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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/8217
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dc.contributor.authorParichha, Abineet-
dc.contributor.authorSethi, Shiv-
dc.date.accessioned2024-01-30T06:49:35Z-
dc.date.available2024-01-30T06:49:35Z-
dc.date.issued2023-11-13-
dc.identifier.citationJournal of Cosmology and Astroparticle Physics, 2023, Article No.061en_US
dc.identifier.issn1475-7516-
dc.identifier.urihttp://hdl.handle.net/2289/8217-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractThe Weakly Interacting Massive Particles (WIMPs) have long been the favoured Cold Dark Matter (CDM) candidate in the standard CDM model. However, owing to great improvement in the experimental sensitivity in the past decade, some parameter space of the Supersymmetric (SUSY)-based WIMP model is ruled out. In addition, a massive stable WIMP as the CDM particle is also at variance with other astrophysical observables at small scales. We consider a model that addresses both these issues. In the model, the WIMP decays into a massive particle and radiation. We study the background evolution and the first order perturbation theory (coupled Einstein-Boltzmann equations) for this model and show that the dynamics can be captured by a single parameter r = mL/q, which is the ratio of the lighter mass and the comoving momentum of the decay particle. We incorporate the relevant equations in the existing Boltzmann code CLASS to compute the matter power spectra and Cosmic Microwave Background (CMB) angular power spectra. The decaying WIMP model is akin to a non-thermal Warm Dark Matter (WDM) model and suppresses matter power at small scales, which could alleviate several issues that plague the CDM model at small scales.We compare the predictions of the model with CMB and galaxy clustering data. As the model deviates from the CDM model at small scales, the evolution of the collapse fraction of matter in the universe is compared with the high-redshift Sloan Digital Sky Survey (SDSS) HI data. Both these data sets yield r & 106, which can be translated into the bounds on other parameters. In particular, we obtain the following lower bounds on the thermallyaveraged self-annihilation cross-section of WIMPs, h vi, and the lighter mass: h vi & 4.9 × 10−34 cm3 sec−1 and mL & 2.4 keV. The lower limit on mL is comparable to constraints on the mass of thermally-produced WDM particle. The limit on the self-annihilation cross-section greatly expands the available parameter space as compared to the stable WIMP scenario.en_US
dc.language.isoenen_US
dc.publisherIOP Publishing Ltden_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2023JCAP...11..061P/abstracten_US
dc.relation.urihttps://arxiv.org/abs/2305.10315en_US
dc.relation.urihttps://doi.org/10.1088/1475-7516/2023/11/061en_US
dc.rights2023, The Publisheren_US
dc.subjectCosmological parameters from LSSen_US
dc.subjectCosmological perturbation theoryen_US
dc.subjectDark matter theoryen_US
dc.subjectParticle physics - cosmology connectionen_US
dc.titleWIMP decay as a possible Warm Dark Matter modelen_US
dc.typeArticleen_US
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