dark matter constraints from gamma-ray boxes
Transcrição
dark matter constraints from gamma-ray boxes
dark matter constraints from gamma-ray boxes Miguel Pato Physik-Department T30d, TU Munich with Alejandro Ibarra, Hyun Min Lee, Sergio Lopez Gehler and Wan-Il Park [JCAP07(2012)043, arXiv:1205.0007] [JCAP05(2013)016, arXiv:1303.6632] NWPAC 2014, Braga, 29 Jan 2014 1. the quest for wimps long-awaited data are being collected as we speak... direct searches indirect searches wimp scattering o nuclei underground yields of wimp annihilation or decay wimp production in the lab collider searches complementarity and uncertainty are key for wimp identication miguel pato (tu munich) 1. the quest for wimps long-awaited data are being collected as we speak... direct searches indirect searches wimp scattering o nuclei underground yields of wimp annihilation or decay { gamma rays { wimp production in the lab collider searches complementarity and uncertainty are key for wimp identication miguel pato (tu munich) 2. indirect dark matter searches Milky Way edge−on dark halo bulge/bar Sun Galactic Centre thin disk thick disk not to scale! 0= @ fp = r (K (T ; ~r )rfp ) @t r (V~c (~r )fp ) 2h (z ) ann fp + Q (T ; ~r ) solar modulation F = 500 MV miguel pato (tu munich) 2. indirect dark matter searches Milky Way edge−on dark halo 111 000 000 111 000 111 Sun not to scale! 0= @ fp = r (K (T ; ~r )rfp ) @t r (V~c (~r )fp ) 2h (z ) ann fp + Q (T ; ~r ) solar modulation F = 500 MV miguel pato (tu munich) 2. indirect dark matter searches Milky Way edge−on dark halo 111 000 000 111 000 111 p e q p e q Sun not to scale! 0= @ fp = r (K (T ; ~r )rfp ) @t r (V~c (~r )fp ) 2h (z ) ann fp + Q (T ; ~r ) solar modulation F = 500 MV miguel pato (tu munich) 2. indirect dark matter searches Milky Way edge−on dark halo 111 000 000 111 000 111 p Vc p Sun diffusive halo not to scale! 0= @ fp = r (K (T ; ~r )rfp ) @t r (V~c (~r )fp ) 2h (z ) ann fp + Q (T ; ~r ) solar modulation F = 500 MV miguel pato (tu munich) 2. indirect searches via gamma rays Milky Way edge−on dark halo 111 000 000 111 000 111 Sun not to scale! gamma-ray \propagation" bkg ! e +e bkg ! e ! e open window for . 10 Mpc sources of < 100 TeV or > 1020 eV photons ! no attenuation, no shift in energy nor direction miguel pato (tu munich) 2. indirect searches via gamma rays Milky Way edge−on dark halo 111 000 000 111 000 111 Sun not to scale! gamma-ray \propagation" bkg ! e +e bkg ! e ! e open window for . 10 Mpc sources of < 100 TeV or > 1020 eV photons ! no attenuation, no shift in energyZnor direction 1 hv i dN 1 = 4 m2 dE d Jann miguel pato (tu munich) 2. indirect searches via gamma rays the paradigmatic case of gamma rays 100 MeV { 100 GeV 100 GeV { 100 TeV miguel pato (tu munich) widely-used data but not fully explored yet need to make the best of the available data 2. indirect searches via gamma rays the paradigmatic case of gamma rays 100 MeV { 100 GeV 100 GeV { 100 TeV miguel pato (tu munich) widely-used data but not fully explored yet need to make the best of the available data 2. indirect searches via gamma rays dwarf galaxies galaxy clusters clumps galactic centre extragalactic halo anisotropies miguel pato (tu munich) 2. indirect searches via gamma rays anisotropies extragalactic diuse galaxy clusters galactic centre dwarfs target/constraint misc miguel pato (tu munich) 1e−23 1e−22 NFW,bb e us i rm 1e−24 1e−25 Ferm agal tr i ex ff di Fe ax Ferm rn i Fo c acti nt ic ce re t ac l Fermi anisotropies SS fs i rm ga HE ar dw Fe thermal 1e−26 sigma*v [cm3/s] 2. indirect searches via gamma rays 1 10 100 m [GeV] miguel pato (tu munich) 1e3 1e4 1e−23 1e−22 NFW,bb e us i rm 1e−24 1e−25 Ferm agal tr i ex ff di Fe ax Ferm rn i Fo c acti nt ic ce re t ac l Fermi anisotropies SS fs i rm ga HE ar dw Fe thermal 1e−26 sigma*v [cm3/s] 2. indirect searches via gamma rays 1 10 100 1e3 1e4 m [GeV] ... but these are all for integrated uxes miguel pato (tu munich) 2. indirect searches via gamma rays 1 hv i dN 1 Z d Jann = 4 m 2 dE for sources in the open window, we can pinpoint injection spectrum # look for spectral features miguel pato (tu munich) 2. indirect searches via gamma rays 1 hv i dN 1 Z d Jann = 4 m 2 dE for sources in the open window, we can pinpoint injection spectrum # look for spectral features astrophysical backgrounds at high energies nuclear lines inverse Compton synchrotron bremsstrahlung pion decay MeV / E (p+1)=2 / E (p+1)=2 / E p / E p (caveat: monoen e in KN) p&2 anything harder than E 2 and at high energies will stick out and can be cleanly looked for miguel pato (tu munich) 2. gamma-ray spectral features 1 lines dN dE / (E m ) dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 [Srednicki+ '86, Rudaz+ '86, Bergstrom & Snellman '88] convoluted m miguel pato (tu munich) Eg 2. gamma-ray spectral features 1 lines dN dE / (E m ) dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 [Srednicki+ '86, Rudaz+ '86, Bergstrom & Snellman '88] convoluted m 2 internal bremsstrahlung dN dE / E 1 \hard" in astroph dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 m miguel pato (tu munich) Eg [Bergstrom '89, Flores+ '89, Bringmann+ '07] Eg 2. gamma-ray spectral features 1 lines dN dE / (E m ) dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 [Srednicki+ '86, Rudaz+ '86, Bergstrom & Snellman '88] convoluted m dN dE / E 1 \hard" in astroph dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 m 3 boxes miguel pato (tu munich) Eg [Ibarra, Lopez Gehler & MP '12] dN dE / const dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 Eg [Bergstrom '89, Flores+ '89, Bringmann+ '07] m Eg hardness 2 internal bremsstrahlung 2. gamma-ray spectral features 1 lines dN dE / (E m ) Eg 2 dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 [Srednicki+ '86, Rudaz+ '86, Bergstrom & Snellman '88] convoluted m dN dE / E 1 \hard" in astroph Eg 2 dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 m 3 boxes miguel pato (tu munich) Eg [Ibarra, Lopez Gehler & MP '12] dN dE / const Eg 2 dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 Eg [Bergstrom '89, Flores+ '89, Bringmann+ '07] m Eg hardness 2 internal bremsstrahlung 2. gamma-ray spectral features 1 lines dN dE / (E m ) Eg 2 dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 [Srednicki+ '86, Rudaz+ '86, Bergstrom & Snellman '88] convoluted m dN dE Eg 2 dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 / const m 3 internal bremsstrahlung miguel pato (tu munich) dN dE Eg [Bergstrom '89, Flores+ '89, Bringmann+ '07] / E 1 \hard" in astroph Eg 2 dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 Eg [Ibarra, Lopez Gehler & MP '12] m Eg hardness 2 boxes 2. gamma-ray spectral features 1 lines dN dE / (E m ) Eg 2 dNg/dEg [Srednicki+ '86, Rudaz+ '86, Bergstrom & Snellman '88] convoluted m dN dE Eg 2 dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 / const m 3 internal bremsstrahlung Eg [Bergstrom '89, Flores+ '89, Bringmann+ '07] / E 1 \hard" in astroph Eg 2 dNg/dEg dN dE miguel pato (tu munich) Eg [Ibarra, Lopez Gehler & MP '12] m Eg hardness 2 boxes 2. gamma-ray spectral features 1 lines dN dE / (E m ) dNg/dEg [Srednicki+ '86, Rudaz+ '86, Bergstrom & Snellman '88] convoluted m hard and up to HE dN / const dE dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 −2.x Eg m 3 internal bremsstrahlung Eg [Bergstrom '89, Flores+ '89, Bringmann+ '07] / E 1 \hard" in astroph dNg/dEg dN dE miguel pato (tu munich) Eg [Ibarra, Lopez Gehler & MP '12] m Eg hardness 2 boxes 2. gamma-ray spectral features 1 lines dN dE / (E m ) dNg/dEg [Srednicki+ '86, Rudaz+ '86, Bergstrom & Snellman '88] convoluted m hard and up to HE dN / const dE dNg/dEg 11111 00000 00000 11111 00000 11111 00000 11111 −2.x Eg alternative signature with implications for a new class of models 3 internal bremsstrahlung m Eg [Bergstrom '89, Flores+ '89, Bringmann+ '07] / E 1 \hard" in astroph dNg/dEg dN dE miguel pato (tu munich) Eg [Ibarra, Lopez Gehler & MP '12] m Eg hardness 2 boxes 3. box phenomenology 1-step cascades 1 X 3 ... 11111 00000 00000 11111 00000 11111 00000 11111 ... 2 = 3 (EX0 + 3 pX0 cos 0 ) Z Z Z dN dN 1 d cos 0 EX X dEX dE3 dE3 3 1 2 F [E0 3 (1 = 23AB 3 E0 box = miguel pato (tu munich) X 0 dEX0 dN dEX0 f ( ) (EX 3 ); E0 3 (1 + 3 )] 3 (EX0 + 3 pX0 cos 0 )) dN3 =dE3 = A(E3 E3 ) dNX =dEX0 = B (EX0 E0 ) 3. box phenomenology 1-step cascades 1 X 3 ... 11111 00000 00000 11111 00000 11111 00000 11111 ... 2 = 3 (EX0 + 3 pX0 cos 0 ) Z Z Z dN dN 1 d cos 0 EX X dEX dE3 dE3 3 1 2 = 23AB F [E0 3 (1 3 E0 box = 1 2 lab miguel pato (tu munich) (...) 3 cm X 0 dEX0 dN dEX0 f ( ) (EX 3 ); E0 3 (1 + 3 )] 3 (EX0 + 3 pX0 cos 0 )) dN3 =dE3 = A(E3 E3 ) dNX =dEX0 = B (EX0 E0 ) 3. box phenomenology 1 X dNX/dEX 1-step cascades 3 ... 11111 00000 00000 11111 00000 11111 00000 11111 ... 2 E− EX = 3 (EX0 dNX dEX Z1 Z d cos 0 dE 0 dNX f (0 ) (E 3 dE3 dN X X dE 0 dE3 1 2 X = 23AB F [E0 3 (1 3 ); E0 3 (1 + 3 )] 3 E0 box Z = X 1 2 (...) 3 (...) lab miguel pato (tu munich) E 3 0 E+ EX + 3 pX0 cos 0 ) cm cm3 3 (EX0 + 3 pX0 cos 0 )) dN3 =dE3 = A(E3 E3 ) dNX =dEX0 = B (EX0 E0 ) 3. box phenomenology 1 X dNX/dEX 1-step cascades 3 ... 11111 00000 00000 11111 00000 11111 00000 11111 ... 2 E− EX = 3 (EX0 dNX dEX Z1 Z d cos 0 dE 0 dNX f (0 ) (E 3 dE3 dN X X dE 0 dE3 1 2 X = 23AB F [E0 3 (1 3 ); E0 3 (1 + 3 )] 3 E0 box Z = 1 2 lab miguel pato (tu munich) E 3 0 E+ EX + 3 pX0 cos 0 ) (...) 3 cm X cm3 3 (EX0 + 3 pX0 cos 0 )) dN3 =dE3 = A(E3 E3 ) dNX =dEX0 = B (EX0 E0 ) 3. box phenomenology 1 X dNX/dEX 1-step cascades 3 ... 11111 00000 00000 11111 00000 11111 00000 11111 ... 2 E− EX = 3 (EX0 dNX dEX Z1 Z d cos 0 dE 0 dNX f (0 ) (E 3 dE3 dN X X dE 0 dE3 1 2 X = 23AB F [E0 3 (1 3 ); E0 3 (1 + 3 )] 3 E0 box Z = 1 2 lab miguel pato (tu munich) E 3 0 E+ EX + 3 pX0 cos 0 ) (...) 3 cm X cm3 3 (EX0 + 3 pX0 cos 0 )) dN3 =dE3 = A(E3 E3 ) dNX =dEX0 = B (EX0 E0 ) 3. box phenomenology 1 X dNX/dEX 1-step cascades 3 ... 11111 00000 00000 11111 00000 11111 00000 11111 ... 2 E− EX = 3 (EX0 Z1 Z d cos 0 dE 0 dNX f (0 ) (E 3 dE3 dN X X dE 0 dE3 1 2 X = 23AB F [E0 3 (1 3 ); E0 3 (1 + 3 )] 3 E0 box Z = E+ 3 (EX0 1 2 (...) 3 no spin −1 lab miguel pato (tu munich) EX cm cm3 + 3 pX0 cos 0 )) dN3 =dE3 = A(E3 E3 ) dNX =dEX0 = B (EX0 E0 ) f dNX dEX E 3 0 + 3 pX0 cos 0 ) 1 cos 3. box phenomenology 1 X dNX/dEX 1-step cascades 3 ... 11111 00000 00000 11111 00000 11111 00000 11111 ... 2 E− EX = 3 (EX0 E+ EX (isotropic emission) Z1 Z d cos 0 dE 0 dNX f (0 ) (E (E 0 + p 0 cos 0 )) 3 = dE3 dN 3 X 3 X X X dE 0 dE3 1 2 X dN3 =dE3 = A(E3 E3 ) = 23AB F box [E0 3 (1 3 ); E0 3 (1 + 3 )] dNX =dEX0 = B (EX0 E0 ) 3 E0 Z f dNX dEX E 3 0 + 3 pX0 cos 0 ) 1 2 (...) 3 no spin −1 lab miguel pato (tu munich) cm cm3 1 cos 3. box phenomenology 1 X dNX/dEX 1-step cascades 3 ... 11111 00000 00000 11111 00000 11111 00000 11111 ... 2 E− EX = 3 (EX0 Z1 Z d cos 0 dE 0 dNX f (0 ) (E 3 dE3 dN X X dE 0 dE3 1 2 X = 23AB F [E0 3 (1 3 ); E0 3 (1 + 3 )] 3 E0 box Z = E+ 3 (EX0 1 2 (...) 3 spin −1 lab miguel pato (tu munich) EX cm cm3 + 3 pX0 cos 0 )) dN3 =dE3 = A(E3 E3 ) dNX =dEX0 = B (EX0 E0 ) f dNX dEX E 3 0 + 3 pX0 cos 0 ) 1 cos 3. box phenomenology 1 X dNX/dEX 1-step cascades 3 ... 11111 00000 00000 11111 00000 11111 00000 11111 ... 2 E− EX = 3 (EX0 E+ EX (isotropic emission) Z1 Z d cos 0 dE 0 dNX f (0 ) (E (E 0 + p 0 cos 0 )) 3 = dE3 dN 3 X 3 X X X dE 0 dE3 1 2 X dN3 =dE3 = A(E3 E3 ) = 23AB F box [E0 3 (1 3 ); E0 3 (1 + 3 )] dNX =dEX0 = B (EX0 E0 ) 3 E0 Z f dNX dEX E 3 0 + 3 pX0 cos 0 ) 1 2 (...) 3 no spin −1 lab miguel pato (tu munich) cm cm3 1 cos 3. box phenomenology boxes are realised in nature!p p 11111 00000 00000 11111 00000 11111 00000 11111 p ... = E0 (1 + cos 0 ) Z dN 2 Fbox [m (1 dN = dE dE dE 2 m =2 p E if E m =2 / p if E m =2 E E miguel pato (tu munich) )=2; m (1 + )=2] dN =dE / E p dN =dE0 = 2(E0 m =2) 3. box phenomenology boxes are realised in nature!p p 11111 00000 00000 11111 00000 11111 00000 11111 p ... = E0 (1 + cos 0 ) Z dN 2 Fbox [m (1 dN = dE dE dE 2 m =2 p E if E m =2 / p if E m =2 E E miguel pato (tu munich) )=2; m (1 + )=2] dN =dE / E p dN =dE0 = 2(E0 m =2) 3. box phenomenology [Ibarra, Gehler & MP '12; Ibarra, Lee, Gehler, Park & MP '13] dNg/dEg gamma-ray boxesp a 11111 00000 00000 11111 00000 11111 00000 11111 a E E− = E0 a (1 + a cos 0 ) dN dE = 4E Fbox [E r E = 2 1 1 m ma2 ; E+ ] m2 E+ Eg dNa =dEa = 2(Ea m ) dN =dE0 = 2(E0 ma =2) .. as ma ! m : a 0, E+ E , E 0 .. as ma ! 0: a 1, E+ m , E 0 miguel pato (tu munich) Ec Ec = m2 line at m =2 box ending at m 3. box phenomenology [Ibarra, Gehler & MP '12; Ibarra, Lee, Gehler, Park & MP '13] dNg/dEg gamma-ray boxesp a 11111 00000 00000 11111 00000 11111 00000 11111 a E E− = E0 a (1 + a cos 0 ) dN dE = 4E Fbox [E r E = 2 1 1 m ma2 ; E+ ] m2 E+ Eg dNa =dEa = 2(Ea m ) dN =dE0 = 2(E0 ma =2) .. as ma ! m : a 0, E+ E , E 0 .. as ma ! 0: a 1, E+ m , E 0 miguel pato (tu munich) Ec Ec = m2 line at m =2 box ending at m 3. methodology 10 [Ibarra, Gehler & MP '12; Ibarra, Lee, Gehler, Park & MP '13] -6 centre region ΦΓ @GeV -1cm -2s -1sr -1D 10 -7 10 mDM = 100 GeV <Σv> = 3 10 -26cm 3s -1 -8 10 -9 10 -10 99.9 mΦ = 10 GeV 40 60 m ' m : moderate ne-tuning line at m =2 with 4 (usual line is at m with 2 ) wide box 95 m : no ne-tuning at all high-energy shoulder at m amplitude saturation as m ! 0 m 10 -11 2 narrow box 5 10 20 50 EΓ @GeV D 100 200 .. narrow box is harder, but wide box extends to higher energies ! similar constraints (!) .. sub-thermal constraints in both cases (!) miguel pato (tu munich) 3. methodology 10 [Ibarra, Gehler & MP '12; Ibarra, Lee, Gehler, Park & MP '13] -6 centre region ΦΓ @GeV -1cm -2s -1sr -1D 10 -7 10 mDM = 100 GeV <Σv> = 3 10 -26cm 3s -1 -8 10 -9 99.9 mΦ = 10 GeV 10 -10 40 60 m ' m : moderate ne-tuning line at m =2 with 4 (usual line is at m with 2 ) wide box 95 m : no ne-tuning at all high-energy shoulder at m amplitude saturation as m ! 0 m 10 -11 2 narrow box 5 10 20 50 EΓ @GeV D 100 200 .. narrow box is harder, but wide box extends to higher energies ! similar constraints (!) .. sub-thermal constraints in both cases (!) derivation of constraints conservative: no background, ;b = 0 intermediate: scaled-down background t ;b / E (iii) aggressive: background meets measurements, error-dominated (i) (ii) miguel pato (tu munich) 4. results: constraints target: jl j 2 [0; 36] , jb j 2 [5; 36] ; jl j 2 [0; 7] , jb j 2 [0; 5] (Fermi-LAT centre region; Vertongen & Weniger '11) ! ! 4 10 -25 10 -25 centre region intermediate approach <Σv> @cm3s -1D 10 -28 .. .. .. .. 10 20 50 100 mDM @GeV D D m mDM = 0.001 D m mDM = 0.05 D m mDM = 0.4 D m mDM = 0.9 200 500 1000 ediate interm essiv aggr 10 -28 10 -29 5 e rvativ conse 10 -27 10 -27 10 -29 5 <Σv> @cm 3s -1D 10 -26 10 -26 centre region D m mDM = 0.001 10 20 e Vertongen & Weniger H2011L 50 100 mDM @GeVD 200 500 1000 [Ibarra, Gehler & MP '12] saturation of constraints as m ! 0 constraints across parameter space, not only in ne-tuned regions background modelling important at small m no direct comparison to usual lines, but similar results miguel pato (tu munich) 4. results: constraints target: Region 3 (Fermi-LAT; Weniger '12) jl j < 0:8 , jb j < 0:3 (H.E.S.S. '06) ! aa 10 - 23 narrow box m a m Χ = 0.999 ! 4 10 - 23 10 2 10 - 24 wide box m a m Χ = 0.1 10 - 24 thermal 10 - 26 1 10 -1 AT L i- 3 10 - 25 10 - 26 10 - 2 S. S. AT 10 2 m Χ @GeVD 10 3 10 4 1 10 -1 rm 10 - 27 10 - 2 conservative aggressive 10 - 28 10 thermal L i- Fe m r Fe E. H. XΣv\ aa XΣv\ th . .S S E. H. XΣv\ aa XΣv\ th 10 - 25 10 XΣv\ aa @cm sD 3 XΣv\ aa @cm sD 10 10 - 27 10 2 conservative aggressive 10 - 28 10 10 2 m Χ @GeVD 10 3 10 4 [Ibarra, Lee, Gehler, Park & MP '13] .. H.E.S.S. meets Fermi-LAT and extends to multi-TeV .. rst ever gamma-ray box constraints at TeV energies .. thermal x-sec probed for m ' 10 GeV few TeV future ACTs can probe boxes from thermal x-sec above 10 TeV, a region hardly accessible to direct, collider and other indirect searches miguel pato (tu munich) 4. results: constraints target: Region 3 (Fermi-LAT; Weniger '12) jl j < 0:8 , jb j < 0:3 (H.E.S.S. '06) ! aa ! 4 10 - 23 narrow box m a m Χ = 0.999 10 2 10 - 24 10 - 25 E. H. 10 - 26 S. S. thermal 1 10 -1 AT -L mi 10 - 27 XΣv\ aa XΣv\ th 3 XΣv\ aa @cm sD 10 r Fe 10 - 2 conservative aggressive 10 - 28 10 10 2 m Χ @GeVD 10 3 10 4 [Ibarra, Lee, Gehler, Park & MP '13] .. H.E.S.S. meets Fermi-LAT and extends to multi-TeV .. rst ever gamma-ray box constraints at TeV energies .. thermal x-sec probed for m ' 10 GeV few TeV future ACTs can probe boxes from thermal x-sec above 10 TeV, a region hardly accessible to direct, collider and other indirect searches miguel pato (tu munich) 4. results: constraints Region 3 (Fermi-LAT; Weniger '12) jl j < 0:8 , jb j < 0:3 (H.E.S.S. '06) ! aa ! 4 10 - 23 narrow box m a m Χ = 0.999 3 direct XΣv\ aa @cm sD 10 - 24 10 - 25 10 E. H. 10 - 26 S. S. thermal 1 10 -1 AT -L mi 10 - 27 10 2 XΣv\ aa XΣv\ th target: r Fe 10 - 2 conservative aggressive 10 - 28 10 10 2 m Χ @GeVD 10 3 10 4 [Ibarra, Lee, Gehler, Park & MP '13] .. H.E.S.S. meets Fermi-LAT and extends to multi-TeV .. rst ever gamma-ray box constraints at TeV energies .. thermal x-sec probed for m ' 10 GeV few TeV future ACTs can probe boxes from thermal x-sec above 10 TeV, a region hardly accessible to direct, collider and other indirect searches miguel pato (tu munich) 4. results: constraints Region 3 (Fermi-LAT; Weniger '12) jl j < 0:8 , jb j < 0:3 (H.E.S.S. '06) ! aa ! 4 10 - 23 3 direct XΣv\ aa @cm sD 10 - 24 collider narrow box m a m Χ = 0.999 10 - 25 E. H. 10 - 26 S. S. 10 thermal 1 10 -1 AT -L mi 10 - 27 10 2 XΣv\ aa XΣv\ th target: r Fe 10 - 2 conservative aggressive 10 - 28 10 10 2 m Χ @GeVD 10 3 10 4 [Ibarra, Lee, Gehler, Park & MP '13] .. H.E.S.S. meets Fermi-LAT and extends to multi-TeV .. rst ever gamma-ray box constraints at TeV energies .. thermal x-sec probed for m ' 10 GeV few TeV future ACTs can probe boxes from thermal x-sec above 10 TeV, a region hardly accessible to direct, collider and other indirect searches miguel pato (tu munich) 4. results: constraints Region 3 (Fermi-LAT; Weniger '12) jl j < 0:8 , jb j < 0:3 (H.E.S.S. '06) ! aa ! 4 10 - 23 3 XΣv\ aa @cm sD 10 - 24 10 - 25 collider direct indirect narrow box m a m Χ = 0.999 E. H. 10 - 26 S. S. 10 thermal 1 10 -1 AT -L mi 10 - 27 10 2 XΣv\ aa XΣv\ th target: r Fe 10 - 2 conservative aggressive 10 - 28 10 10 2 m Χ @GeVD 10 3 10 4 [Ibarra, Lee, Gehler, Park & MP '13] .. H.E.S.S. meets Fermi-LAT and extends to multi-TeV .. rst ever gamma-ray box constraints at TeV energies .. thermal x-sec probed for m ' 10 GeV few TeV future ACTs can probe boxes from thermal x-sec above 10 TeV, a region hardly accessible to direct, collider and other indirect searches miguel pato (tu munich) 4. results: constraints Region 3 (Fermi-LAT; Weniger '12) jl j < 0:8 , jb j < 0:3 (H.E.S.S. '06) ! aa ! 4 10 - 23 3 XΣv\ aa @cm sD 10 - 24 10 - 25 collider direct indirect narrow box m a m Χ = 0.999 # E. H. 10 - 26 S. r Fe 10 thermal 1 cta 10 -1 " AT -L mi 10 - 27 S. 10 2 XΣv\ aa XΣv\ th target: ! 10 - 2 conservative aggressive 10 - 28 10 10 2 m Χ @GeVD 10 3 10 4 [Ibarra, Lee, Gehler, Park & MP '13] .. H.E.S.S. meets Fermi-LAT and extends to multi-TeV .. rst ever gamma-ray box constraints at TeV energies .. thermal x-sec probed for m ' 10 GeV few TeV future ACTs can probe boxes from thermal x-sec above 10 TeV, a region hardly accessible to direct, collider and other indirect searches miguel pato (tu munich) 4. results: constraints target: Region 3 (Fermi-LAT; Weniger '12) jl j < 0:8 , jb j < 0:3 (H.E.S.S. '06) ! aa 10 - 23 narrow box m a m Χ = 0.999 ! 4 10 - 23 10 2 10 - 24 wide box m a m Χ = 0.1 10 - 24 thermal 10 - 26 1 10 -1 AT L i- 3 10 - 25 10 - 2 E. H. 10 - 26 S. S. AT 10 2 m Χ @GeVD 10 3 10 4 1 10 -1 rm 10 - 27 10 - 2 conservative aggressive 10 - 28 10 thermal L i- Fe m r Fe XΣv\ aa XΣv\ th . .S S E. H. XΣv\ aa XΣv\ th 10 - 25 10 XΣv\ aa @cm sD 3 XΣv\ aa @cm sD 10 10 - 27 10 2 conservative aggressive 10 - 28 10 10 2 m Χ @GeVD 10 3 10 4 [Ibarra, Lee, Gehler, Park & MP '13] BR( ! aa ! 4 ) . 0:02 1 for m = O(10) GeV few TeV (wrt thermal) BR( ! aa ! 4 ) . 10 3 for m TeV (wrt PAMELA/AMS-02/Fermi-LAT) if the e excess is due to cascade annihilations, we should either see a gamma-ray box or else the decay to photons must be heavily suppressed miguel pato (tu munich) 4. results: constraints target: Region 3 (Fermi-LAT; Weniger '12) jl j < 0:8 , jb j < 0:3 (H.E.S.S. '06) ! aa ! 4 10 - 23 wide box m a m Χ = 0.1 10 2 10 - 24 XΣv\ aa XΣv\ th 3 XΣv\ aa @cm sD 10 10 - 25 E. H. 10 - 26 S. S. thermal AT 10 -1 L i- Fe 1 rm 10 - 27 10 - 2 conservative aggressive 10 - 28 10 10 2 m Χ @GeVD 10 3 10 4 [Ibarra, Lee, Gehler, Park & MP '13] BR( ! aa ! 4 ) . 0:02 1 for m = O(10) GeV few TeV (wrt thermal) BR( ! aa ! 4 ) . 10 2 for m TeV (wrt PAMELA/AMS-02/Fermi-LAT) if the e excess is due to cascade annihilations, we should either see a gamma-ray box or else the decay to photons must be heavily suppressed miguel pato (tu munich) 5. conclusions .. alternative feature with unique phenomenology .. strong constraints with present observations .. golden opportunity for CTA dNg/dEg gamma-ray boxes −2.x Eg E− miguel pato (tu munich) Ec E+ Eg 5. conclusions .. alternative feature with unique phenomenology .. strong constraints with present observations .. golden opportunity for CTA dNg/dEg gamma-ray boxes −2.x Eg E− the way forward in dark matter searches where? accurate description of dark matter distribution what? search for smoking guns how? interplay direct+indirect+collider searches miguel pato (tu munich) Ec E+ Eg 5. conclusions .. alternative feature with unique phenomenology .. strong constraints with present observations .. golden opportunity for CTA dNg/dEg gamma-ray boxes −2.x Eg E− the way forward in dark matter searches where? accurate description of dark matter distribution what? search for smoking guns how? interplay direct+indirect+collider searches { fully explore all available data { miguel pato (tu munich) Ec E+ Eg
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