Constraining warm dark matter candidates including sterile neutrinos and light gravitinos with WMAP and the Lyman-{alpha} forest

By M.Viel, Julien Lesgourgues, M. Haehnelt, S. Matarrese, A. Riotto. 2005

775 citations recorded by the source corpus.

The matter power spectrum at comoving scales of $(1\ensuremath{-}40){h}^{\ensuremath{-}1}\text{ }\text{ }\mathrm{Mpc}$ is very sensitive to the presence of Warm Dark Matter (WDM) particles with large free-streaming lengths. We present constraints on the mass of WDM particles from a combined analysis of the matter power spectrum inferred from the large samples of high-resolution high signal-to-noise Lyman-$\ensuremath{\alpha}$ forest data of Kim et al. (2004) and Croft et al. (2002) and the cosmic microwave background data of WMAP. We obtain a lower limit of ${m}_{\mathrm{WDM}}\ensuremath{\gtrsim}550\text{ }\text{ }\mathrm{eV}$ ($2\ensuremath{\sigma}$) for early decoupled thermal relics and ${m}_{\mathrm{WDM}}\ensuremath{\gtrsim}2.0\text{ }\text{ }\mathrm{keV}$ ($2\ensuremath{\sigma}$) for sterile neutrinos. We also investigate the case where in addition to cold dark matter a light thermal gravitino with fixed effective temperature contributes significantly to the matter density. In that case the gravitino density is proportional to its mass, and we find an upper limit ${m}_{3/2}\ensuremath{\lesssim}16\text{ }\text{ }\mathrm{eV}$ ($2\ensuremath{\sigma}$). This translates into a bound on the scale of supersymmetry breaking, ${\ensuremath{\Lambda}}_{\mathrm{susy}}\ensuremath{\lesssim}260\text{ }\text{ }\mathrm{TeV}$, for models of supersymmetric gauge mediation in which the gravitino is the lightest supersymmetric particle.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/684bafed7ce43ac75fbd181fbd068383e50d9e02

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Citations in the corpus

Small-Scale Challenges to the ΛCDM Paradigm (2017, methodology): “For example, WDM models have an effective free-streaming length λfs that scales inversely with particle mass (Bode, Ostriker & Turok 2001; Viel et al. 2005); in the Planck (2016) cosmology, this relation is approximately λfs = 33 (mWDM 1 keV )−1.11 kpc (8) and the corresponding free-streaming mass…”
A QUANTITATIVE EXPLANATION OF THE OBSERVED POPULATION OF MILKY WAY SATELLITE GALAXIES (2009, background): “…high redshift Lyα forest indicate that the small scale power expected in the standard ΛCDM scenario (inflationary cold dark matter with a cosmological constant) is indeed present in the primordial fluctuation spectrum (Narayanan et al. 2000; Viel et al. 2005; Abazajian 2006; Seljak et al. 2006).”
History of dark matter (2018, neutral): “VII), the combination of constraints from x-ray observations and measurements of the Lyman-α forest (Viel et al., 2005; Seljak, Slosar, and McDonald, 2006) disfavor sterile neutrino dark matter over this entire mass range.”
Cosmological and astrophysical parameters from the Sloan Digital Sky Survey flux power spectrum and hydrodynamical simulations of the Lyman α forest (2005, background): “…al. 1998, McDonald et al. 2000, Hui et al. 2001, Croft et al. 2002 [C02], McDonald 2003, Viel et al. 2003, Viel, Haehnelt & Springel 2004 [VHS], Desjacques & Haehnelt 2004, Viel, Weller & Haehnelt 2004, McDonald et al. 2004 [M04a], McDonald et al. 2004b [M04b], Viel et al. 2005, Lidz et al. 2005).”
Constraints on sterile neutrinos as dark matter candidates from the diffuse X-ray background (2005, background): “Together with the claims of Hansen et al. (2002) and Viel et al. (2005), putting a lower bound of m s > 2 keV on the neutrino mass from Lyman α forest observations, this would lead to a very narrow window for allowed sterile neutrino masses, if not excluding it completely.”
Impact of dark matter decays and annihilations on reionization (2006, background): “Furthermore, Viel et al. (2005) derived a lower limit mν s > 2 keV from the study of matter power spectrum fluctuations.”
The properties of warm dark matter haloes (2013, methodology): “Bode et al. (2001) and Viel et al. (2005) find that ν can take values between 1 and 1.2 depending on the fitting procedure; we adopted ν = 1 for simplicity.”
Constraints on neutrinos and WDM Hints, neutrino bounds and WDM constraints from SDSS DR14 Lyman-$\alpha$ and Planck full-survey data (2019, methodology): “Since it extends the lever arm of other cosmological probes towards smaller scales, it has often been used to constraint the parameters of models affecting only the smallest scales – like warm dark matter (WDM) [1–4] or interacting dark matter [5–7] – or altering the global shape of the power spectr”
A lower bound on the mass of dark matter particles (2008, background): “Therefore, various simplifying approximations have to be realized [30, 33–39].”
A fundamental problem in our understanding of low-mass galaxy evolution (2012, methodology): “Simulations are based on a WMAP5 cosmology, with the power spectrum truncated as suggested by Viel et al. (2005), using the analytical expression in Macciò et al. (2012).”
Sterile neutrino Dark Matter (2018, background): “ the thermal relics, n tr ˝n , thus reconciling astrophysical and cosmological DM observables. For thermal relics the suppression of power spectrum at small scales (large comoving k) behaves as k 10 [234,236]. This scale can be directly related to the freestreaming (31) (see [235]). The situation is”
Constraining dark matter-neutrino interactions using the CMB and large-scale structure (2014, background): “12 and mWDM is the mass of the warm thermal relic [53].”