimination with SR and IC - Liu, Yin, Zhu, 0812.0964: DMnu from GC - M.Pohl, 0812.1174: electrons from DM - J.Hisano, M.Kawasaki, K.Kohri, K.Nakayama, 0812.0219: DMnu from GC - A.Arvanitaki, S.Dimopoulos, S.Dubovsky, P.Graham, R.Harnik, S.Rajendran, 0812.2075: Decaying DM in GUTs - R.Allahverdi, B.Dutta, K.Richardson-McDaniel, Y.Santoso, 0812.2196: SuSy B-L DM- S.Hamaguchi, K.Shirai, T.T.Yanagida, 0812.2374: Hidden-Fermion DM decays - D.Hooper, A.Stebbins, K.Zurek, 0812.3202: Nearby DM clump - C.Delaunay, P.Fox, G.Perez, 0812.3331: DMnu from Earth - Park, Shu, 0901.0720: Split- UED DM - .Gogoladze, R.Khalid, Q.Shafi, H.Yuksel, 0901.0923: cMSSM DM with additions - Q.H.Cao, E.Ma, G.Shaughnessy, 0901.1334: Dark Matter: the leptonic connection - E.Nezri, M.Tytgat, G.Vertongen, 0901.2556: Inert Doublet DM - C.-H.Chen, C.-Q.Geng, D.Zhuridov, 0901.2681: Fermionic decaying DM - J.Mardon, Y.Nomura, D.Stolarski, J.Thaler, 0901.2926: Cascade annihilations (light non-abelian new bosons) - P.Meade, M.Papucci, T.Volansky, 0901.2925: DM sees the light - D.Phalen, A.Pierce, N.Weiner, 0901.3165: New Heavy Lepton - T.Banks, J.-F.Fortin, 0901.3578: Pyrma baryons - Goh, Hall, Kumar, 0902.0814: Leptonic Higgs - K.Bae, J.-H. Huh, J.Kim, B.Kyae, R.Viollier, 0812.3511: electrophilic axion from flipped-SU(5) with extra spontaneously broken symmetries and a two component DM with Z 2 parity - ...
Results Which DM can fit the data? M.Pospelov and A.Ritz, 0810.1502: Secluded DM - A.Nelson and C.Spitzer, 0810.5167: Slightly Non-Minimal DM - Y.Nomura and J.Thaler, 0810.5397: DM through the Axion Portal - R.Harnik and G.Kribs, 0810.5557: Dirac DM - D.Feldman, Z.Liu, P.Nath, 0810.5762: Hidden Sector - T.Hambye, 0811.0172: Hidden Vector - Yin, Yuan, Liu, Zhang, Bi, Zhu, 0811.0176: Leptonically decaying DM - K.Ishiwata, S.Matsumoto, T.Moroi, 0811.0250: Superparticle DM - Y.Bai and Z.Han, 0811.0387: sUED DM - P.Fox, E.Poppitz, 0811.0399: Leptophilic DM - C.Chen, F.Takahashi, T.T.Yanagida, 0811.0477: Hidden-Gauge-Boson DM - K.Hamaguchi, E.Nakamura, S.Shirai, T.T.Yanagida, 0811.0737: Decaying DM in Composite Messenger - E.Ponton, L.Randall, 0811.1029: Singlet DM - A.Ibarra, D.Tran, 0811.1555: Decaying DM - S.Baek, P.Ko, 0811.1646: U(1) Lmu-Ltau DM - C.Chen, F.Takahashi, T.T.Yanagida, 0811.3357: Decaying Hidden-Gauge-Boson DM - I.Cholis, G.Dobler, D.Finkbeiner, L.Goodenough, N.Weiner, 0811.3641: 700+ GeV WIMP - E.Nardi, F.Sannino, A.Strumia, 0811.4153: Decaying DM in TechniColor - K.Zurek, 0811.4429: Multicomponent DM - M.Ibe, H.Murayama, T.T.Yanagida, 0812.0072: Breit-Wigner enhancement of DM annihilation - E.Chun, J.-C.Park, 0812.0308: sub-GeV hidden U(1) in GMSB - M.Lattanzi, J.Silk, 0812.0360: Sommerfeld enhancement in cold substructures - M.Pospelov, M.Trott, 0812.0432: super-WIMPs decays DM - Zhang, Bi, Liu, Liu, Yin, Yuan, Zhu, 0812.0522: Discrimination with SR and IC - Liu, Yin, Zhu, 0812.0964: DMnu from GC - M.Pohl, 0812.1174: electrons from DM - J.Hisano, M.Kawasaki, K.Kohri, K.Nakayama, 0812.0219: DMnu from GC - A.Arvanitaki, S.Dimopoulos, S.Dubovsky, P.Graham, R.Harnik, S.Rajendran, 0812.2075: Decaying DM in GUTs - R.Allahverdi, B.Dutta, K.Richardson-McDaniel, Y.Santoso, 0812.2196: SuSy B-L DM- S.Hamaguchi, K.Shirai, T.T.Yanagida, 0812.2374: Hidden-Fermion DM decays - D.Hooper, A.Stebbins, K.Zurek, 0812.3202: Nearby DM clump - C.Delaunay, P.Fox, G.Perez, 0812.3331: DMnu from Earth - Park, Shu, 0901.0720: Split- UED DM - .Gogoladze, R.Khalid, Q.Shafi, H.Yuksel, 0901.0923: cMSSM DM with additions - Q.H.Cao, E.Ma, G.Shaughnessy, 0901.1334: Dark Matter: the leptonic connection - E.Nezri, M.Tytgat, G.Vertongen, 0901.2556: Inert Doublet DM - C.-H.Chen, C.-Q.Geng, D.Zhuridov, 0901.2681: Fermionic decaying DM - J.Mardon, Y.Nomura, D.Stolarski, J.Thaler, 0901.2926: Cascade annihilations (light non-abelian new bosons) - P.Meade, M.Papucci, T.Volansky, 0901.2925: DM sees the light - D.Phalen, A.Pierce, N.Weiner, 0901.3165: New Heavy Lepton - T.Banks, J.-F.Fortin, 0901.3578: Pyrma baryons - Goh, Hall, Kumar, 0902.0814: Leptonic Higgs - K.Bae, J.-H. Huh, J.Kim, B.Kyae, R.Viollier, 0812.3511: electrophilic axion from flipped-SU(5) with extra spontaneously broken symmetries and a two component DM with Z 2 parity - ...
Results Which DM spectra can fit the data? Model-independent results: fit to PAMELA positrons * + balloon experiments *adding anti-protons does not change much, non-leptonic channels give too smooth spectrum for balloons
Results Which DM spectra can fit the data? Model-independent results: fit to PAMELA positrons * + balloon experiments (1) annihilate into leptons (e.g. ), mass 1 TeV µ + µ − ∼
Data sets Electrons + positrons from FERMI: “Designed as a high-sensitivity FERMI-LAT gamma-ray observatory, (Usa + France +Italy + Germany + Japan + Sweden) the FERMI Large Area Telescope is also an electron detector with a large acceptance”
Data sets Electrons + positrons adding FERMI: FERMI 2009 e + + e − 10 � 1 - no excess HESS 2009 HESS 2008 - spectrum . ATIC 2008 ∼ E − 3 . 04 PPB � BETS EC � AMS � � � � � � � � E 3 � e � � e � � GeV 2 � cm 2 sec � � � � � � � HEAT � � � � � CAPRICE94 � � � � � � � � � � ���� � � Tang et al. 1984 � � ��� � � � � � � � � � � � � � � � � � � ������������� � � � � � � � � � � � � � � � 10 � 2 � � � � � � � � � � � � � � background ? � � � � � 10 � 3 10 2 10 3 10 4 10 energy in GeV [formerly predicted GLAST sensitivity]
Results Which DM spectra can fit the data?
Results Which DM spectra can fit the data? µ + µ − , M DM ≃ 1 TeV 10 � 1 FERMI 2009 HESS 2008 ATIC 2008 E 3 � e � � e � � in GeV 2 � cm 2 s sr � � ��� � � � � � � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � � �� � � � � � � � 10 � 3 10 2 10 3 10 4 10 Energy in GeV
Results Which DM spectra can fit the data? µ + µ − , M DM ≃ 1 TeV 10 � 1 FERMI 2009 HESS 2008 ATIC 2008 E 3 � e � � e � � in GeV 2 � cm 2 s sr � � ��� � � � � � � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � τ + τ − , M DM ≃ 2 TeV � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � � �� � � 10 � 1 � � � FERMI 2009 � HESS 2008 � ATIC 2008 E 3 � e � � e � � in GeV 2 � cm 2 s sr � � ��� � � � � � � 10 � 3 � � � � � � � � 10 2 10 3 10 4 10 � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � Energy in GeV � � � � � � 10 � 2 � � � � � � � � �� � � � � � � � 10 � 3 10 2 10 3 10 4 10 Energy in GeV
Results Which DM spectra can fit the data? µ + µ − , M DM ≃ 1 TeV 10 � 1 FERMI 2009 HESS 2008 ATIC 2008 E 3 � e � � e � � in GeV 2 � cm 2 s sr � � ��� � � � � � � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � τ + τ − , M DM ≃ 2 TeV � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � � �� � � 10 � 1 � � � FERMI 2009 � HESS 2008 � ATIC 2008 E 3 � e � � e � � in GeV 2 � cm 2 s sr W + W − , M DM ≃ 10 TeV � � ��� � � � � � � 10 � 3 � � � � � � � � 10 2 10 3 10 4 10 � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � 10 � 1 Energy in GeV � � � � � � 10 � 2 � � � � � � FERMI 2009 � � �� HESS 2008 � ATIC 2008 � E 3 � e � � e � � in GeV 2 � cm 2 s sr � � � � � ��� � � � � � � � � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � 10 � 3 � �� 10 2 10 3 10 4 10 � � Energy in GeV � � � � � 10 � 3 10 2 10 3 10 4 10 Energy in GeV
Results Which DM spectra can fit the data? Notice: µ + µ − , M DM ≃ 1 TeV - same spectra still fit PAMELA positron and anti-protons! Caveats: 10 � 1 - scanning non- systematically propagation parameters FERMI 2009 HESS 2008 ATIC 2008 - varying background (within errors) E 3 � e � � e � � in GeV 2 � cm 2 s sr � � ��� � � � - annihilations only (direct ones; and no decay) � � � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � τ + τ − , M DM ≃ 2 TeV � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � � �� � � 10 � 1 � � � FERMI 2009 � HESS 2008 � ATIC 2008 E 3 � e � � e � � in GeV 2 � cm 2 s sr W + W − , M DM ≃ 10 TeV � � ��� � � � � � � 10 � 3 � � � � � � � � 10 2 10 3 10 4 10 � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � 10 � 1 Energy in GeV � � � � � � 10 � 2 � � � � � � FERMI 2009 � � �� HESS 2008 � ATIC 2008 � E 3 � e � � e � � in GeV 2 � cm 2 s sr � � � � � ��� � � � � � � � � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � 10 � 3 � �� 10 2 10 3 10 4 10 � � Energy in GeV � � � � � 10 � 3 10 2 10 3 10 4 10 Energy in GeV
Results Which DM spectra can fit the data? Notice: µ + µ − , M DM ≃ 1 TeV - same spectra still fit PAMELA positron and anti-protons! Caveats: 10 � 1 - scanning non- systematically propagation parameters FERMI 2009 HESS 2008 ATIC 2008 - varying background (within errors) E 3 � e � � e � � in GeV 2 � cm 2 s sr � � ��� � � � - annihilations only (direct ones; and no decay) � � � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � τ + τ − , M DM ≃ 2 TeV � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � � �� � � 10 � 1 � � � FERMI 2009 � HESS 2008 � ATIC 2008 E 3 � e � � e � � in GeV 2 � cm 2 s sr W + W − , M DM ≃ 10 TeV � � ��� � � � � � � 10 � 3 � � � � � � � � 10 2 10 3 10 4 10 � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � 10 � 1 Energy in GeV � � � � � � 10 � 2 � � � � � � FERMI 2009 � � �� HESS 2008 � ATIC 2008 � E 3 � e � � e � � in GeV 2 � cm 2 s sr � � � � � ��� � � � � � � � � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � 10 � 3 � �� 10 2 10 3 10 4 10 � � Energy in GeV � � � � - no features => � M DM > 1 TeV 10 � 3 - smooth lepton spectrum 10 2 10 3 10 4 10 Energy in GeV
Results Which DM spectra can fit the data? y Notice: µ + µ − , M DM ≃ 1 TeV r - same spectra still fit PAMELA positron and anti-protons! a Caveats: 10 � 1 n - scanning non- systematically propagation parameters FERMI 2009 HESS 2008 ATIC 2008 - varying background (within errors) E 3 � e � � e � � in GeV 2 � cm 2 s sr i � � ��� � � � - annihilations only (direct ones; and no decay) � � m � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � τ + τ − , M DM ≃ 2 TeV � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � � i �� � � l 10 � 1 � � e � FERMI 2009 � HESS 2008 � ATIC 2008 E 3 � e � � e � � in GeV 2 � cm 2 s sr W + W − , M DM ≃ 10 TeV r � � ��� � � � � � � 10 � 3 � � � � � � P � � 10 2 10 3 10 4 10 � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � 10 � 1 Energy in GeV � � � � � � 10 � 2 � � � � � � FERMI 2009 � � �� HESS 2008 � ATIC 2008 � E 3 � e � � e � � in GeV 2 � cm 2 s sr � � � � � ��� � � � � � � � � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � 10 � 3 � �� 10 2 10 3 10 4 10 � � Energy in GeV � � � � - no features => � M DM > 1 TeV 10 � 3 - smooth lepton spectrum 10 2 10 3 10 4 10 Energy in GeV
Results Which DM spectra can fit the data? y Notice: µ + µ − , M DM ≃ 1 TeV r - same spectra still fit PAMELA positron and anti-protons! a Caveats: 10 � 1 n - scanning non- systematically propagation parameters FERMI 2009 HESS 2008 ATIC 2008 - varying background (within errors) E 3 � e � � e � � in GeV 2 � cm 2 s sr i � � ��� � � � - annihilations only (direct ones; and no decay) � � m � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � τ + τ − , M DM ≃ 2 TeV � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � � i �� � � l 10 � 1 � � e � FERMI 2009 � HESS 2008 � ATIC 2008 E 3 � e � � e � � in GeV 2 � cm 2 s sr W + W − , M DM ≃ 10 TeV r � � ��� � � � � � � 10 � 3 � � � � � � P � � 10 2 10 3 10 4 10 � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � 10 � 1 Energy in GeV � � � � � � 10 � 2 � � � � � � FERMI 2009 � � �� HESS 2008 � ATIC 2008 � E 3 � e � � e � � in GeV 2 � cm 2 s sr � � � � � ��� � � � � � � � � � � � � � � � � � � ���� � �� ��� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � ������ � � � � � � � � � � � � 10 � 2 � � � � � � � 10 � 3 � �� 10 2 10 3 10 4 10 � � Energy in GeV � � � � � See e.g. Strumia, Papucci et al. ( to appear) 10 � 3 10 2 10 3 10 4 10 Energy in GeV see also: Bergstrom, Edsjo, Zaharijas today
Indirect Detection Indirect Detection from DM annihilations in galactic center γ ( − ) ( − ) DM p , and W − , Z, b, τ − , t, h . . . � e ∓ , D . . . γ ( − ) ( − ) W + , Z, ¯ b, τ + , ¯ t, h . . . � e ± , p , and D . . . DM γ typically sub-TeV energies
Indirect Detection Indirect Detection from DM annihilations in Sagittarius Dwarf γ ( − ) ( − ) DM p , and W − , Z, b, τ − , t, h . . . � e ∓ , D . . . γ ( − ) ( − ) W + , Z, ¯ b, τ + , ¯ t, h . . . � e ± , p , and D . . . DM γ
Indirect Detection Indirect Detection e ± radio-waves from synchrotron radiation of in GC e ± S S N N (energy in B ~ kinetic energy) e ± - compute the population of from DM annihilations in the GC - compute the synchrotron emitted power for different configurations of galactic � B (assuming ‘scrambled’ B; in principle, directionality could focus emission, lift bounds by O(some))
Indirect Detection Indirect Detection e ± from Inverse Compton on in halo γ e ± e ± - upscatter of CMB, infrared and starlight photons on energetic - probes regions outside of Galactic Center
Comparing with data
Gamma constraints HESS has detected -ray γ emission from Gal Center and Gal Ridge. The DM signal must not excede that. HESS coll. 0 1 -1
Gamma constraints HESS has detected -ray γ Gal Center emission from Gal Center and Gal Ridge. The DM signal must not excede that. HESS coll. 0 1 -1
Gamma constraints HESS has detected -ray γ emission from Gal Center Gal Ridge and Gal Ridge. The DM signal must not excede that. HESS coll. 0 1 -1
Gamma constraints HESS has detected -ray γ emission from Gal Center and Gal Ridge. The DM signal must not excede that. HESS coll. 0 1 -1 Data: HESS coll., astro-ph/0408145 and astro-ph/0610509 σ v ann = 10 − 23 cm 3 / sec k O
Gamma constraints HESS has detected -ray γ emission from Gal Center and Gal Ridge. The DM signal must not excede that. HESS coll. 0 1 -1 Data: HESS coll., astro-ph/0408145 and astro-ph/0610509 σ v ann = 10 − 23 cm 3 / sec σ v ann = 10 − 23 cm 3 / sec o N k O Data: HESS coll., astro-ph/0603021
Gamma constraints HESS has detected -ray γ emission from Gal Center and Gal Ridge. The DM signal must not excede that. HESS coll. Moreover: no detection from 0 1 -1 Sgr dSph => upper bound. Data: HESS coll., astro-ph/0408145 and astro-ph/0610509 σ v ann = 10 − 23 cm 3 / sec σ v ann = 10 − 23 cm 3 / sec o N k O Data: HESS coll., astro-ph/0603021
Gamma constraints EGRET and FERMI have measured diffuse -ray γ emission. The DM signal must not excede that. FERMI coll. 10 � 20 region 10 � 60 region Data: EGRET coll.,Strong et al. astro-ph/0406254 10 � 1 10 � 1 Σ v ann � 5 10 � 22 cm 3 � s DM DM � W � W � Σ v ann � 5 10 � 23 cm 3 � s DM DM � Μ � Μ � M DM � 10 TeV NFW Profile 2 d � � d Ε 1 � MeV cm � 2 s � 1 sr � 1 � M DM � 1.5 TeV IsoT Profile 2 d � � d Ε 1 � MeV cm � 2 s � 1 sr � 1 � EGRET Data: FERMI coll., several talks in 2009 10 � 2 EGRET 10 � 2 FERMI 10 � 3 Preliminary Total Total CMB IR 10 � 3 10 � 4 IR CMB SL Ε 1 Ε 1 SL 10 � 4 10 � 5 10 10 2 10 3 10 4 10 5 10 6 10 10 2 10 3 10 4 10 5 10 6 10 7 Photon energy Ε 1 � MeV � Photon energy Ε 1 � MeV �
Galactic Center constraints γ +ATIC-2 GC − γ GR − γ The PAMELA and ATIC regions are in conflict with gamma constraints, unless... Bertone, Cirelli, Strumia, Taoso 0811.3744
Galactic Center constraints γ Bertone, Cirelli, Strumia, Taoso 0811.3744 see also: Bertone, Pieri, Pato today
Galactic Center constraints γ Bertone, Cirelli, Strumia, Taoso 0811.3744 ...not-too-steep profile needed.
Galactic Center constraints γ Bertone, Cirelli, Strumia, Taoso 0811.3744 ...not-too-steep profile needed. Or: take different boosts here (at Earth, for e + ) than there (at GC, for gammas). Or: take ad hoc DM profiles (truncated at 100 pc, with central void..., after all we don’t know ).
Inverse Compton constraints γ DM DM � ΜΜ , Einasto profile 10 � 20 10 � 21 10 � 22 Σ v � cm 3 � s � 10 � 23 EGRET 5 � 30 10 � 24 EGRET 10 � 60 The PAMELA EGRET 10 � 20 and ATIC regions 10 � 25 FERMI 10 � 20 are in conflict with gamma 10 � 26 constraints, 10 2 10 3 10 4 M DM � GeV � unless... Cirelli, Panci 0904.3830
Inverse Compton constraints γ DM DM � ee, Einasto profile DM DM � ΜΜ , Einasto profile DM DM � ΤΤ , Einasto profile 10 � 20 10 � 20 10 � 20 10 � 21 10 � 21 10 � 21 10 � 22 10 � 22 10 � 22 Σ v � cm 3 � s � Σ v � cm 3 � s � Σ v � cm 3 � s � 10 � 23 10 � 23 10 � 23 EGRET 5 � 30 EGRET 5 � 30 EGRET 5 � 30 10 � 24 EGRET 10 � 60 10 � 24 EGRET 10 � 60 10 � 24 EGRET 10 � 60 EGRET 10 � 20 EGRET 10 � 20 EGRET 10 � 20 10 � 25 FERMI 10 � 20 10 � 25 FERMI 10 � 20 10 � 25 FERMI 10 � 20 10 � 26 10 � 26 10 � 26 10 2 10 3 10 4 10 2 10 3 10 4 10 2 10 3 10 4 M DM � GeV � M DM � GeV � M DM � GeV � DM DM � ee, IsoT profile DM DM � ΜΜ , IsoT profile DM DM � ΤΤ , IsoT profile 10 � 20 10 � 20 10 � 20 10 � 21 10 � 21 10 � 21 10 � 22 10 � 22 10 � 22 Σ v � cm 3 � s � Σ v � cm 3 � s � Σ v � cm 3 � s � 10 � 23 10 � 23 10 � 23 EGRET 5 � 30 EGRET 5 � 30 EGRET 5 � 30 10 � 24 EGRET 10 � 60 10 � 24 EGRET 10 � 60 10 � 24 EGRET 10 � 60 EGRET 10 � 20 EGRET 10 � 20 EGRET 10 � 20 10 � 25 FERMI 10 � 20 10 � 25 FERMI 10 � 20 10 � 25 FERMI 10 � 20 10 � 26 10 � 26 10 � 26 10 2 10 3 10 4 10 2 10 3 10 4 10 2 10 3 10 4 M DM � GeV � M DM � GeV � M DM � GeV � Cirelli, Panci 0904.3830 see also: Regis, Ullio 0904.4645
DM annihilations: the game Dark Matter annihilations
DM annihilations: the game huge σ ann v Dark Matter annihilations ordinary, thermal σ ann v
DM annihilations: the game huge σ ann v Dark Matter annihilations ordinary, thermal σ ann v
DM annihilations: the game PAMELA positrons huge σ ann v Dark Matter annihilations ordinary, thermal σ ann v
DM annihilations: the game PAMELA positrons huge σ ann v Dark Matter annihilations ordinary, thermal σ ann v
DM annihilations: the game PAMELA positrons leptons only huge σ ann v Dark Matter annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, WW, qq
DM annihilations: the game PAMELA positrons leptons only huge σ ann v Dark Matter annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, WW, qq
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, WW, qq
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, WW, qq
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, WW, qq
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, WW, qq
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ −
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ −
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ −
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ −
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e -
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - 1 < 3 TeV, τ + τ −
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - 1 < 3 TeV, τ + τ −
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - 1 < 3 TeV, τ + τ − ray & radio γ constraints HESS
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - 1 < 3 TeV, τ + τ − standard (NFW, Ein) DM profiles ray & radio γ constraints HESS distrust the GC
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - 1 < 3 TeV, τ + τ − standard (NFW, Ein) DM profiles ray & radio γ constraints HESS distrust the GC
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - 1 < 3 TeV, τ + τ − standard (NFW, Ein) DM profiles ray & radio γ constraints HESS distrust the GC
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - 1 < 3 TeV, τ + τ − standard (NFW, Ein) DM profiles ray & radio γ constraints HESS distrust the GC diffuse ICS γ constraints EGRET + FERMI
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - (?) 1 < 3 TeV, τ + τ − standard (NFW, Ein) standard (NFW, Ein) DM profiles DM profiles ray & radio γ constraints HESS smooth (isothermal) distrust the GC DM profiles diffuse ICS γ constraints EGRET + FERMI
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - (?) 1 < 3 TeV, τ + τ − standard (NFW, Ein) standard (NFW, Ein) DM profiles DM profiles ray & radio γ constraints HESS smooth (isothermal) distrust the GC DM profiles diffuse ICS γ constraints EGRET + FERMI
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - (?) 1 < 3 TeV, τ + τ − standard (NFW, Ein) standard (NFW, Ein) DM profiles DM profiles ray & radio γ constraints HESS smooth (isothermal) distrust the GC DM profiles diffuse ICS γ constraints EGRET + FERMI
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - (?) 1 < 3 TeV, τ + τ − standard (NFW, Ein) standard (NFW, Ein) DM profiles DM profiles ray & radio γ constraints HESS smooth (isothermal) distrust the GC DM profiles diffuse ICS γ ?? numerical constraints simulations?! EGRET + FERMI
DM annihilations: the game PAMELA anti-p PAMELA positrons leptons only huge σ ann v Dark Matter ATIC 2+4 annihilations ordinary, ordinary, thermal σ ann v mixed BRs 10 TeV, 1 TeV, WW, qq µ + µ − FERMI e + +e - HESS e + +e - (?) 1 < 3 TeV, τ + τ − standard (NFW, Ein) standard (NFW, Ein) DM profiles DM profiles ray & radio γ constraints HESS smooth (isothermal) distrust the GC DM profiles diffuse ICS γ ?? numerical constraints simulations?! EGRET + FERMI
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