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Constraints on the Parameters of Radiatively Decaying Dark Matter from the Dark Matter Halos of the Milky Way and Ursa Minor

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Constraints on the Parameters of Radiatively Decaying Dark Matter from the Dark Matter Halos of the Milky Way and Ursa Minor A&A 471, 51–57 (2007) Astronomy DOI: 10.1051/0004-6361:20066774 & c ESO 2007 Astrophysics Constraints on the parameters of radiatively decaying dark matter from the dark matter halos of the Milky Way and Ursa Minor A. Boyarsky1,2,3, J. Nevalainen4, and O. Ruchayskiy5,2 1 CERN, PH-TH, 1211 Geneve 23, Switzerland e-mail: [email protected] 2 École Polytechnique Fédérale de Lausanne, Institute of Theoretical Physics, FSB/ITP/LPPC, BSP 720, 1015 Lausanne, Switzerland 3 On leave of absence from Bogolyubov Institute of Theoretical Physics, Kyiv, Ukraine 4 Helsinki University Observatory, Finland e-mail: [email protected] 5 Institut des Hautes Études Scientifiques, 91440 Bures-sur-Yvette, France e-mail: [email protected] Received 20 November 2006 / Accepted 19 April 2007 ABSTRACT Aims. We improve the earlier restrictions on parameters of the warm dark matter (DM) in the form of a sterile neutrinos. Methods. The results were obtained from not observing the DM decay line in the X-ray spectrum of the Milky Way (using the recent XMM-Newton PN blank sky data). We also present a similar constraint coming from the recent XMM-Newton observation of Ursa Minor – dark, X-ray quiet dwarf spheroidal galaxy. Results. The new Milky way data improve on (by as much as the order of magnitude at masses ∼3.5 keV) existing constraints. Although the observation of Ursa Minor has relatively poor statistics, the constraints are comparable to those recently obtained using observations of the Large Magellanic Cloud or M 31. This confirms a recent proposal that dwarf satellites of the MW are very interesting candidates for the DM search and dedicated studies should be made to this purpose. Key words. Galaxy: halo – galaxies: individual: Ursa Minor – cosmology: dark matter – X-rays: galaxies 1. Introduction Secondly, warm DM with the mass of particle in keV range can ease the problem of the dark halo structures in comparison This past year has seen a lot of activity, devoted to search- with the cold dark matter scenario (Bode et al. 2001; Goerdt ing for the decay signals of the DM particle in X-ray et al. 2006). By determining the matter power spectrum from the spectra of various astrophysical objects (Boyarsky et al. Lyman-α forest data from SDSS Seljak et al. (2006) and Viel 2006a,b,c; Riemer-Sørensen et al. 2006a; Watson et al. 2006; et al. (2006) argue that the mass of the DM particles should be Riemer-Sørensen et al. 2006b, e.g). It was noticed long ago by in the range ∼>10 keV (∼>14 keV in the case of Seljak et al. 2006). Dodelson & Widrow (1994) that a right-handed neutrino with As this method gives direct bounds for the free-streaming length masses in the keV range presents a viable warm dark matter of the neutrinos, the bounds on the mass of the DM particle de- (WDM) candidate. Such a particle possesses a specific radia- pend on the momentum distribution function of the sterile neu- tive decay channel, so one can search for its decay line in the trinos and, therefore, on their production mechanism. The results X-ray spectra of astrophysical objects (Dolgov & Hansen 2002; quoted above are claimed for the simplest Dodelson-Widrow Abazajian et al. 2001b). model (1994). Recently, the interest in the sterile neutrino as a DM can- At the same time, studies of the Fornax dwarf spheroidal didate has been greatly revitalized. First, the discovery of neu- galaxy (Goerdt et al. 2006; Strigari et al. 2006) disagree with trino oscillations (see e.g. Strumia & Vissani 2006, for a re- the predictions of CDM models and suggest lower mass than view) strongly suggest the existence of right-handed neutrinos. in Seljak et al. (2006) and Viel et al. (2006) for the DM parti- Probably the easiest way to explain the data on oscillations is by cle Mdm ∼ 2 keV. This result agrees with the earlier studies of adding several right-handed, or sterile, neutrinos, to the Standard Hansen et al. (2002) and Viel et al. (2005), which used a different Model. It has been demonstrated recently in Asaka et al. (2005) dataset. For other interesting applications of the sterile neutrinos and Asaka & Shaposhnikov (2005) that a simple extension of the with the mass ∼few keV see e.g. Kusenko (2006b), Biermann & Standard Model by three singlet fermions with masses smaller ν Kusenko (2006), Stasielak et al. (2006), Kusenko (2006a), and than the electroweak scale (dubbed the MSM in Asaka et al. Hidaka & Fuller (2006). 2005) allows accommodation of the data on neutrino masses and mixings, allows baryon asymmetry of the Universe to be to account for it by introducing a sterile neutrino with the mass around explained, and provides a candidate for the dark matter particle 1 eV. There are also models that explain not all, but only some of these in the form of the lightest of the sterile neutrinos1. phenomena (e.g. LSND and DM, but not the baryon asymmetry as e.g. in de Gouvea 2005) We do not give any review here. We would like to 1 The νMSM does not explain the unconfirmed results of the stress that, although our work is motivated by the recent results on the LSND experiment (Aguilar et al. 2001). There are other models that try νMSM, our method and results do not rely on any particular model. Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20066774 52 A. Boyarsky et al.: Dark matter constraints from the Galaxy and Ursa Minor It has been argued in Boyarsky et al. (2006c) and In the absence of a clearly detectable line, one can put an upper Riemer-Sørensen et al. (2006a) that the preferred targets for ob- limit on the flux of DM from the astrophysical data, which will servations are objects from the local halo, including our own lead via Eq. (4) to the restrictions of parameters of the sterile Milky Way and its satellites. In particular, Boyarsky et al. neutrino Ms and θ. (2006c) showed that the best observational targets are the dwarf spheroidals (Ursa Minor, Draco, etc.). Indeed, these objects are X-ray quiet, while at the same time one expects the DM decay 3. Restrictions from the blank sky observation signal from them, comparable to what comes from galaxy clus- 3.1. Modeling the DM halo of the MW ters. Because at the time of writing of Boyarsky et al. (2006c) no public data were available for these dwarf spheroidals, the obser- As shown in the previous section, one needs to know the distri- vations of the core of Large Magellanic Cloud (LMC) were used bution of the DM to obtain the restrictions on parameters of the to produce the strongest restrictions on parameters of the ster- sterile neutrino. In the case of nearby objects (including our own ile neutrino. It was stressed in Boyarsky et al. (2006c) that other Galaxy and dwarf satellites from the local halo), the DM dis- dwarf satellite galaxies should be studied as well, in order to tribution can be deduced e.g. by using the rotation curves of the minimize uncertainties related to the DM modeling in each sin- stars in the galaxy. Here we follow the analysis of Boyarsky et al. gle object. In this paper we continue studies of the dwarf satel- (2006c). Various DM profiles, used to fit observed velocity dis- lites of the MW by analyzing the data from XMM-Newton obser- tributions, differ the most in the center of a distribution. In the vation of Ursa Minor and confirm the restrictions of Boyarsky case of the MW we choose, as in Boyarsky et al. (2006c), to et al. (2006c). use the observations away from the center, to minimize this un- It was also shown in Boyarsky et al. (2006c) that the im- certainty. In particular, in references Klypin et al. (2002) and provement of the results from MW DM halo can be achieved Battaglia et al. (2005) it was shown that the DM halo of the by using longer exposure data (notably, longer exposure of the MW can be described by the Navarro-Frenk-White (NFW) pro- closed filter observations). In this paper, we improve our restric- file (Navarro et al. 1997) tions, coming from the MW DM halo by using the blank sky ρ r3 dataset with better statistics from Nevalainen et al. (2005). ρnfw = s s , (r) 2 (5) r(r + rs) 2. DM with radiative decay channel with parameters, given in Table 13. The relation between virial parameters and ρs, rs are given in the Appendix A. Quoted halo Although throughout this paper we are talking mostly about the parameters provide DM decay flux (from the directions with sterile neutrino DM, the results can be applied to any DM par- φ>90◦) consistent within ∼5% with the one, given by Eqs. (6), ticle that possesses the monoenergetic radiative decay channel, Γ (7). Only “maximal disk” models in Klypin et al. (2002) would emits photon of energy Eγ and has a decay width . In the case provide 30−50% weaker restrictions; however, these models are of the sterile neutrino (with mass below that of an electron), the highly implausible, see Klypin et al. (2002). Similarly, taking radiative decay channel is into a photon and active neutrino Pal the lower limit for the virial mass of Battaglia et al. (2005), one & Wolfenstein (1982). As the mass of an active neutrino is much M would obtain 25% weaker restrictions than the ones, presented Eγ = s Γ 4 lower than keV, 2 in this case.
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