Constraining sterile neutrino warm dark matter with<i>Chandra</i>observations of the Andromeda galaxy

Watson, Casey; Li, Zhiyuan; Polley, Nicholas

doi:10.1088/1475-7516/2012/03/018

Cited by 93 publications

(142 citation statements)

References 157 publications

(302 reference statements)

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“…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). The higher energy range of 3−48 keV has been constrained from the diffuse X-ray background observed with the High Energy Astronomy Observatory (HEAO; Boyarsky et al 2006a) and the 3−80 keV with NuSTAR (Riemer-Sørensen et al 2015).…”

Section: Constraints On Sterile Neutrinosmentioning

confidence: 88%

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: 88%

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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“…These limits are independent of the production mechanism of sterile neutrinos. For m χ 10 keV, strong constraints have been obtained using Chandra, Suzaku, and XMM-Newton [70,[79][80][81][82][83][84][85][86][87][88][89][90][91][92][93][94][95]. For m χ 50 keV, strong constraints have been obtained using INTEGRAL [96,97], completely ruling out mixingproduced sterile neutrinos as the sole dark matter constituent.…”

Section: B Summary Of Prior Constraints On Sterile Neutrino Dark Mattermentioning

confidence: 99%

Almost closing the νMSM sterile neutrino dark matter window with NuSTAR

Perez¹,

Ng²,

Beacom³

et al. 2017

Phys. Rev. D

149

260

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We use NuSTAR observations of the Galactic Center to search for X-ray lines from the radiative decay of sterile neutrino dark matter. Finding no evidence of unknown lines, we set limits on the sterile neutrino mass and mixing angle. In most of the mass range 10-50 keV, these are now the strongest limits, at some masses improving upon previous limits by a factor of ∼ 10. In the νMSM framework, where additional constraints from dark matter production and structure formation apply, the allowed parameter space is reduced by more than half. Future NuSTAR observations may be able to cover much of the remaining parameter space. P r e v io u s X -r a y c o n s t r a in t s M W s a t e ll it e c o u n t s a n d p h a s e s p a c e c o n s t r a in t sNuSTAR GC 2016 FIG. 1. Simplified overview of constraints on νMSM sterile neutrino dark matter in the plane of mass and mixing angle; details are described in Sec. IV, and the experimental constraints included are listed in Fig. 8. For parameters between the gray regions, the observed dark matter abundance can be produced through resonant production in the νMSM. Most of this region is ruled out by constraints from structure formation (blue) or astrophysical X-ray observations (green). Our new constraint (red line and hatched region) is obtained from NuSTAR observations of the GC, and rules out about half of the previously allowed parameter space (white region).

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“…In addition, one needs to explain the active-sterile mixing θ i4 . Depending on the case, this mixing would either need to be sizable, of θ i4 ∼ O(0.1), for eV-sterile neutrinos [11,12] or it should be really tiny, at most of θ i4 ∼ O(10 −4 ), for keV-sterile neutrinos [31][32][33][34][35][36][37][38][39][40][41][42][43].…”

Section: Jhep07(2014)039mentioning

confidence: 99%

Common origin of reactor and sterile neutrino mixing

Merle

Morisi

Winter

2014

J. High Energ. Phys.

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If the hints for light sterile neutrinos from short-baseline anomalies are to be taken seriously, global fits indicate active-sterile mixings of a magnitude comparable to the known reactor mixing. We therefore study the conditions under which the active-sterile and reactor mixings could have the same origin in an underlying flavour model. As a starting point, we use µ − τ symmetry in the active neutrino sector, which (for three neutrinos) yields a zero reactor neutrino angle and a maximal atmospheric one. We demonstrate that adding one sterile neutrino can change this setting, so that the active-sterile mixing and non-zero θ 13 can be generated simultaneously. From the phenomenological perspective, electron (anti)neutrino disappearance can be easily accommodated, while muon neutrino disappearance can vanish. Even the LSND results can be reconciled if the Majorana phases have very specific values. From the theory perspective, the setting requires the misalignment of some of the flavon vacuum expectation values, which may be achieved in an A 4 or D 4 flavour symmetry model using extra dimensions.

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Constraining sterile neutrino warm dark matter withChandraobservations of the Andromeda galaxy

Cited by 93 publications

References 157 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

Almost closing the νMSM sterile neutrino dark matter window with NuSTAR

Common origin of reactor and sterile neutrino mixing

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