Constraints on dark matter models from the observation of Triangulum-II with the <i>Fermi</i> Large Area Telescope

Biswas, Sayan; Bhattacharjee, Pooja; Majumdar, P.; Das, Subinoy; Das, Mousumi; Joarder, P. S.

doi:10.1088/1475-7516/2017/11/003

Cited by 8 publications

(7 citation statements)

References 67 publications

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“…γ-flux upper limit for Γ = 1 is almost 2 orders of magnitude lower than the one corresponding to Γ = 2.4. This result is consistent with our previous work for Triangulum-II (Tri-II) [66], in which we have also found that the flux upper limit in 95 % C.L. is increased by increasing the spectral indices.…”

Section: Results Of the Power-law Modelingsupporting

confidence: 93%

Analysis of Fermi-LAT data from Tucana-II: possible constraints on the Dark Matter models with an intriguing hint of a signal

Bhattacharjee

Majumdar

Biswas

et al. 2019

J. Cosmol. Astropart. Phys.

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Tucana-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 bb 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.

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Section: Results Of the Power-law Modelingsupporting

confidence: 93%

Analysis of Fermi-LAT data from Tucana-II: possible constraints on the Dark Matter models with an intriguing hint of a signal

Bhattacharjee

Majumdar

Biswas

et al. 2019

J. Cosmol. Astropart. Phys.

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“…Overall, in all these cases, due to the stringent flux density limits, our results put comparable limits as some of the recent works (e.g. Archambault et al 2017;Biswas et al 2017;Bhattacharjee et al 2019;Vollmann et al 2020) from other radio as well as high energy observations of the dSph galaxies.…”

Section: Constraints On Dark Mattersupporting

confidence: 89%

Stringent constraint on the radio signal from dark matter annihilation in dwarf spheroidal galaxies using the TGSS

Basu,

Roy,

Choudhuri

et al. 2021

Preprint

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Weakly Interacting Massive Particles (WIMPs) are considered to be one of the favoured dark matter candidates. Searching for any detectable signal due to the annihilation and decay of WIMPs over the entire electromagnetic spectrum has become a matter of interest for the last few decades. WIMP annihilation to Standard Model particles gives rise to a possibility of detection of this signal at low radio frequencies via synchrotron radiation. Dwarf Spheroidal Galaxies (dSphs) are expected to contain a huge amount of dark matter which makes them promising targets to search for such large scale diffuse radio emission. In this work, we present a stacking analysis of 23 dSph galaxies observed at low frequency (147.5 MHz) as part of the TIFR-GMRT Sky Survey (TGSS). The non-detection of any signal from these stacking exercises put very tight constraints on the dark matter parameters. The best limit comes from the novel method of stacking after scaling the radio images of the individual dSph galaxy fields after scaling them by the respective half-light radius. The constraint on the thermally averaged cross-section is below the thermal relic cross-section value over a range of WIMP mass for reasonable choices of relevant astrophysical parameters. Such analysis using future deeper observation of individual targets as well as stacking can potentially reveal more about the WIMP dark matter properties.

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“…5(a,b) and 6, we can notice that none of the LSB galaxies have put any constraint on any of these above mentioned theoretical models. The LAT sensitivities obtained from these four LSB galaxies are nearly 3 orders higher than the LAT sensitivity estimated from Tri-II [19]. Hence, from Figs.…”

Section: Constraints On the Annihilation Cross-sectionmentioning

confidence: 59%

“…(a,b) and Fig. 6, we have also compared the LAT-sensitivity obtained from LSB galaxies with newly discovered ultra faint dwarf spheroidal (dSph) galaxy, Triangulum-II (Tri-II) [19] for its two different values of velocity dispersion σ. In Fig 5(a,b), we have considered two DM particle models, namely, minimal supergravity (mSUGRA) [57] and Minimal Supersymmetric Standard Model (MSSM) [58].…”

Section: Constraints On the Annihilation Cross-sectionmentioning

confidence: 99%

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Multiwavelength analysis of low surface brightness galaxies to study possible dark matter signature

Bhattacharjee,

Majumdar,

Das

et al. 2019

Preprint

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Low Surface Brightness (LSB) galaxies are thought to be one of the most dark matter (DM) dominated galaxies in our Universe. They have very diffuse, low surface density stellar disks that have poor star formation rates and hence appear faint in optical images. LSB galaxies are also very rich in neutral hydrogen (HI) gas which usually extends well beyond their stellar disks. Their extended HI rotation curves indicate the presence of very massive DM halos compared to normal bright galaxies and their mass to light (M/L) ratios are high, which is typical for dark matter dominated galaxies. Hence, LSB galaxies are ideal laboratories for the indirect detection of DM using observations of γ-ray emission which could possibly originate from pair-annihilation (or decay) of the weakly interacting massive particles (WIMPs) in their halos. In this paper we have searched for WIMP annihilation or decay signatures in four LSB galaxies, UGC 12632, UGC 12732, UGC 11707, UGC 3371. Here we present analysis of nearly nine years data from the Fermi Large Area Telescope (LAT). Above 100 MeV, no excess emission was detected from the LSB galaxies. We have then determined the stacked γ-ray flux using spectra expected for WIMP annihilation. With the RX-DMFIT code, we have also predicted the possible upper limits for the detection of radio emission associated with WIMP annihilation from LSB galaxies. We have compared our results with different proposed theoretical WIMP models to examine the constraints on the parameter space of the DM models. We also discuss the possibility of detecting a positive signal from LSB galaxies using the upcoming ground-based γ-ray telescope, the Cherenkov Telescope Array.

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Constraints on dark matter models from the observation of Triangulum-II with the Fermi Large Area Telescope

Cited by 8 publications

References 67 publications

Analysis of Fermi-LAT data from Tucana-II: possible constraints on the Dark Matter models with an intriguing hint of a signal

Analysis of Fermi-LAT data from Tucana-II: possible constraints on the Dark Matter models with an intriguing hint of a signal

Stringent constraint on the radio signal from dark matter annihilation in dwarf spheroidal galaxies using the TGSS

Multiwavelength analysis of low surface brightness galaxies to study possible dark matter signature

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