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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7293
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dc.contributor.authorBhattacharjee, Pooja-
dc.contributor.authorMajumdar, Pratik-
dc.contributor.authorBiswas, Sayan-
dc.contributor.authorJoarder, Partha S.-
dc.date.accessioned2019-09-16T15:15:10Z-
dc.date.available2019-09-16T15:15:10Z-
dc.date.issued2019-08-21-
dc.identifier.citationJournal of Cosmology and Astroparticle Physics, 2019, p028en_US
dc.identifier.issn1475-7516 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/7293-
dc.descriptionRestricted Accessen_US
dc.description.abstractTucana-II (Tuc-II), a recently discovered and confirmed Ultra Faint Dwarf Spheroidal galaxy, has a high mass to light ratio as well as a large line-of-sight stellar velocity dispersion, thus making it an ideal candidate for an indirect dark matter (DM) search. In this paper, we have analyzed nine years of γ-ray data obtained from the Fermi-LAT instrument from the direction of Tuc-II. The fact that a very weak significant γ-ray excess (2.2σ) over the background of Tuc-II have been detected from the location of this galaxy. We have observed that this excess of γ-ray emission from the of location Tuc-II rises with longer periods of data. If WIMP pair annihilation is assumed for this faint emission, for bbar b annihilation channel the test statistics (TS) value peaks at DM mass ~ 14 GeV and for τ+τ− annihilation channel it peaks at DM mass 4 GeV. It is then called for an estimation of the 95% confidence level upper limit of the possible velocity weighted self-annihilation cross-section of the DM particles (WIMPs) within Tuc-II by fitting the observed γ-ray flux with spectra expected for DM annihilation. The estimated upper limits of the cross-sections from Tuc-II are then compared with two other dwarf galaxies that are considered to be good DM candidates in several studies. We have also compared our results with the cross-sections obtained in various popular theoretical models of the WIMPs to find that our results impose reasonable tight constraints on the parameter spaces of those DM models. In the concluding section, we compared our results with the similar results obtained from a combined dSph analysis by the Fermi-LAT collaboration as well as the results obtained from the studies of DM in the dwarf galaxies by the major ground-based Cherenkov experiments.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2019JCAP...08..028B/abstracten_US
dc.relation.urihttps://arxiv.org/abs/1804.07542v1en_US
dc.relation.urihttps://doi.org/10.1088/1475-7516/2019/08/028en_US
dc.rights2019 IOP Publishing Ltd and Sissa Medialaben_US
dc.subjectdark matter theoryen_US
dc.subjectdwarfs galaxiesen_US
dc.subjectgamma ray detectorsen_US
dc.subjectgamma ray experimentsen_US
dc.titleAnalysis of Fermi-LAT data from Tucana-II: possible constraints on the Dark Matter models with an intriguing hint of a signalen_US
dc.typeArticleen_US
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