Radio signals from galactic and extragalactic dark matter
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From this document you will learn the answers to the following questions:
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1 Radio signals from galactic and extragalactic dark matter Nicolao Fornengo Department of Theoretical Physics, University of Torino and Istituto Nazionale di Fisica Nucleare (INFN) Torino Italy Torino CETUP* 2012 Workshop Deadwood/Lead, SD (USA)
2 Astrophysical dark matter signals Direct detection Cosmic Antiprotons Electrons/Positrons Antideuterons Neutrinos from the Earth, Sun from the Milky Way Gamma rays galactic emission extragalactic emission Radio waves galactic emission extragalactic/cosmological emission Effects on the CMB recombination altered by early time particle injection from DM Sunyaev-Zeldovic effect in galaxy clusters
3 Radio signals from dark matter DM annihilation/decay into e+/e- produce radio signals by synchrotron emission in galactic/extragalactic magnetic fields Emission in the MHz-GHz frequency range occurs for: Electrons/positrons energies in the GeV-TeV range (*) Magnetic fields of the order of microg q E 15 GHz /B µg GeV (*) Relevant interval for WIMP DM in the GeV-TeV mass range More specifically: electron energies < 10 GeV produce signals at frequencies < GHz
4 Targets Galactic Center Good target for spiky DM profile On the scale of the bulge: WMAP haze? GC is avery active region: desentanglement of a signal rather complicated Galactic Halo Mid/high latitudes may be cleaner Low radio frequences for soft e+/e- spectra, microwave range otherwise Extragalactic diffuse emission ARCADE 2: isotropic radio emission significantly brighter than expected: requires a new population of unresolved sources which become the most numerous at very low (observationally unreached) brightness [maybe DM?] Anisotropies studies may be a goal for the future Extragalactic objects Non-thermal emission with spherical morphology correlated with the DM halo profile inferred from kinematic measurements in the external part of extragalactic objects can be a strong evidence for WIMP induced emission Most promising targets: dwarf spheroidal galaxies and clusters of galaxies
5 Based on: NF, Lineros, Regis, Taoso, Phys.Rev.Lett. 107 (2011) [arxiv: ] NF, Lineros, Regis, Taoso, JCAP 01(2012)005 [arxiv: ] NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
![0569] NF, Lineros, Regis, Taoso, JCAP 01(2012)005](/docs-images/41/22518170/images/page_5.jpg "[arxiv:1110.")
6 Galactic radio signal
7 Synchrotron emissivity Synchrotron flux: j (x) = Z de n e (E,x) dw d (x) Electron number density: n e (E,x) Emission power: dw d (,B?)= p 3 e 3 B? m e c 2 F c,? B? : perp component of B ~ c,? = 3eB?E 2 4 m 3 ec 5 F (x) =x Z 1 x d K 5/3 ( )
8 Electron number density Source term q(x,e)= 1 2 (x) 2 ( v) M DM dn de (E) Electron/positron propagation K 0 E b(e) = q(x,e) Diffusion: L z [kpc] K 0 kpc 2 /Myr MIN MED MAX Energy losses: b(e) =b ISRF (E)+b synch (E,B) b ISRF (E) : Compton scattering on ISRF b synch (E,B)= 4e4 B 2 9m 4 c 7 E2 disk diffusive halo dark matter halo R g Lz
9 Magnetic field r r B(r, z) =B 0 exp R m z L m GMF Model Parameters L m [kpc] R m [kpc] I L z R g II L z R g III 1 R g IV constant
![Parameters L m [kpc] R m [kpc] I](/docs-images/41/22518170/images/page_9.jpg "L z R g II L z R g III 1 R g IV")
10 Morphology of radio sky at 45 MHz observed NFW MED propag params NFW MIN propag params NF, Lineros, Regis, Taoso, JCAP 01 (2012) 005 [arxiv: ] NFW MAX propag params 10 GeV DM Annihilation into muon with thermal cross section Exp decaying B(r,z) with B TOT = 10 microg
11 Sky temperature at the galactic poles NFW MED propag params B 0 = 6 µg GSM North pole GSM South pole Surveys North pole Surveys South pole Fornengo, Lineros, Regis, Taoso (2011) Exp decaying B(r,z) with B TOT = 10 microg T [K] (ν/mhz) MeV 1 GeV 3 GeV 10 GeV µ + µ channel bb channel M DM = 10 GeV M DM = 100 GeV log 10 (ν/mhz) NF, Lineros, Regis, Taoso, JCAP 01 (2012) 005 [arxiv: ]
![10 microg T [K] (ν/mhz) 2.](/docs-images/41/22518170/images/page_11.jpg "5 10 7 10 6 10 5 300 MeV 1 GeV 3 GeV 10 GeV 10 4 10 3 µ + µ channel bb channel M DM = 10 GeV M DM = 100 GeV 1")
12 Galactic radio signal Fornengo, Lineros, Regis, Taoso (2011) 45 MHz Data: l < 3 DM models: l = 0 T [K] (ν/mhz) M DM =10 GeV MED GMF model I 45 MHz µ + µ bb τ + τ e + e NFW Isothermal Galactic latitude [degrees] Fornengo, Lineros, Regis, Taoso (2011) 10 9 M DM =10 GeV µ + µ GMF model I 45 MHz MIN MED MAX NFW Isothermal T [K] (ν/mhz) Galactic latitude [degrees] NF, Lineros, Regis, Taoso, JCAP 01 (2012) 005 [arxiv: ]
![latitude [degrees] Fornengo, Lineros, Regis, Taoso (2011) 10 9 M DM =10 GeV µ + µ GMF model I 45 MHz MIN MED MAX NFW Isothermal T](/docs-images/41/22518170/images/page_12.jpg "[K] (ν/mhz) 2.")
13 Skymaps 22 MHz 45 MHz 408 MHz 820 MHz 1420 MHz NF, Lineros, Regis, Taoso, JCAP 01 (2012) 005 [arxiv: ]
14 Galactic radio signal: bounds Bounds from combination of all frequency-skymaps T DM apple T obs +3 σv [cm 3 /s] bb MIN MED MAX GMF model I NFW Isothermal hadronic channel (bb) Fornengo, Lineros, Regis, Taoso (2011) σv [cm 3 /s] Conservative bounds: - no astrophysical background subtraction - no DM substructures included [MHz] Survey rms noise [K] 22 DRAO Guzman et al Haslam et al Dwingeloo Stockert M DM [GeV] e + e GMF model I MIN MED MAX NFW Isothermal M DM [GeV] Bounds from all sky leptonic channel (ee) Fornengo, Lineros, Regis, Taoso (2011) Bounds from all sky NF, Lineros, Regis, Taoso, JCAP 01 (2012) 005 [arxiv: ]
15 Galactic radio signal: bounds Bounds from combination of all frequency-skymaps T DM apple T obs +3 σv [cm 3 /s] µ + µ GMF model I MIN MED MAX NFW Isothermal Fornengo, Lineros, Regis, Taoso (2011) M DM [GeV] Bounds from all sky Fornengo, Lineros, Regis, Taoso (2011) σv [cm 3 /s] µ + µ GMF model I Cut b >15 degrees MIN MED MAX NFW Isothermal Bounds excluding GC region M DM [GeV] NF, Lineros, Regis, Taoso, JCAP 01 (2012) 005 [arxiv: ]
![all sky Fornengo, Lineros, Regis, Taoso (2011) σv [cm 3 /s] 10 22 10 23 10 24 10 25 µ + µ GMF model I Cut b >15 degrees MIN MED MAX NFW](/docs-images/41/22518170/images/page_15.jpg "Isothermal 10 26 10 27 Bounds excluding GC region 10 28 10 0 10 1 10 2 10 3 M DM [GeV] NF, Lineros, Regis, Taoso, JCAP 01 (2012) 005")
16 Galactic radio signal: bounds [MHz] Survey rms noise [K] 22 DRAO Guzman et al Haslam et al Dwingeloo Stockert 0.02 Fornengo, Lineros, Regis, Taoso (2011) σv [cm 3 /s] Mhz 45 Mhz 408 Mhz 820 Mhz 1420 Mhz µ + µ NFW MED GMF model I All-sky bounds from individual frequencies M DM [GeV] NF, Lineros, Regis, Taoso, JCAP 01 (2012) 005 [arxiv: ]
![02 Fornengo, Lineros, Regis, Taoso (2011) σv [cm 3 /s] 10 21 10 22 10 23 10 24 10 25 10 26 22 Mhz 45 Mhz 408 Mhz](/docs-images/41/22518170/images/page_16.jpg "820 Mhz 1420 Mhz µ + µ NFW MED GMF model I 10 27 10 28 All-sky bounds from individual frequencies 10 0 10 1 10 2")
17 Cosmological radio signal
18 Radio observables Radio emission may occurr also in extragalactic halos Three relevant observables: Intensity of the emission Ø High frequency: CMB largely dominates Ø Close and below 1 GHz: CMB may be efficiently subtracted Ø Low frequencies: extra-galactic sources dominate Differential number counts of sources Ø Quite useful to study different radio populations Ø Dominated by radio-loud AGNs down to the mjy level Ø Star-forming galaxies and radio-quiet AGN take over at fainter fluxes Angular correlations Ø Angular distribution of sources is a powerful probe of LS clustering Ø Wide-area radio surveys allow to test large scales Ø 2-point correlation function and angular power spectrum
19 Key elements: Dark matter radio signals Halo mass function and concentration DM distribution in halos Cosmological evolution e+/e- propagation and energy losses Magnetic fields DM benchmarks Name Mass ( a v)[cm 3 s 1 ] [s] Dominant [GeV] annihilating case decaying case final state B b b B µ + µ
![Magnetic fields DM benchmarks Name Mass ( a v)[cm 3 s 1 ] [s] Dominant [GeV]](/docs-images/41/22518170/images/page_19.jpg "annihilating case decaying case final state B1 100 3 10 26 4 10 28 b b B2 10 3 10")
20 Total intensity 10 6 Radio 10-5 Gamma-rays 2 T [GHz 2 K] CMB Best-fit power-law of the excess decaying B1 decaying B2 annihilating B1 annihilating B2 AGN [GHz] SFG E 2 dn/de [GeV cm -2 s -1 sr -1 ] CHANDRA IC COMPTEL FERMI FSR E [GeV] 0 Radio is more constraining than gamma-rays for DM producing leptons For DM producing hadrons, contstraining power is similar NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
![10-6 10-7 10-8 10-9 10-10 CHANDRA IC COMPTEL FERMI FSR 10-11 10-6 10-5 10-4 10-3 10-2 10-1 10 0 10 1 10 2 E [GeV] 0 Radio is more constraining](/docs-images/41/22518170/images/page_20.jpg "than gamma-rays for DM producing leptons For DM producing hadrons, contstraining power is similar NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033")
21 Source number counts 10 5 Benchmark B c S 5/2 dn/ds [Jy 3/2 sr -1 ] MHz, c= GHz, c=1 4.8 GHz, c=0.1 AGN SFG DM Log( S[Jy] ) S 5/2 dn/ds [Jy 3/2 sr -1 ] GHz annihilating B1 annihilating B2 decaying B1 decaying B Log( S[Jy] ) DM constribution becomes more dominant for sub-microjy levels Decaying-DM spectrum steeper -> takes over at even smaller fluxes Annihilating DM(density) 2 + (growing of concentration at small halo masses): makes the smaller and fainter structures more important than brighter halos NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
22 Differential number counts DM ann DM dec Benchmark B2 Faint sources 0.1 µjy < S < 1 µjy dn/dz [deg -2 ] SFG S > 3 mjy 1.4 GHz AGN 10 0 DM ann DM dec Bright sources redshift z DM-induced radio emission is mostly produced at low-redshifts NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
23 Angular correlation l (l+1) C l /(2 ) GHz S < 1 µjy DM 1.4 GHz S > 10 mjy NVSS SFG Faint sources DM AGN Bright sources Multipole l Benchmark B2 l (l+1) C l /(2 ) [mk 2 ] l (l+1) C l /(2 ) [µk 2 ] MHz AGN+SFG DM ann 150 GHz DM ann from Haslam et al. map DM dec AGN+SFG All brightnesses SPT DM dec Multipole l Bright sources: 1-halo term dominates, follows Poisson noise; astro sources dominate Faint sources: 2-halo term dominates; DM dominates at low multipoles NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
24 Effect of clustering 10 3 Benchmark B GHz NFW, M cut =10 6 M sun 2 T [GHz 2 K] cvir1 cvir2 M cut =10 6 M sun NFW Burkert Moore M cut =10-6 M sun S 5/2 dn/ds [Jy 3/2 sr -1 ] NFW, M cut =10-6 M sun Burkert, M cut =10 6 M sun Moore, M cut =10-6 M sun [GHz] Log( S[Jy] ) Main uncertainty comes from extrapolation al low masses Uncertainty in clustering (without considering here subcstructures) reaches 2 odm NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
25 Effect of clustering NFW, M cut =10 6 M sun Moore, M cut =10 6 M sun Benchmark B1 1.4 GHz S < 1 mjy l (l+1) C l / (2 ) Burkert, M cut =10 6 M sun NFW, M cut =10-6 M sun 1h-term 2h-term Multipole l NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
26 Effect of substructures 10 3 Benchmark B T [GHz 2 K] no subhalo s M cut =10 6 M sun s M cut =10-6 M sun [GHz] S 5/2 dn/ds [Jy 3/2 sr -1 ] GHz subhalos resolved subhalos unresolved no subhalo s M cut =10 6 M sun s M cut =10-6 M sun Log( S[Jy] ) NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
27 Effect of substructures l (l+1) C l / (2 ) [erg cm -2 s -1 sr -1 ] C l from host halo Benchmark B1 1.4 GHz s C l from subhalo (M cut =10 6 M sun, biased) s C l from subhalo (M cut =10-6 M sun, biased) C l from subhalo (M cut =10-6 M sun, anti-biased) S < 1 mjy 1h-term 2h-term Multipole l NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
28 2 T [GHz 2 K] (1) (2) B = B 0 = 10 µg B = B 0 ( M / M max ) 0.1, B 0 = 10 µg B = B 0 exp( -r / (R vir /50) ), B 0 = 10 µg B = B 0 = 1 µg [GHz] Effect of magnetic field Benchmark B2 NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ] Log( S[Jy] ) S 5/5 dn/ds [Jy 3/2 sr -1 ] GHz B = B 0 = 10 µg B = B 0 ( M / M max ) 0.1, B 0 = 10 µg B = B 0 exp( -r / (R vir /50) ), B 0 = 10 µg The bulk of the DM signal comes from low redshift: z-dep for B not critical Scaling with mass of objects may be more critical case (1): emission suppression is small objects -> depletion is number counts at small S case (2): emission suppression in large objects
29 Effect of magnetic field Benchmark B2 1.4 GHz 0.1 µjy < S < 1 µjy l (l+1) C l / (2 ) [erg cm -2 s -1 sr -1 ] h-term 2h-term B = B 0 = 10 µg B = B 0 ( M / M max ) 0.1, B 0 = 10 µg B = B 0 exp( -r / (R vir /50) ), B 0 = 10 µg Multipole l NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
30 Constraints on DM properties Annihilation rate v [cm 3 s -1 ] µ + µ Annihilating dark matter Intensity Counts Angular Annihilation rate v [cm 3 s -1 ] MAX MIN µ + µ b - b _ WIMP mass M [GeV] WIMP mass M [GeV] Future survey are expected to improve considerably the bounds from number counts and anisotropies NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
31 Constraints on DM properties MAX MIN Decaying dark matter Decay rate -1 [s -1 ] µ + µ b - b _ WIMP mass M [GeV] NF, Lineros, Regis, Taoso, JCAP 03 (2012) 033 [arxiv: ]
32 ARCADE excess After subtraction of an isotropic component, ARCADE reports a remaining flux (interpreted as extragalactic) 5 6 times larger than the total contribution from detected extragalactic radio sources ARCADE: Singal et al., Astrophys. J. 730 (2011) 138 A. Kogut et al., Astrophys. J. 734 (2011) 4 Extrapolating the source number counts to lower (unreached) brightness, the excess remains Systematics effects and galactic sources seems excluded Such a level of radio extragactic emission does not appear to have an immediate explanation in terms of standard astrophysical scenarios,, expecially when multiwavelength constraints are applied [GHz] T [K] CMB v= cm 3 /s, NFW B = 10 µg, b.f. sub =7 Sources contrib. from number counts µ + µ, M DM =10 GeV _ b - b, M DM =100 GeV, b.f.=20 Best-fit power-law of the excess NF, Lineros, Regis, Taoso, PRL 107 (2011) [arxiv: ] DM can easily explain the excess without special fine tunings (Slight) preference for light (around 10 GeV) and leptophilic DM Nicolao Fornengo, University of Torino and INFN-Torino (Italy) CETUP* Deadwood/Lead, SD
33 ARCADE excess Astrophysical galactic origin: appears to be rather unlikely Free free emission has been excluded based on the spectral shape Diffuse Galactic synchrotron foreground is estimated using two different methods (a cosecant dependence on Galactic latitude and the correlation between radio and atomic line emissions) A new population of numerous and faint radio sources (able to dominate source counts around μjy flux) has to be introduced Ordinary star forming galaxies with a radio to far infrared flux ratio which increases significantly with redshift can in principle offer a solution: this possibility is strongly constrained by multi wavelength observations The radio to far infrared emission has to be increased by a factor of 5 above what is observed in local galaxies, while current measurements show very mild evolution Radiative emission of secondary electrons in star forming galaxies would overproduce the gamma ray background from pion decays The same is true also for primary electrons unless such putative galaxies have extremely low gas density (and, in turn, low ratio of primary electrons to pions) or extremely efficient proton escape Nicolao Fornengo, University of Torino and INFN-Torino (Italy) CETUP* Deadwood/Lead, SD
34 ARCADE excess corresponding multiwavelength signals COMPTEL 10 4 differential number counts 1.4 GHz 10-6 CHANDRA FERMI 10 3 E 2 dn/de [GeV cm -2 s -1 sr -1 ] IC 0 FSR S 5/2 dn/ds [Jy 3/2 sr -1 ] unresolved substructures resolved substructures E [GeV] 10-1 AGN GAL DM Log( S[Jy] ) NF, Lineros, Regis, Taoso, PRL 107 (2011) 27 [arxiv: ] See also: Hooper et al., arxiv: Nicolao Fornengo, University of Torino and INFN-Torino (Italy) CETUP* Deadwood/Lead, SD
35 Conclusions Radio emission in the MHz-GHz frequency range may be produced by DM annihilation/decay in our Galaxy or in the extragalactic environment Radio signals already pose bounds on WIMP DM comparable to other indirect detection searches: Galactic radio emission close to thermal annihilation for light DM Low-frequency surveys quite competivitve for light DM Potential channels of discovery (but require increased sensitivities): Source number counts at low brightnesses (below microjy) Angular correlations at low multipoles and low brightnesses Various sources of uncertainty are present: DM matter distribution (in the Galaxy / cosmological) Electron/positron propagation and energy losses Magnetic fields (galactic / extragalactic) Promising future with the development of many new, high-sensitivty detectors: ASKAP, EVLA, MeerKAT, LOFAR, SKA Nicolao Fornengo, University of Torino and INFN-Torino (Italy) CETUP* Deadwood/Lead, SD
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