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The effects of the small-scale behaviour of dark matter power spectrum on CMB spectral distortion

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dc.contributor.author Sarkar, A
dc.contributor.author Sethi, S. K
dc.contributor.author Das, Subinoy
dc.date.accessioned 2020-11-11T01:08:38Z
dc.date.available 2020-11-11T01:08:38Z
dc.date.issued 2017-07
dc.identifier.citation Journal of Cosmology and Astroparticle Physics, Vol. 2017, No. 7, 12 en_US
dc.identifier.issn 1475-7516
dc.identifier.uri http://prints.iiap.res.in/handle/2248/6820
dc.description Restricted Access © IOP Publishing https://doi.org/10.1088/1475-7516/2017/07/012 en_US
dc.description.abstract After numerous astronomical and experimental searches, the precise particle nature of dark matter is still unknown. The standard Weakly Interacting Massive Particle(WIMP) dark matter, despite successfully explaining the large-scale features of the universe, has long-standing small-scale issues. The spectral distortion in the Cosmic Microwave Background(CMB) caused by Silk damping in the pre-recombination era allows one to access information on a range of small scales 0.3 Mpc < k < 104 Mpc−1 , whose dynamics can be precisely described using linear theory. In this paper, we investigate the possibility of using the Silk damping induced CMB spectral distortion as a probe of the small-scale power. We consider four suggested alternative dark matter candidates — Warm Dark Matter (WDM), Late Forming Dark Matter (LFDM), Ultra Light Axion (ULA) dark matter and Charged Decaying Dark Matter (CHDM); the matter power in all these models deviate significantly from the ΛCDM model at small scales. We compute the spectral distortion of CMB for these alternative models and compare our results with the ΛCDM model. We show that the main impact of alternative models is to alter the sub-horizon evolution of the Newtonian potential which affects the late-time behaviour of spectral distortion of CMB. The y-parameter diminishes by a few percent as compared to the ΛCDM model for a range of parameters of these models: LFDM for formation redshift zf = 105 (7%); WDM for mass mwdm = 1 keV (2%); CHDM for decay redshift zdecay = 105 (5%); ULA for mass ma = 10−24 eV (3%). This effect from the pre-recombination era can be masked by orders of magnitude higher y-distortions generated by late-time sources, e.g. the Epoch of Reionization and tSZ from the cluster of galaxies. We also briefly discuss the detectability of this deviation in light of the upcoming CMB experiment PIXIE, which might have the sensitivity to detect this signal from the pre-recombination phase. en_US
dc.language.iso en en_US
dc.publisher IOP Publishing en_US
dc.subject CMBR theory en_US
dc.subject Cosmological perturbation theory en_US
dc.subject Sunyaev-Zeldovich effect en_US
dc.subject Dark matter theory en_US
dc.title The effects of the small-scale behaviour of dark matter power spectrum on CMB spectral distortion en_US
dc.type Article en_US


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