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Astrophysical Signatures of Axino Dark Matter

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Astrophysical Signatures of Axino Dark Matter Astrophysical signatures of Axino dark matter Seng Pei Liew (U. of Tokyo) Phys. Lett. B 721 (2013) , pp. 111; (based on...) arXiv: 1301.7536 JCAP 1405 (2014) 044; arXiv: 1403.6621 SUSY 2014, Manchester Axion as a solution of the Strong CP problem from non-perturbative effects but from experiments (fine-tuning problem) Introduce a new field a such that at the minimum of the potential, 2 for U(1) and SU(2) gauge couplings supersymmetrize axino bino wino appears in both KSVZ and DFSZ models 3 Axino can be a DM candidate L. Roszkowski,(mass: Particle Dark keV~TeV) Matter [hep-ph/0404052] Figure 1. Aschematicrepresentationofsomewell–motivatedWIMP–type particles 4 for which a priori one can have ω ∼ 1. σint represents a typical order of magnitude of interaction strength with ordinary matter. The neutrino provides hot DM which is disfavored. The box marked “WIMP’ stands for several possible candidates, e.g.,from Kaluza–Klein scenarios. can in principle extend up to the Planck mass scale, but not above, if we are talking about elementary particles. The interaction cross section could reasonably be expected to be of −38 2 −2 the electroweak strength (σEW 10 cm =10 pb) but could also be as tiny as that ∼ 2 −32 −34 purely due to gravity: (mW /MP) σEW 10 σEW 10 pb. What can we put into∼ this vast plane shown∼ in Fig. 1?∼ One obviouscandidateisthe neutrino, since we know that it exists. Neutrino oscillationexperimentshavebasically convinced us that its mass of at least 0.1 eV. On the upper side, if it were heavier than afeweV,itwouldoverclosetheUniverse.Theproblemofcour∼ se is that such a WIMP would constitute hot DM which is hardly anybody’s favored these days. While some like it hot, or warm, most like it cold. Cold, or non–relativistic at the epoch of matter dominance (although not necessarily at freezeout!) and later, DM particles are strongly favored by afewindependentarguments. One is numerical simulations of large structures. Also, increasingly accurate studies of CMB anisotropies, most notably recent results from WMAP [1],implyalargecoldDM (CDM) component and strongly suggest that most ( 90%)ofitisnon–baryonic. In the SUSY world, of course we could add a sneutrino∼ ν,which,likeneutrinos,interacts > weakly. From LEP its mass 70 GeV (definitely a cold DM! candidate), but then Ων 1. Uninteresting and ν does not∼ appear in Fig. 1. " ! The main suspect! for today is of course the neutralino χ.Unfortunately,westillknow little about its properties. LEP bounds on its mass are actually not too strong, nor are they robust: they depend on a number of assumptions. In minimal SUSY (the so-called MSSM) 2 130 GeV γ-line Studies on γ-rays from the Fermi data T. Bringmann, X. Huang, A. Ibarra, S. Vogl, C. Weniger [arXiv:1203.1312] C. Weniger [arXiv:1204.2797] E. Tempel, A. Hektor and M. Raidal [arXiv:1205.1045] and many more... See T. Bringmann, C. Weniger [arXiv:1208.5481] for a review From the Galactic Center, they found C. Weniger [arXiv:1204.2797] E. Tempel, A. Hektor and M. Raidal [arXiv:1205.1045] A DM signal? • Less significant feature from the Fermi Collaboration • γ-lines from the Earth limb? • Instrumental? Still inclonclusive... Summary & Updates: C. Weniger [arXiv:1303.1798] From A. Albert’s talk, the Fermi Symposium Nov. 2012 Neutralino • Annihilating DM DM γ DM 130 GeV Neutralino • γ from loop effects γ DM DM 130 GeV W boson etc. Neutralino • γ from loop effects Typically... γ DM DM SM << DM DM 130 GeV W boson etc. SM Neutralino • γ from loop effects Typically... γ DM DM SM << DM DM 130 GeV W boson etc. SM Too much continuum γ & antiprotons! Gravitino F. Takayama, M. Yamaguchi [hep-ph/0005214] Decaying DM • Small bilinear R-parity violation 28 • Long lifetime Lifetime ~ 10 sec W. Buchmuller, M. Garny [arXiv:1206.7056] γ W, Z, h Gravitino << 260 GeV ν l, ν Too much continuum γ & antiprotons! Axino Small bilinear R-parity violation • Decaying DM • Long lifetime γ W, Z Axino ~ 260 GeV Branching ratio largeν enough tol, ν explain the 130-GeV γ-line! M. Endo, K. Hamaguchi, SPL, K. Mukaida, K. Results Nakayama [arXiv:1301.7536] PQ Scale (Wino NLSP, similar for Bino NLSP) RPV parameter 13 From Ruchayskiy’s talk Unidentified spectral line at E 3.5 keV Unidentified spectral line at E⇠ 3.5 keV ⇠ [1402.4119] Boyarsky et al. 2014 [1402.4119] M31 galaxy XMM-Newton,Boyarsky center et al. 2014 & outskirts PerseusM31 cluster galaxy XMM-Newton, XMM-Newton, outskirts center & only outskirts PerseusBlank cluster sky XMM-Newton XMM-Newton, outskirts only Blank sky XMM-Newton [1402.2301] [1402.2301] Bulbul et al. 2014 73 clusters XMM-Newton,Bulbul et central al. 2014 regions 73 clusters XMM-Newton, central regions of clusters only. Up to z =0.35, of clusters only. Up to z =0.35, including Coma, Perseus including Coma, Perseus Perseus cluster Chandra, center only Perseus cluster Chandra, center only VirgoVirgo cluster cluster Chandra, Chandra, center center only only Position:Position:3.53.5 keV. keV. Statistical Statistical error error for for line line position position 3030 eV.eV. ⇠⇠ SystematicsSystematics ( (50 50eVeV – between – between cameras, cameras, determination determination of of known known ⇠ ⇠ instrumentalinstrumental lines) lines) 28 Lifetime:Lifetime: 10 10sec28 sec (uncertainty (uncertainty(10)(10)) ) ⇠ ⇠ O O OlegOleg Ruchayskiy Ruchayskiy HNL HNLIN COSMOLOGYIN COSMOLOGY 1717 Stacked X-ray spectrum [1402.2301] 14 ) ) -1 -1 0.8 XMM - MOS 3.51 ± 0.03 (0.05) XMM - PN 3.57 ± 0.02 (0.03) keV keV 1.2 Full Sample -1 -1 Full Sample 0.7 6 Ms 2 Ms 1 0.6 Flux (cnts s Flux (cnts s 0.8 0.015 0.04 0.01 0.02 0.005 0 0 Residuals Residuals -0.005 -0.02 3 3.2 3.4 3.6 3.8 4 3 3.2 3.4 3.6 3.8 4 Energy (keV) Energy (keV) ) ) -1 -1 XMM - MOS XMM - MOS Centaurus+ keV Rest of the Sample keV 3.57 keV 3.57 keV -1 -1 Coma + (69 Clusters) Ophiuchus 4.9 Ms All spectra are525.3 ks blue-shifted0.25 to the Flux (cnts s Flux (cnts s same frame of reference and 0.01 backgrounds are similarly0.005 subtracted 0 Residuals Residuals -0.005 3 3.2 3.4 3.6 3.8 4 Energy (keV) ) -1 0.75 XMM - PN 3.57 keV Rest of the Sample keV -1 (69 Clusters) 1.8 Ms 0.5 Flux (cnts s 0.02 0 Residuals -0.02 3 3.2 3.4 3.6 3.8 4 Energy (keV) Figure 6. 3 4keVbandoftherebinnedXMM-Newton spectra of the detections.The spectra were rebinned to make the excess at 3.57 keV more apparent.− (APJ VERSION INCLUDES ONLY THE REBINNED MOS SPECTRUM OF THE FULL SAMPLE).⇠ nax dwarf galaxies (Boyarsky et al. 2010; Watson et al. at a 1σ level. Since the most confident measurements 2012), as showin in Figure 13(a). It is in marginal ( 90% are provided by the highest signal-to-noise ratio stacked significance) tension with the most recent Chandra⇠limit MOS observations of the full sample, we will use the flux from M31 (Horiuchi et al. 2014), as shown in Figure at energy 3.57 keV when comparing the mixing angle 13(b). measurements for the sterile neutrino interpretation of For the PN flux for the line fixed at the best-fit MOS this line. energy, the corresponding mixing angle is sin2(2✓)= +1.2 +1.8 11 4.3 1.0 ( 1.7) 10− . This measurement is consistent with− that− obtained⇥ from the stacked MOS observations 3.2. Excluding Bright Nearby Clusters from the Sample Surface brightness profile 4 M31 surface brightness profile Perseus cluster surface brigtness profile 10 20 on-center NFW DM line, rs = 360 kpc off-center upper limit NFW DM line, rs = 872 kpc NFW, c = 11.7 β-model, β = 0.71, rc = 287 kpc NFW, c = 19 8 15 /sec] /sec] 2 2 Decaying DM 6 density profile 10 R200 [cts/cm [cts/cm 6 6 4 5 Flux x 10 Flux x 10 2 0 0 0 0.2 0.4 0.6 0.8 1 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2 Radius [deg] Radius [deg] FIG. 2: The line’s brightness profile in M31 (left) and the Perseus clusterisothermal (right). An beta NFW DMprofile distribution (gas distribution) is assumed, the scale rs is fixed to its best-fit values from [22] (M31) or [23] (Perseus) and the overall normalization is adjusted to pass through the left-most point. Blank sky dataset 0.10 For the Perseus cluster the observations can be grouped in 3radialbinsbytheiroff-centerangle.Foreachbinwefix the line position to its average value across Perseus (3.47 ± [cts/sec/keV] 0.07 keV). The obtained line fluxes together with 1σ errors Normalized count rate -3 are shown in Fig. 2. For comparison, we draw the expected 2⋅10 -3 line distribution from dark matter decay using the NFW pro- 2⋅10 -3 1⋅10 file of [23] (best fit value rs =360kpc, black solid line; 1σ -4 5⋅10 0 upper bound rs =872kpc, black dashed line). The isother- 0⋅10 -4 mal β-profile from [26] is shown in magenta. The surface -5⋅10 [cts/sec/keV] -3 Data - model -1⋅10 brightness profile follows the expected DM decay line’s dis- -3 -2⋅10 -3 tribution in Perseus. -2⋅10 2.0 3.0 4.0 5.0 6.0 7.0 8.0 Finally, we compare the predictions for the DM lifetime from Energy [keV] the two objects.
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