Constraints on decaying dark matter from<i>XMMNewton</i>observations of M31

Boyarsky, Alexey; Iakubovskyi, Dmytro; Ruchayskiy, Oleg; Savchenko, V.

doi:10.1111/j.1365-2966.2008.13266.x

Cited by 140 publications

(185 citation statements)

References 114 publications

(220 reference statements)

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“…Above/below the dashed black lines the sterile neutrinos will be over/under produced relative to the observed dark matter density (Laine & Shaposhnikov 2008;Canetti et al 2013b). The grey shaded regions are X-ray exclusion lines from XMM-Newton and Chandra observations (Boyarsky et al 2008a(Boyarsky et al , 2006aRiemer-Sørensen & Hansen 2009) with the Boyarsky et al (2008a) constraints rescaled by a factor of two due to mass estimate uncertainties as recommended in Boyarsky et al (2009b). The cyan and purple regions are the parameter space ruled out by the present Sgr* analysis assuming an NFW profile for the Milky Way halo.…”

Section: Constraints On Sterile Neutrinosmentioning

confidence: 99%

“…The two free parameters of mass, m s , and mixing angle with the active neutrinos, sin 2 (2θ), are unconstrained from particle physics, but as seen in Fig. 7 various observations have already excluded large parts of this parameter space (Laine & Shaposhnikov 2008;Canetti et al 2013b;Boyarsky et al 2008a;Riemer-Sørensen & Hansen 2009;Boyarsky et al 2006a;Horiuchi et al 2014). …”

Section: Annihilation-like Dark Mattermentioning

confidence: 99%

“…In Fig. 7 we show a selection of the strongest robust constraints (Boyarsky et al 2008a;Riemer-Sørensen & Hansen 2009;Horiuchi et al 2014). Some analyses have claimed stronger constraints, but were later found to be too optimistic (Abazajian & Koushiappas 2006;Boyarsky et al 2006bBoyarsky et al , 2008bAbazajian et al 2001b;Watson et al 2006Watson et al , 2012Yüksel et al 2008).…”

Section: Constraints On Sterile Neutrinosmentioning

confidence: 99%

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Constraints on the presence of a 3.5 keV dark matter emission line fromChandraobservations of the Galactic centre

Riemer-Sørensen

2016

A&A

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Context. Recent findings of line emission at 3.5 keV in both individual and stacked X-ray spectra of galaxy clusters have been speculated to have dark matter origin. Aims. If the origin is indeed dark matter, the emission line is expected to be detectable from the Milky Way dark matter halo. Methods. We perform a line search in public Chandra X-ray observations of the region near Sgr A*. We derive upper limits on the line emission flux for the 2.0−9.0 keV energy interval and discuss their potential physical interpretations including various scenarios of decaying and annihilating dark matter. Results. While we find no clear evidence for its presence, the upper flux limits are not inconsistent with the recent detections for conservative mass profiles of the Milky Way. Conclusions. The results depend mildly on the spectral modelling, and strongly on the choice of dark matter profile.

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Section: Constraints On Sterile Neutrinosmentioning

confidence: 99%

Section: Annihilation-like Dark Mattermentioning

confidence: 99%

Section: Constraints On Sterile Neutrinosmentioning

confidence: 99%

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Constraints on the presence of a 3.5 keV dark matter emission line fromChandraobservations of the Galactic centre

Riemer-Sørensen

2016

A&A

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“…Figure 3. Upper limit on the decay rate from NGC3227 (red), the Milky Way halo observed with a prototype cryogenic spectrometer (salmon) [27], XMM observations of the Milky Way (sand) [35], Chandra observations of the Bullet Cluster [30] and M31 [36,37] (orange), HEAO-1 observations of the diffuse x-ray background (aquamarine) [25,26], INTEGRAL SPI line search in the Milky Way halo (blue) [38,39]. Filled regions are excluded.…”

Section: X-ray Versus Cmbmentioning

confidence: 99%

X-ray photons from late-decaying majoron dark matter

Bazzocchi

Lattanzi

Riemer-Sørensen

et al. 2008

J. Cosmol. Astropart. Phys.

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Abstract.An attractive way to generate neutrino masses as required to account for current neutrino oscillation data involves the spontaneous breaking of lepton number. The resulting majoron may pick up a mass due to gravity. If its mass lies in the kilovolt scale, the majoron can play the role of late-decaying Dark Matter (LDDM), decaying mainly to neutrinos. In general the majoron has also a sub-dominant decay to two photons leading to a mono-energetic emission line which can be used as a test of the LDDM scenario. We compare expected photon emission rates with observations in order to obtain model independent restrictions on the relevant parameters. We also illustrate the resulting sensitivities within an explicit seesaw realisation, where the majoron couples to photons due to the presence of a Higgs triplet.

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“…We present the results of the combined analysis of many XMM-Newton observations of two objects at different redshifts-the Perseus cluster (z ¼ 0.0179 [12]) and the Andromeda galaxy (M31, z ¼ −0.001), a Local Group member-together with a long exposure "blank sky" data set. (Each of the data sets used in previous decaying DM searches in M31 [13][14][15][16][17] had less statistics than we use. The nondetection of any signal in these works does not come in contradiction with our results.)…”

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confidence: 99%

X-Ray Line May Have Dark Matter Origin

Abazajian¹

2014

Physics

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We report a weak line at 3.52 AE 0.02 keV in x-ray spectra of the Andromeda galaxy and the Perseus galaxy cluster observed by the metal-oxide-silicon (MOS) and p-n (PN) CCD cameras of the XMMNewton telescope. This line is not known as an atomic line in the spectra of galaxies or clusters. It becomes stronger towards the centers of the objects; is stronger for Perseus than for M31; is absent in the spectrum of a deep "blank sky" data set. Although for each object it is hard to exclude that the feature is due to an instrumental effect or an atomic line, it is consistent with the behavior of a dark matter decay line. Future (non-)detections of this line in multiple objects may help to reveal its nature. DOI: 10.1103/PhysRevLett.113.251301 PACS numbers: 95.35.+d, 13.35.Hb, 14.60.St, 95.85.Nv The nature of dark matter (DM) is a question of crucial importance for both cosmology and for fundamental physics. As neutrinos-the only known particles that could be DM candidates-are too light to be consistent with various observations [1][2][3][4], it is widely anticipated that new particles should exist. Although many candidates have been put forward (see, e.g., Ref.[5]), little is known experimentally about the properties of DM particles: their masses, lifetimes, and interaction types remain largely unconstrained. A priori, a given DM candidate can possess a decay channel if its lifetime exceeds the age of the Universe. Therefore, the search for a DM decay signal provides an important test to constrain the properties of DM in a model-independent way. For fermionic particles, one should search above the Tremaine-Gunn limit [1] (≳300 eV). If the mass is below 2m e c 2 , such a fermion can decay to neutrinos and photons with energy E γ ¼ 1 2 m dm [6]. One can search for such particles in x rays [7,8] (see Ref.[9] for a review of previous searches). For each particular model, the particle's parameters are related by the requirement to provide the correct DM abundance. For example, for one very interesting DM candidate-the right-handed neutrino-this requirement restricts the mass range to 0.5-100 keV [9,10]. A large part of the available parameter space for sterile neutrinos is consistent with all astrophysical and cosmological bounds [11], and it is important to probe it further.The DM decay line is much narrower than the spectral resolution of the existing x-ray telescopes and, as previous searches have shown, should be rather weak. The x-ray spectra of astrophysical objects are crowded with weak atomic and instrumental lines, not all of which may be known. Therefore, even if the exposure of available observations continues to increase, it is hard to exclude an astrophysical or instrumental origin of any weak line found in the spectrum of an individual object. However, if the same feature is present in the spectra of many different objects, and its surface brightness and relative normalization between objects are consistent with the expected behavior of the DM signal, this can provide much more convincing evidence about it...

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Constraints on decaying dark matter fromXMMNewtonobservations of M31

Cited by 140 publications

References 114 publications

Constraints on the presence of a 3.5 keV dark matter emission line fromChandraobservations of the Galactic centre

Constraints on the presence of a 3.5 keV dark matter emission line fromChandraobservations of the Galactic centre

X-ray photons from late-decaying majoron dark matter

X-Ray Line May Have Dark Matter Origin

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