Pos(EPS-HEP 2009)012 ∗ Astrumia@Df.Unipi.It Speaker

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PoS(EPS-HEP 2009)012 http://pos.sissa.it/ ∗ [email protected] Speaker. We summarize the status of Dark Matter,the focussing cosmic-ray on excess recent observed developments, by mostly PAMELA prompted and by FERMI. ∗ Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. c

European Physical Society Europhysics Conference onJuly High 16 Energy - Physics, 22 EPS-HEP 2009 2009, Krakow, Poland Dipartimento di Fisica dell’Università di PisaE-mail: and INFN, Italia Alessandro Strumia Dark Matter Theory PoS(EPS-HEP 2009)012 DM DM ]. This is all 1 ? 2 (1.1) Alessandro Strumia collider . 005 [ . weak multiplet that 0 0 , heavier DM masses 2 ∼ ± v one M π 4 110 . SM SM / 0 4 g = ∼ 2 h at velocity σ DM Ω DM SM is typical of weak scale particles. If DM v 2 σ 0025 . TeV 0

? 2 = : we assume that DM fills direct g 3 sec cm 26 . Many theories of Dark Matter, such as the MSSM, are − g SM 10 DM · 3 ]. The following table shows in the few main cases the predicted ≈ 13 Pl M 1 SM SM , we need to predict L now ? M T ≈ v σ cosmology ? ) suggests DM at the weak scale: the key question is if DM is expected to be light and H 1.1 indirect Eq. ( Cosmology and astrophysics established that DM exists, but so far could see DM only via its DM DM . In order to predict compatible with a wide range of DMM couplings, and consequently with a wide range of DM masses enough to be produced at the LHC.are As obtained a typical for cross larger section DM is couplings only has gauge interactions [ 2. Cosmology and colliders i.e. i) we hope toto see see end-products DM of scattering astrophysical on DMof normal annihilations which matter; in SM iii) cosmic particle we rays; is hope ii)next involved to in sections we produce we DM hope DM summarize couplings, at the we various LHC. do possibilities. As not we know have which no search idea is better. In the the positive information we havecollision-less so far dust on can DM. be Various DM: boundsthe from tell latter that case an the anything oscillating DM that ultra-light cosmologicalstandard behaves scalar abundance as big-bang: to could be a in determined neutral such byvalue new a of thermal particle. case the freeze-out DM within the In annihilation observed cross DM section: abundance is reproduced for a well defined where numerical values include order one factors.is This the relic of a weak scale particle, we can soon discover in the following three ways: gravitational interactions, weighting the total DM amount: Dark Matter Theory 1. Introduction PoS(EPS-HEP 2009)012 is (2.1) DM ). This Ω 2.1 2 Alessandro Strumia cm in 3 3 3 3 . . . . 45 SI − σ gets kinematically sup- ) − W + 100GeV. Weaker bounds apply 100/fb 10 W 12 1 1 ∼ = 400 0 200 0 → ∼ ∼ M ∼ ∼ dt for L 2 R cm DM DM is around or above 1 TeV. This is bad for two ( 2 5 7 6 0 12 43 54 . . . . σ . − 2 9 M 3 10 ∼ < SI σ − wino 2 nick- DM mass Events at LHC name in TeV stable higgsino 1 sneutrino 0 , the too large 2 2 2 W / / / Spin Y ) 22 0 1 1 is resonantly enhanced if the pseudo-scalar Higgs happens to have a mass / / ( σ U ). L M ) 2 ( 22 1 3 1 3 05 0 0 0 1 1 Quantum numbers SU , presently constrained to be SI σ pressed. Such a possibility, realized e.g. inby ‘intert LEP Higgs doublet’ searches. models is not fully excluded If DM is acan mixture reduce between DM a gauge gauge couplingsis neutral possible allowing singlet within any with the DM MSSM, gauge masshiggsino where charged and lighter a wino. multiplet(s), than DM one in neutralino is table an arbitrary ( mixing betweenDM bino, could be apossibility singlet within which the MSSM, only withleptons has DM and some as sleptons, non-gauge a but interactions. binoobtained it only with if got supergauge sleptons This mostly are Yukawa just was interactions excluded abovethe to the their by MSSM LEP is LEP best bound. that (Another searches. possibility allowedvery within The close observed to 2 Within the MSSM, the main channelproduction for DM of production gluinos at that the LHC cascadelong-lived is decay NLSP not down can direct give to but clean indirect the extra DM signals. LSP. If DM is the gravitino, the If DM is lighter than the Experiments searched for DM elastic scatterings on a variety of nuclei; the main parameter • • • • if DM is heavier or lighter. used to compare their datanucleon, with theory is the spin-independent DM cross section on an average 3. Direct searches reasons: DM heavier than alost TeV would in be the hardly backgrounds) discoverable and atthe would LHC electroweak not (the scale. suggest low event a DM rate clean lighterunless can connection than one get with a or the more TeV annihilates hierarchy of the too problem following much of possibilities leaving are a realized: too low abundance, The main message is that the typical DM mass Dark Matter Theory DM masses (taking into account co-annihilations and Sommerfeld enhancements): PoS(EPS-HEP 2009)012 . 2 g N scatter- DM W N somewhat N 4 SI 6 W m σ 4 ± M Α N loop » DM Alessandro Strumia ] is not confirmed, ] observed an unex- SI 5 4 Σ W N DM . This naturally happens if DM 2 g N 4 N 6 h m DM h 2 M Α ), which is excluded by a few orders of magnitude, scalar 4 , » contamination in PAMELA, etc.). We here focus on fraction in cosmic rays, suggesting the existence of 1.1 SI p tree ) N Σ DM with mass difference around 100 keV, the DM kinetic − e 0 N + in eq. ( 0 + σ e ( / DM is correspondingly smaller than + e Z → ] observations still demonstrate a deviation from the naive power-law N 7 ]. These possibilities will be soon confirmed or excluded by running exper- -exchange, higgs exchange, loop mediation. comparable to 2 Z : SI N 2 N 4 σ Z SI m DM Z σ 2 M spectrum: although the peak hinted by previous ATIC data [ Α vector ] and HESS [ , » + 6 e , producing an excess in their cosmic ray fluxes. ¯ SI d tree N Σ + , DM γ − , e ¯ p ] or an inelastic DM , 3 DM annihilations or decays around the Milky Way can produce SM particles that decay into This topic attracted interest because recently the PAMELA experiment [ The following Feynman diagrams illustrate three possible sources of DM/nucleon scattering The Higgs exchange effect is suppressed by the nucleon mass, but still gives a The loop effect, present if DM lies in a weak multipletThe with positive charged signal heavier components, claimed is by the DAMA experiment is compatible with null results of all p , -exchange give a ± spectrum, indicating an excessfluxes compared at to the conventional Earth. background Thepulsar, predictions or excess of could could be cosmic be an ray due experimental mistake to ( a new astrophysical component, such as a nearby pected rise with energy of the the FERMI [ iments, and appear already disfavored by present data. 4. Indirect searches e energy in our galaxy [ Z unless the DM coupling to the a new positron component.in The the sharp rise suggests that the new component may be visible also and their typical Dark Matter Theory is a real particle (a real scalar or a Majorana fermion like the neutralino). above the experimental bounds unless the DM coupling to the Higgs is somewhat smaller than within the sensitivity of planned experiments. other experiments only if DM has unexpected properties, such as a form factor in DM ing [ PoS(EPS-HEP 2009)012 1000 brehm . 3 100 GeV − in E ] and the 10 8 energy 1 Photon s Alessandro Strumia IC 0.1 3 star CMB dust cm FERMI09 22 0.01 5 6 7 8 - - - - -

10 10 10 10

Γ F sr sec cm GeV in E d d E

2 ´ 2 with MED diffusion [ a, signaling a new component. 2.0 1 − 4 = τ 10 v + Σ τ à à à ò à à ì with ò ì 3 à ì - à ì ò æ 10 ì ò Τ à æ ò ì æ GeV + ò ì æ ò ì Τ æ ò ì in ò æ ò æ æ ò æ ò æ into æ æ 2 ò æ 5 ò æ Energy ò æ 10 ò æ ò æ æ ò æ æ ò æ æ ò æ æ æ æ ò , with any DM mass above about 100 GeV; b) DM that can be computed in a model-independent way. Z FERMI HESS08 HESS09 ¯ p annihilates 10 , + 0.01 0.03

e that

0.003

or of

L + H

sec cm GeV e e E

+ - 2 3 2 W TeV 3. 4 = 10 10GeV are affected by the solar activity and thereby provide essentially ﬂux compared with the FERMI and HESS data. Right: the DM contribution M . We consider DM annihilations into − ∼ e 3 + with GeV 10 + in DM energy 2 ? spectrum. 10 æ PAMELA excess 08 + shows the PAMELA (left) and FERMI, HESS (middle) data together with a possible æ e à + æ Positron ì 1 e æ à ì æ æ background æ æ à ì æ æ 10 ò PAMELA æ à æ ì æ Observations below According to standard astrophysics, the positron/electron fraction above 10 GeV should de- As directions of charged comic rays get randomized by galactic magnetic ﬁelds, the infor- Fig. PAMELA data suggest two classes of DM interpretations for the excess: a) DM that annihilates ò æ à ì æ ò à % % % % æ ì æ 1 3 ò à ì æ

30 10

ò à ì Positron fraction crease with energy, while PAMELA finds the steep increase in fig. no information on the underlying particle physics. mation lies in the energyor spectra. anti-protons. Dark Observations Matter so couldficulty far manifest is have as been bringing an made above excess only thediscriminating in below the atmosphere the 100 sign a rarer of GeV: large positrons the the charge. enough experimental Furthermore, calorimeter dif- cosmic with ray a fluxes roughly spectrometer decrease able as of DM fit. 4.1 The the most interesting possibility: thethan excess a could new background be to the Dark first Matter manifestation searches. of Dark Matter, rather isothermal DM profile: all good fitsexcess. are very Middle: similar. Left: the the e positronto fraction the compared with diffuse the photon PAMELA energy(black spectra thick produced by line); bremsstrahlung we (dashed also(blue). red curve) separately and show Inverse the Compton 3 IC components from star-light (red), CMB (green), dust As the relevant DM annihilations intothe pairs energy of spectra SM of particles the are final non-relativistic, stable given any channel Figure 1: Sample DM fits into pairs of charged leptons, of annihilates into pairs of quarks or higgs,give but a only soft if DM is heavier than a few TeV, as these channels Dark Matter Theory æ ì ò à ò ò PoS(EPS-HEP 2009)012 at , nor W much ) , mak- propa- r leptons ( m is heavy M p produces ρ τ / , such that , M m excess, giv- µ data only if M M charge. (We , ∼ > + e p ± e v e channel. A Alessandro Strumia , and PAMELA is − v W + ]. W 13 excess, but only above 100 → fraction compatible with the , and analogous to the classi- p ) ). Non-relativistic DM annihi- p DM excess can be suppressed if the − and typically is a few order of / e p p 1.1 + M e → does not depend on − v µ for small velocities down to σ + ]. This phenomenon is fully analogous to the v µ ], if DM has a multi-TeV mass: in such a case 9 ( / ]. Indeed DM annihilations into with energy equal to the DM mass 12 σ [ 10 6 W comparable to the escape velocity from the Milky , W 9 ] observation of a ¯ 3 20% uncertainty. The ¯ − ± 16 10 , so a p ∼ excess is accompanied by a ¯ m ) can be more resonantly enhanced than cosmological anni- v -wave, such that 3 + s > e would grow as 1 − , these channels are compatible with PAMELA ¯ p v 1 E 10 σ ∼ , which is above the energy range observed by PAMELA if v W needed to fit PAMELA grows with M ]. More interestingly, if DM is charged under a vector with mass 3 / − 11 background M , must be one of the main DM annihilation channels [ p 10 propagation model in the turbulent galactic magnetic fields. 9 p excess, as leptons do not decay into protons. On the contrary all other DM m ]. Indeed let us consider for example the DM DM − ± ≈ ATIC, FERMI and HESS observations p e 2) [ > W v 17 . − p + , e 0 9 at E W + ∼ v PAMELA observations + v ¯ σ → p e cosmic ray spectrum, made by calorimeters that cannot discriminate the backgrounds are predicted with a plausible − e ¯ p 10TeV [ These experiments provide the best measurements of the electron plus positron cosmic ray The Adding to the data-set the PAMELA [ The result does not depend much on the unknown DM density profile in our galaxy, Various ways out have been proposed, such as a non-standard cosmologies or a DM clump 1 + ∼ > + -channel DM annihilations mediated by a narrow particle with a mass very close to 2 GeV. 4.3 The spectrum, although ATIC was designed totons. observe nuclei, The and growing FERMI excess andbecome in HESS of to the order observe positron pho- unity fraction ate observed TeV by energies, PAMELA so below that 100 it GeV is could interesting to consider measurements of the astrophysical background restricts the range ofing possible another DM hint interpretations in for favor the of lepto-philic DM [ enough. (Final State Radiationleave produces open some protons the with possibility lower that energy). the Thereby DM models diffusion zone is small, e.g. if it extends away from the galactic plane for only 1 kpc, as in the so-called MIN possibility. Way) nor on the on the typical galactic DM velocity ( magnitude larger than the value suggested by cosmology of eq. ( lighter than DM, the resulting attractivetheir long-range annihilation cross force section: between pairs ofing DM PAMELA compatible particles with enhances standard cosmology [ 4.2 The do not give anychannels ¯ are significantly constrained:gation trusting and for the the availableM astrophysical ¯ models for ¯ protons with QED Sommerfeld enhancement of processes like DM DM close to us. A possibles particle-physics way of reconciling PAMELA with standard cosmology is Dark Matter Theory lations should be dominated bynot the compatible with standard cosmology. astrophysical annihilations ( hilations ( rest produces (anti)protons with cal enhancement of the probability of fallingIn into the the DM sun case, in the view lighter of vector its could long range be attractive the gravity. PoS(EPS-HEP 2009)012 , ν − 9 ’s: e π + and + . e γ γ in γ u ]. New vectors 18 Alessandro Strumia ’s are unavoidably excess. Indeed the γ − ]. Models where DM 10GeV, being probed e and possibly into 14 ∼ + µ 2 , ) + e e e , probed by HESS. However annihilations. If the vectors can fit the PAMELA, FERMI m / M − e fraction will continue to grow at decays, and µ E ∼ VV ( + + τ γ γ e µ E E → ∼ and 0 and γ µ − E excess predict related excesses in yield, while models involving neutral light τ + γ ± τ e with ]. 0 7 γ 15 0± with the largest e γ → γ ± e energy loss is proportional to the energy density ) give the largest ± yield. γ Thereby DM predicts that the e 2 γ . This gives 2 ± interpretations of the → ` scatterings on the galactic ambient light (CMB and star light, partially 0 − ± π ` . e + 1 : from ` → ]. 18 , obtaining Sommerfeld-enhanced DM DM in matter shower in an exponential way, so that calorimeters become more precise V observations ± energy spectrum significantly depends on the DM annihilation mode: modes involving e ν γ spectrum is harder than what expected, and the data indicate two spectral features in it, (that decay into − by FERMI. The resulting the τ vectors give the smallest rescattered by dust) give rise to Bremsstrahlung Inverse Compton and e The DM DM We do not consider the possibility of a DM component that terminates compensated by a new astrophysical com- Models where DM is lighter than about a TeV (such as a 200 GeV supersymmetric wino [ Interesting theories are constructed adding to the SM a DM particle charged under a new light One year ago the ATIC balloon had the best measurement, and its data showed a peak around If both features are real, DM annihilations into γ 2 1. 2. + ]) can no longer produce the PAMELA excess, as it would terminate below 1 TeV where FERMI + fluxes. Indeed neutrinos aregenerated unavoidably by generated 3 different by processes: ponent that grows. is lighter than thethis proton, scenario it nicely explains can why only DM could decay annihilate into only the intowith leptons lighter GeV-scale mass [ leptons mixed with photons can bein searched dedicated for in electron low-energy beam-dump experiments, experiments especially [ higher energy as in fig. 4.4 data show a smooth spectrum. ‘dark vector’ 19 and HESS data [ 700 GeV. The FERMI experiment now provides the first high-statistics measurement of the Dark Matter Theory recall that and easily reach higher energies, where spectrometersprecise see and all eventually tracks useless). as quasi-straight becoming less spectrum, which do not confirme the ATIC peak, butsuggesting still that indicate the an excess appearsare around clearly larger 100 than GeV the statistical and errors terminatesuncertainties, and it around although seems 1 unlikely only that TeV. These the they could features FERMIfeatures be collaboration due really to can systematic there? answer thetermination crucial HESS of question: observations the around are excess. these andclearly visible The above once take-over 1 FERMI of data TeV at a independently lower new energies indicate will component be the around published. 100 GeV should become annihilations give 4 leptons with a smooth energy spectrum can fit all the data [ PoS(EPS-HEP 2009)012 . ) ∼ ` γ Γ Γ Γ - - m - E / profile GC GR dS 4 excess 10 M ( ± e ln GeV / in FERMI ) isothermal ` energy loss is , and - 3 mass Τ m 10 ± + / excesses with the Τ e DM Alessandro Strumia IC m ® ± ( e PAMELA radio , Inverse Compton is - -body simulations re- ) DM ] fluxes do not exceed x GC ~ N Ν ( 2 21 B 10 DM [ at radio-frequencies, 20 22 24 26 u - - - -

γ ν

10 10 10 10

sec cm in v Σ 3 energy goes into IC, irrespec- ± e ] and 20 Γ Γ Γ [ suggested by the - - annihilations are thereby excluded, if - profile γ GC GR dS -body DM simulations, the DM density 4 − M 10 ` N , WMAP. The resulting + ` and GeV in v FERMI isothermal → , σ c: all DM models able of ﬁtting the - and 2 in magnetic ﬁelds. 3 mass AVIES Μ 1 / 10 8 + 2 Μ DM IC excess is present in all the DM halo. As the energy B ® PAMELA radio ± = - e DM B GC ]. . Ν 2 u σ 10 DM 22 24 26 20 22 - - - -

10 10 10 10

FSR ﬂux is roughly reduced by a factor ln

sec cm in v Σ 3 γ . observations of the Galatic Center (blue continuous line), of the Galactic bounds [ γ γ u γ Γ Γ Γ - - is about one order of magnitude larger than - profile GC GR dS ) 4 x ~ 10 ( diffuse in the galactic magnetic fields, radiating γ ]) we compare the values of u ± excesses in terms of DM DM GeV excess is now strongly constrained by FERMI, HESS and PAMELA, the IC 18 e in FERMI isothermal ± : ± , e and - e 3 bounds, computed imposing that the DM mass e 10 ’ region. + e injection from DM annihilations is effectively equivalent to have the smoother DM ◦ ν DM IC (from [ ® ν 20 PAMELA eV, probed by radio-observations: D , radio 2 - γ 6 and ÷ We compare the region favored by PAMELA (green bands) and by PAMELA, FERMI and HESS DM , GC ◦ − γ 2 ± 10 DM e 10 Synchrotron 10 proportional to the energy density 26 20 22 24 - - - - Inverse Compton presently does not provide the dominant constraint, but it plays an important We needed to consider the quasi-constant ‘isothermal’ DM density profile because otherwise, Models where DM annihilates into two light vectors that decay into lepton pairs (giving rise to In fig.

10 10 10 10

sec cm in v Σ states) are less constrained: the 3 flux can be reliably computed to be as in fig. -body simulations reliably predict the DM density profile. ` around the Galactic Center would havepretations been of so large the that various bounds would be violated. Inter- rôle. First because it directly probes if the density profile suggested by spectrum of the γ had we assumed the Einasto or NFW profiles favored by various the various observations by more than 3 N 4 Despite that, a DM densitymains profile again more needed. constant If than the what lightof vectors suggested the have by a long kpc-scale life-time, the consequent smoothing Figure 2: observations (red ellipses) with Ridge (blue dot-dashed), of sphericalin dwarfes the (blue ‘ dashed), with neutrino data, with FERMI observations Dark Matter Theory As it is believed that dominant, and it can betively reliably of computed the precise as value essentially of all the PoS(EPS-HEP 2009)012 c) 1 Γ Ν Γ - - dS GC 4 10 profile excesses. GeV ± e in FERMI NFW (left). Γ , - and - 3 mass µ Τ GR 10 + 4 Τ DM Alessandro Strumia

® radio - PAMELA

GC DM IC 2 (right), 10 − 27 26 25 24 23 He. . . and thereby modify-

10 10 10 10 10

Τ - sec in time life DM + data have been released only τ γ , the region considered in ﬁg. ◦ He, D, 4 Γ Ν Γ - - (middle), dS GC 4 − and 20 10 10, heat gas. However the effect depends profile µ ◦ + ∼ GeV µ z in FERMI NFW 1000 reionize H after matter/radiation decou- Γ , - - and 3 ∼ mass < Μ GR 10 satellite. 9 + z Μ DM

® radio - PAMELA

GC excesses in terms of DM decays solves three difﬁculties DM IC 2 ± LANCK e 10 24 23 27 26 25

10 10 10 10 10

Τ - sec in time life DM ] indicate a hint of an excess: a precise understanding of instru- excess. eV i.e. redshift MeV affect BBN fragmenting c shows that forthcoming FERMI data at higher energies should 26 1 γ ∼ < ∼ Γ Ν Γ T - , here for DM decaying into are at the level of what needed by DM interpretations of the - T 2 dS GC v 4 10 re-couple to matter, affecting the anisotropy pattern of CMB. σ ]: profile γ 23 GeV in FERMI Γ NFW As in ﬁg. - , and 3 mass Μ GR 10 4 DM ® radio - PAMELA

DM GC IC 2 Figure 3: 10 ing their abundances. However, their primordial abundances are not safely measured. pling, such that on the unknown non-linear small-scale DM clustering. 25 24 23 27 26

The alternative interpretation of the Preliminary FERMI data [ The DM annihilation rate, being proportional to the DM density squared, is enhanced in the

10 10 10 10 10

- Τ time life DM sec in 2. DM annihilations at 1. DM annihilations at 3. DM annihilations after structure formation, at hopefully test the DM-related 4.6 DM decay faced by DM annihilations. First, theone decay does rate not is need not to linked invent with Sommerfeld cosmological or freeze-out, other so enhancements. that Second, cosmological constraints early universe by the largerthe DM universe history density, [ affecting cosmological observables in various stages of and only below 10 GeV: fig. mental and astrophysical backgrounds is needed to hopefully reach a4.5 conclusion. Constraints from cosmology All these constraints on The second constraint is themeasurements strongest being performed and by most the robust P one, and it can be improved by the CMB Dark Matter Theory predict roughly the same ICin flux. one angular Second, region because (with so galactic latitude far between FERMI 10 PoS(EPS-HEP 2009)012 p γ ]. ν ± e , m 25 γ / , M T 24 / [ M 5 − e M / ∼ b spectra. However 4 Alessandro Strumia GUT Ω ). ± M / sec. DM that decays are polluted by extra − e e 26 ± ∼ DM e + 10 e τ Ω cosmic rays measured by to chiral fermions. ∼ v ± τ e π bounds for the Einasto profile is quasi-constant, a possibility 4 ν ) . on galactic star-light and CMB. ∼ r excesses compatibly with all γ ( ± ρ ± M e modes are compatible with bounds and e is again preferred. γ τ 3TeV and ) or excluded ( ) . Or maybe that nor in r γ − ( ∼ e p ρ + injection term is less enhanced close to the M e γ − 3TeV provides one of the best fits to the , e and in can fit the ± + ≈ e ± e − 10 e µ M flux, so that + and γ µ − − coupling gives mass with shows that, as a result, the DM decay interpretation of the µ µ π + 3 + − 4 µ µ µ bounds even for a NFW DM density profile. 3TeV provides one of the best fits to the ∼ : thereby the + 2 or ν µ λ ≈ , ρ − − γ τ M µ imply a large + + τ µ 0 π is large. Fig. with → ρ − -body simulations τ ]. DM might be not the only particle charged under the new strong interactions: N + VV -body simulations: a more constant τ rather than to 24 N → ρ → excess is present everywhere in the DM halo (rather than only close to us, as if the observations only if the (effective) DM density decays into ± γ e τ fewTeV [ and cosmological constraints. disfavored by the from spectra. This solution is marginallyfavored compatible by with ∼ 100GeV, the cosmological DM abundance is naturally obtained as If the The on-going analysis will have a huge impact on the Dark Matter field. Maybe the final result We see that the needed DM mass and lifetime are The most plausible scenario for DM is that it is theMaybe relic we of have a already new weak seen scale the particle. first If signals. true, The excesses in - DM DM - DM DM - DM that decays into M excesses is compatible with ∼ [1] WMAP collaboration, arXiv:astro-ph/0603449. [2] For a recent summary see D.P. Finkbeiner, T. Lin, N. Weiner, arXiv:0906.0002. ± astrophysical backgrounds, and DM did not show up in ¯ References will be evidence for lepto-philic Dark Matter in via a GUT-suppressed dimension 6 operator naturally give the needed Other channels are less favored (e.g. excess is produced by aaround 100 nearby GeV, generated pulsar), by FERMI Inverse Compton should scattering be of able to observe a related excess of e Furthermore, if DM iskept a in proton-like thermal particle, equilibrium compositeT by of sphalerons chiral down fermions, to withfor the an electroweak asymmetry symmetry breaking scale at as well known the few TeVhierarchy scale puzzle, independently where appears a in strong technicolor solutions to the higgs mass Galactic Center where we should soon see direct and/or indirect signals of DM, and produce DM at the LHC. Dark Matter Theory do not apply, as theproportional DM to life-time is not enhanced in the early universe. Third, the decay rate is 5. Conclusions PAMELA, FERMI (or ATIC) and HESSor can decays be into interpreted leptonic final in states. terms The of following Dark solutions Matter emerge: annihilations PoS(EPS-HEP 2009)012 Alessandro Strumia 11 . I hope that collider physics will take advantage by such procedure, now fermi.gsfc.nasa.gov common in astrophysics and cosmology, making all LHC data public. [arXiv:astro-ph/0306207]. [arXiv:0810.5292]. W. L. Guo and Y. L. Wu, Phys. Rev. D 79 (2009) 055012 [arXiv:0901.1450]. J. Hisano, S. Matsumoto and M.M. M. Cirelli, Nojiri, A. Phys. Strumia, Rev. M. Lett. Tamburini, 92 Nucl. (2004) Phys. 031303. B787 (2007) 152 [arXiv:0706.4071]. therein. S. Galli, F. Iocco, G. BertoneT. and R. A. Slatyer, Melchiorri, N. Phys. Padmanabhan, Rev. D.P. D Finkbeiner,G. Phys. 80 Huetsi, Rev. (2009) A. D 023505 Hektor 80 [arXiv:0905.0003]. and (2009) M. 043526M. Raidal, [arXiv:0906.1197]. Cirelli, arXiv:0906.4550. F. Iocco and P. Panci, arXiv:0907.0719. site [3] B. Feldstein, A.L. Fitzpatrick, E. Katz,[4] arXiv:0908.2991. PAMELA collaboration, arXiv:0810.4995. [5] ATIC collaboration, Nature 456 (2008) 362. [6] FERMI/LAT collaboration, arXiv:0905.0025. [7] H.E.S.S. Collaboration, arXiv:0811.3894. H.E.S.S. Collaboration, arXiv:0905.0105. [8] F. Donato, N. Fornengo, D. Maurin and P. Salati, Phys. Rev. D[9] 69, 063501 (2004) M. Cirelli, M. Kadastik, M. Raidal, A. Strumia, Nucl. Phys. B813 (2009) 1 [arXiv:0809.2409]. Dark Matter Theory [10] F. Donato, D. Maurin, P. Brun, T. Delahaye and P. Salati, Phys. Rev.[11] Lett. 102 M. (2009) Ibe, 071301 H. Murayama and T. T. Yanagida, arXiv:0812.0072. [12] A. Sommerfeld, Ann. Phys. 403 (1931) 257. [13] M. Cirelli, R. Franceschini, A. Strumia, Nucl. Phys. B800 (2008) 204[14] [arXiv:0802.3378] and ref.s N. Arkani-Hamed, D. P. Finkbeiner, T. Slatyer[15] and N. J.D. Weiner, arXiv:0810.0713. Bjorken, R. Essig, P. Schuster, N.[16] Toro, arXiv:0906.0580. PAMELA collaboration, arXiv:0810.4994. [17] T. Delahaye, R. Lineros, F. Donato, N.[18] Fornengo and P. Meade, P. Salati, M. arXiv:0712.2312. Papucci, A. Strumia, T.[19] Volansky, arXiv:0905.0480. P. Grajek, G. Kane, D. Phalen,[20] A. Pierce and G. S. Bertone, Watson, M. arXiv:0812.4555. Cirelli, A. Strumia,[21] M. Taoso, J. JCAP Hisano, 0901 M. (43) Kawasaki, 2009 K. [arXiv:0811.3744]. Kohri[22] and K. I. Nakayama, Z. arXiv:0812.0219. Rothstein, T. Schwetz and[23] J. Zupan, J. arXiv:0903.3116. Hisano, M. Kawasaki, K. Kohri, T. Moroi and K. Nakayama, arXiv:0901.3582. [24] E. Nardi, F. Sannino A. Strumia,[25] JCAP 0903 (009) A. 2009 Arvanitaki et [arXiv:0811.4153]. al., arXiv:0812.2075. [26] In view of a contract with NASA, every photon detected by FERMI is publicly available at the web