X-Ray Line Signal from Decaying Axino Warm Dark Matter

Physics Letters B 735 (2014) 92–94 Contents lists available at ScienceDirect Physics Letters B www.elsevier.com/locate/physletb X-ray line signal from decaying axino warm dark matter ∗ Ki-Young Choi a, , Osamu Seto b a Korea Astronomy and Space Science Institute, Daejon 305-348, Republic of Korea b Department of Life Science and Technology, Hokkai-Gakuen University, Sapporo 062-8605, Japan a r t i c l e i n f o a b s t r a c t Article history: We consider axino warm dark matter in a supersymmetric axion model with R-parity violation. In this Received 11 March 2014 scenario, axino with the mass ma˜ 7keVcan decay into photon and neutrino resulting in the X-ray line Received in revised form 14 May 2014 signal at 3.5 keV, which might be the origin of unidentified X-ray emissions from galaxy clusters and Accepted 3 June 2014 Andromeda galaxy detected by the XMM-Newton X-ray observatory. Available online 6 June 2014 © 2014 The Authors. Published by Elsevier B.V. This is an open access article under the CC BY license Editor: A. Ringwald 3 (http://creativecommons.org/licenses/by/3.0/). Funded by SCOAP . 1. Introduction In Section 2 we introduce the model of axino dark matter and in Section 3 we consider the R-parity violation and decay of axinos. Various astrophysical and cosmological observations provide We summarize in Section 4. convincing evidences for the existence of dark matter (DM). Dark matter distribution spans in wide range of scales from galaxy to 2. Axino dark matter clusters of galaxies and the large scale structure of the Universe. Recently, anomalous X-ray line emissions have been observed The strong CP problem and the hierarchy problem in the Stan- from galaxy clusters and also in the Andromeda galaxy [1,2]. While dard Model can be naturally solved in the supersymmeric axion those might be a result of systematic effects, it would be interest- model [12,13]. If axino, the fermionic superpartner of axion, is the ing if the line came from the new source of astrophysical phenom- lightest supersymmetric particle (LSP), then it is a good candidate ena or from new physics. It was suggested that the signal might of dark matter [14–18]. The effective operator of the axino can be come from decaying dark matter with the mass and lifetime, derived by the supersymmetric transformation of the axion inter- actions and is given by mDM 7keV, α × 27 × 28 Leff = s ˜ μ ν ˜ b b τDM 2 10 –2 10 sec, (1) a˜ i aγ5 γ , γ G Gμν 16π fa assuming the they are the dominant component of dark mat- αY CaY Y ˜ μ ν ˜ ter. Some theoretically interesting particle models have been sug- + i aγ5 γ , γ YYμν, (2) 16π f gested such as sterile neutrino [1–4], exciting dark matter [5], a millicharged dark matter [6,7], axion like particle [8–10], in the ˜ where fa is the Peccei–Quinn breaking scale, and αs, G, Gμν and effective theory [11]. ˜ αY , Y , Yμν are the gauge couplings, gaugino fields and the field In this paper, we study the warm dark matter axino in a strength for SU(3)c and U (1)Y gauge groups respectively. The R-parity violating supersymmetric model. With bilinear R-parity mass of axino is expected to be of the order of gravitino mass, breakings, neutralinos mix with neutrinos and thus the axino can but it can be much smaller [19–24], or much larger [25] than the decay into photon and neutrino. We find that the axino mass with typical supersymmetric particle mass scale, depending on the spe- 7keVcan have the proper lifetime and relic density for the X-ray cific models [26]. Here we take the light axino mass of the order line emission. In this scenario, as an interesting consequence, the of keV as dark matter component. upper bound on the neutrino mass imposes that the Bino mass is The primordial axinos are generated from the thermal plasma lighter than about 10 GeV. during reheating after the primordial inflation. If the reheating temperature is lower than the decoupling temperature [14] * Corresponding author. 2 3 E-mail addresses: kiyoungchoi@kasi.re.kr (K.-Y. Choi), seto@physics.umn.edu fa 0.1 T = 1011 GeV , (3) (O. Seto). dec 12 10 GeV αs http://dx.doi.org/10.1016/j.physletb.2014.06.008 0370-2693/© 2014 The Authors. Published by Elsevier B.V. This is an open access article under the CC BY license (http://creativecommons.org/licenses/by/3.0/). Funded by SCOAP3. K.-Y. Choi, O. Seto / Physics Letters B 735 (2014) 92–94 93 the axinos cannot reach the thermal equilibrium. Then axinos are generated through scatterings and decay of heavy particles in the thermal plasma, and the amount could be abundant enough for axino to be the dominant dark matter component [15–17]. The abundance of thermally produced axinos depends on the reheating temperature for the KSVZ axion model [27].1 The axino number density to entropy density ratio is estimated as [16,17,32,33] 11 2 −5 6 1.108 10 GeV TR Y ˜ = 2.0 × 10 g log . (4) a s 6 gs fa 10 GeV With this, the relic density of non-relativistic axino at present is −5 −4 −3 Fig. 1. The reheating temperature TR versus fa for given ξi = 10 , 10 , 10 given by (Blue, Red, Green) respectively to explain X-ray line emission. The small value of 8 fa < 5 × 10 GeV (cyan) is disallowed by the SN1987A. On the curved black line 2 ma˜ Ya˜ the thermally produced axino and non-thermally produced axion (misalignment) Ω˜h = 0.28 . (5) a 10 keV 10−4 can give correct relic density for dark matter. The upper region of the black line is disallowed due to the overabundance of axino and axion dark matter. (For interpre- We can find that O(1–10 keV) axino can be a natural candidate tation of the references to color in this figure legend, the reader is referred to the for warm dark matter when the reheating temperature is around web version of this article.) 6 7 11 10 –10 GeV and Peccei–Quinn scale fa = 10 GeV. Such thermally produced keV axino is a warm dark matter candidate2 and be erased in the early Universe by the B–L violating interac- may solve various problems at the small scale in cold dark mat- tions [42–44]. However if one of the lepton flavors of the R-parity ter model [35,36]. This range of reheating temperature is free from violating couplings is preserved and the slepton mixing is small the gravitino problem [37,38]. enough, the problem can be avoided [45]. Due to the R-parity violation, the stability of LSP is not guar- 3. R-parity violation and axino decay anteed anymore [46–48]. For bilinear R-parity breakings, the light axino decays dominantly into photon and neutrino and the decay We consider the bilinear type R-parity violation with the usual rate is given by [49–51] μ-term superpotential in the minimal supersymmetric standard √ C 2 α2 m3 2˜ 2 model = = aY Y em a˜ | |2 νi Γa˜ Γa˜→γν U ˜ ˜ , (11) i 128π 3 f 2 γ Z v = i a i WR/ p iμLi Hu, (6) where the photino–Zino mixing is given by where Li and Hu are chiral super fields of the lepton doublet ∗ and up-type Higgs doublet and i parameterizes the size of the S Z˜ α Sγα˜ R-parity violation. By redefining the L and H , we can eliminate = i d Uγ˜ Z˜ M Z , (12) m ˜ the R-parity violating term in Eq. (6), then R-parity violating effect α χα appears only in the scalar potential [39,40], with the neutralino mixing matrix S. In the case of M1 M2, μ, ∗ V = m2 L˜ H + B L˜ H + h.c., (7) it is simplified to be R/ p Li Hd i d i i u 2 2 3 − 2 2 − 2 C α m˜ where the coefficients are Bi Bi and mL H (m˜ mH )i . aY Y em a 2 i d Li d Γa˜ ξ . (13) 128π 3 f 2 i From this scalar potential, the sneutrinos obtain non-zero vacuum a i expectation values (VEVs) Although axino can also decay to three neutrinos mediated by Z- 2 + mL H cos β Bi sin β boson, this mode is highly suppressed and negligible. ν˜ =− i d v, (8) i 2 The X-ray emission line observed by the XMM-Newton can be m ˜ νi explained with an appropriate lifetime and the relic abundance of √ axinos, if those satisfy the relation where tan β ≡H /H and v ≡ H 2 +H 2/ 2 174 GeV u d u d and mν˜ is the sneutrino mass. Since the non-zero VEVs of sneutri- 2 i Ωa˜h nos induce mixings between leptons and gauginos, the neutrinos τ˜ = τDM , (14) a 0.1 mix with neutralinos and can obtain mass at the tree level as [40,41] where τDM is given in Eq. (1). We note here that, even though 2 2 2 2 2 2 the axinos are not the dominant component of dark matter, the μ M (M1 g + M2 g )/g ξ m 1 i i , (9) enhanced decay rate can compensate to adjust the observed flux ν 2 + 2 2 − 2 (g M1 g M2)v μ sin β cos β 2M1 M2μ of X-ray line.

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