Search for dark matter annihilation in the Wolf-Lundmark-Melotte dwarf irregular galaxy with H.E.S.S.

Abdallah, H.; Adam, R.; Aharonian, F.; Benkhali, F. Ait; Angüner, E. O.; Arcaro, C.; Armand, Céline; Armstrong, T. P.; Ashkar, Halim; Backes, Michael; Baghmanyan, Vardan; Martins, Victor Barbosa; Barnacka, A.; Barnard, M.; Becherini, Y.; Berge, D.; Bernlöhr, K.; Bi, Baiyang; Böttcher, M.; Boisson, C.; Bolmont, J.; Lavergne, Mathieu de Bony de; Breuhaus, M.; Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.; Caroff, S.; Carosi, A.; Casanova, S.; Chand, T.; Chandra, S.; Chen, A.; Cotter, Garret; Curyło, M.; Mbarubucyeye, J. Damascene; Davids, I. D.; Davies, J.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati‐Ataï, A.; Dmytriiev, A.; Donath, Axel; Doroshenko, V.; Duffy, C.; Dyks, J.; Egberts, K.; Eichhorn, F.; Einecke, S.; Emery, Gabriel; Ernenwein, J.-P.; Feijen, Kirsty; Fegan, S. J.; Fiaßon, A.; Clairfontaine, G. Fichet de; Fontaine, G.; Funk, Sebastian; Füßling, M.; Gabici, S.; Gallant, Y. A.; Giavitto, G.; Giunti, Luca; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M.-H.; Hahn, Joachim; Haupt, M.; Hermann, G.; Hinton, Jim; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.; Hörbe, M.; Horns, D.; Huber, David Miles; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jardin-Blicq, A.; Joshi, Vikas; Jung-Richardt, I.; Kasai, E.; Kastendieck, M. A.; Katarzyński, K.; Katz, U.; Khangulyan, D.; Khélifi, B.; Klepser, S.; Kluźniak, W.; Komin, Nu.; Konno, Ruslan; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna, G.; Lemière, A.; Lemoine‐Goumard, M.; Lenain, J.‐P.; Levy, C.; Löhse, T.; Lypova, I.; Mackey, Jonathan; Majumdar, Jhilik; Malyshev, D.; Marandon, V.; Marchegiani, ¶.; Marcowith, A.; Mares, Arnaud; Martí-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Meyer, M.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Montanari, A.; Moore, C. J.; Morris, Paul; Moulin, Emmanuel; Müller, J.; Murach, T.; Nakashima, Kaori; Nayerhoda, A.; Naurois, M. de; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O’Brien, P. T.; Odaka, Hirokazu; Ohm, S.; Olivera-Nieto, Laura; Wilhelmi, E. de Oña; Ostrowski, M.; Panter, M.; Panny, Sebastian; Parsons, R. D.; Peron, Giada; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Noel, A. Priyana; Prokhorov, Dmitry; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Remy, Quentin; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Sailer, Simon; Sánchez, David; Santangelo, A.; Sasaki, M.; Scalici, M.; Schüßler, F.; Schutte, H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, Atreyee; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, Marion; Stawarz, Ł.; Sun, Lei; Steenkamp, R.; Stegmann, C.; Steinmassl, Simon; Steppa, C.; Takahashi, Tadayuki; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani, D.; Tluczykont, M.; Tomankova, L.; Trichard, C.; Tsirou, M.; Tuffs, R.; Uchiyama, Y.; Walt, D. J. van der; Eldik, C. van; Rensburg, C. van; Soelen, B. van; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, Jacco; Völk, H. J.; Vuillaume, Thomas; Wadiasingh, Zorawar; Wagner, S. J.; Watson, Jason; Werner, F.; White, R.; Wierzcholska, A.; Wong, Yu Wun; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, Davit; Zdziarski, A. A.; Zech, A.; Zhu, Shou-hua; Zorn, J.; Zouari, Samuel; Żywucka, N.

doi:10.1103/physrevd.103.102002

Cited by 17 publications

(15 citation statements)

References 47 publications

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“…These searches have been complemented by recent searches in the TeV regime: H.E.S.S. has observed the Wolf-Lundmark-Melotte (WLM) dIrr galaxy [144] in the Southern hemisphere (see Fig. 1) for 18 hours, constraining an annihilation cross section in the order of magnitude σv 10 −21 GeV 2 cm −5 in the range of DM masses of a few TeV.…”

Section: Irregular and Spiral Local Galaxiesmentioning

confidence: 99%

TeV Dark Matter Searches in the Extragalactic Gamma-ray Sky

Hütten

Kerszberg

2022

Galaxies

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High-energetic gamma rays from astrophysical targets constitute a unique probe for annihilation or decay of heavy particle dark matter (DM). After several decades, diverse null detections have resulted in strong constraints for DM particle masses up to the TeV scale. While the gamma-ray signature is expected to be universal from various targets, uncertainties of astrophysical origin strongly affect and weaken the limits. At the same time, spurious signals may originate from non-DM related processes. The many gamma-ray targets in the extragalactic sky being searched for DM play a crucial role to keep these uncertainties under control and to ultimately achieve an unambiguous DM detection. Lately, a large progress has been made in combined analyses of TeV DM candidates towards different targets by using data from various instruments and over a wide range of gamma-ray energies. These approaches not only resulted in an optimal exploitation of existing data and an improved sensitivity, but also helped to level out target- and instrument-related uncertainties. This review gathers all searches in the extragalactic sky performed so far with the space-borne Fermi-Large Area Telescope, the ground-based imaging atmospheric Cherenkov telescopes, and the High-Altitude Water Cherenkov Gamma-Ray Observatory (HAWC). We discuss the different target classes and provide a complete list of all analyses so far.

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Section: Irregular and Spiral Local Galaxiesmentioning

confidence: 99%

TeV Dark Matter Searches in the Extragalactic Gamma-ray Sky

Hütten

Kerszberg

2022

Galaxies

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“…Searches at the high energies (0.1-100 TeV) with the High Energy Stereoscopic System have been used to constrain the crosssection of self-annihilating WIMPS in the Galactic Centre and nearby dwarf galaxies (Abdallah et al 2018(Abdallah et al , 2021. Such searches are sensitive to mono-energetic photon annihilation products arising from the χχ → γ γ annihilation channel as well as to the γ -ray continuum resulting from a wide range of other (W + W − , Z + Z − , b b, t t, e + e − , μ + μ − and τ + τ − ) annihilation channels available in Supersymmetric Standard Models (see Bergström, Ullio, & Buckley 1998).…”

Section: Introductionmentioning

confidence: 99%

“…The most likely places to observe electromagnetic signatures of dark matter are in dense dark matter cores, which are predicted to occur in the nuclei of galaxies, and should have size scales in the range 0.1 to 5 kpc (Lazar et al 2020). Thus searches have concentrated on objects such as the Galactic Centre (Siegert et al 2016a;Reynolds et al 2017), the Large Magellanic Cloud (LMC; Siffert et al 2011) and nearby dwarf galaxies (Siegert et al 2016b(Siegert et al , 2022aAlbert et al 2017;Cook et al 2020;Abdallah et al 2021). The dwarf galaxies have the advantage of being more dark matter-dominated, with fewer sources of strong emission which arise from particle acceleration from other astrophysical processes such as star formation, supernovae and massive black holes.…”

Section: Introductionmentioning

confidence: 99%

A search for annihilating dark matter in 47 Tucanae and Omega Centauri

Bond

Bekki

Westmeier

2022

Publ. Astron. Soc. Aust.

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A plausible formation scenario for the Galactic globular clusters 47 Tucanae (47 Tuc) and Omega Centauri $(\omega$ Cen) is that they are tidally stripped remnants of dwarf galaxies, in which case they are likely to have retained a fraction of their dark matter cores. In this study, we have used the ultra-wide band receiver on the Parkes telescope (Murriyang) to place upper limits on the annihilation rate of exotic Light Dark Matter particles $(\chi)$ via the $\chi\chi\rightarrow e^+e^-$ channel using measurements of the recombination rate of positronium (Ps). This is an extension of a technique previously used to search for Ps in the Galactic Centre. However, by stacking of spectral data at multiple line frequencies, we have been able to improve sensitivity. Our measurements have resulted in $3-\sigma$ flux density (recombination rate) upper limits of 1.7 mJy $\left(1.4\times 10^{43}\, \mathrm{s}^{-1}\right)$ and 0.8 mJy $\left(1.1 \times 10^{43} \mathrm{s}^{-1}\right)$ for 47 Tuc and $\omega$ Cen, respectively. Within the Parkes beam at the cluster distances, which varies from 10–23 pc depending on the frequency of the recombination line, and for an assumed annihilation cross-section $\langle\sigma v\rangle = 3\times 10^{-29} \mathrm{cm}^3\, \mathrm{s}^{-1}$ , we calculate upper limits to the dark matter mass and rms dark matter density of ${\lesssim} 1.2-1.3\times 10^5 f_n^{-0.5}$ $\left(m_\chi/\mathrm{MeV\, c}^{-2}\right)$ $\mathrm{M}_{\odot}$ and ${\lesssim} 48-54 f_n^{-0.5}$ $\left(m_\chi/\mathrm{MeV\, c}^{-2}\right)$ $\mathrm{M}_{\odot} \mathrm{pc}^{-3}$ for the clusters, where $f_n=R_n/R_p$ is the ratio of Ps recombination transitions to annihilations, estimated to be ${\sim}0.01$ . The radio limits for $\omega$ Cen suggest that, for a fiducial dark/luminous mass ratio of ${\sim}0.05$ , any contribution from Light Dark Matter is small unless $\langle\sigma v\rangle < 7.9\times 10^{-28}\ \left(m_\chi/\mathrm{MeV\, c}^{-2}\right)^2 \mathrm{cm}^3 \mathrm{s}^{-1}$ . Owing to the compactness and proximity of the clusters, archival 511-keV measurements suggest even tighter limits than permitted by CMB anisotropies, $\langle\sigma v\rangle < 8.6\times 10^{-31}\ (m_\chi/\mathrm{MeV\, c}^{-2})^2 \mathrm{cm}^3 \mathrm{s}^{-1}$ . Due to the very low synchrotron radiation background, our recombination rate limits substantially improve on previous radio limits for the Milky Way.

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“…In the absence of any excess in the data over the estimated γ-ray background, only upper limits on the dark matter annihilation cross-section have been derived as a function of the presumed DM mass. These limits are obtained from either one dSph or by performing a stack of their respective observations with either a continuous spectrum [13][14][15][16][17][18][19][20][21][22][23][24][25] or a mono-energetic line [24][25][26][27]. More recently, combined DM searches have been carried out to increase the statistics and the sensitivity to a potential DM signal.…”

Section: Introductionmentioning

confidence: 99%

Dark matter indirect detection limits from complete annihilation patterns

Armand¹,

Herrmann²

2022

Preprint

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While cosmological and astrophysical probes suggest that dark matter would make up for 85% of the total matter content of the Universe, the determination of its nature remains one of the greatest challenges of fundamental physics. Assuming the ΛCDM cosmological model, Weakly Interacting Massive Particles would annihilate into Standard Model particles, yielding γ-rays, which could be detected by ground-based telescopes. Dwarf spheroidal galaxies represent promising targets for such indirect searches as they are assumed to be highly dark matter dominated with the absence of astrophysical sources nearby. Previous studies have led to upper limits on the annihilation cross-section assuming single exclusive annihilation channels. In this work, we consider a more realistic situation and take into account the complete annihilation pattern within a given particle physics model. This allows us to study the impact on the derived upper limits on the dark matter annihilation cross-section from a full annihilation pattern compared to the case of a single annihilation channel. We use mock data for the Cherenkov Telescope Array simulating the observations of the promising dwarf spheroidal galaxy Sculptor. We show the impact of considering the full annihilation pattern within a simple framework where the Standard Model of particle physics is extended by a singlet scalar. Such a model shows new features in the shape of the predicted upper limit which reaches a value of σv = 3.8 × 10 −24 cm −3 s −1 for a dark matter mass of 1 TeV at 95% confidence level. We suggest to consider the complete particle physics information in order to derive more realistic limits.

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Search for dark matter annihilation in the Wolf-Lundmark-Melotte dwarf irregular galaxy with H.E.S.S.

Cited by 17 publications

References 47 publications

TeV Dark Matter Searches in the Extragalactic Gamma-ray Sky

TeV Dark Matter Searches in the Extragalactic Gamma-ray Sky

A search for annihilating dark matter in 47 Tucanae and Omega Centauri

Dark matter indirect detection limits from complete annihilation patterns

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