Charge constraints of macroscopic dark matter

Sidhu, Jagjit Singh

doi:10.1103/physrevd.101.043526

Cited by 10 publications

(5 citation statements)

References 43 publications

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“…Later, we had proposed a systematic approach to the astrophysical quantities in play in the empirical determination of the DM distribution [15] (hereafter Paper I). In Paper I, we also presented a likelihood function that can be used in the particle interpretation of data coming from direct and indirect searches in order to self-consistently include astrophysical uncertainties that affect our determination of the DM distribution [16][17][18][19][20][21][22][23][24].…”

Section: Introductionmentioning

confidence: 99%

Handling the uncertainties in the Galactic Dark Matter distribution for particle Dark Matter searches

Benito

Cuoco

Iocco

2019

J. Cosmol. Astropart. Phys.

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In this work we characterize the distribution of Dark Matter (DM) in the Milky Way (MW), and its uncertainties, adopting the well known "Rotation Curve" method. We perform a full marginalization over the uncertainties of the Galactic Parameters and over the lack of knowledge on the morphology of the baryonic components of the Galaxy. The local DM density ρ 0 is constrained to the range 0.3−0.8 GeV/cm 3 at the 2σ level, and has a strong positive correlation to R 0 , the local distance from the Galactic Center. The not well-known value of R 0 is thus, at the moment, a major limitation in determining ρ 0 . Similarly, we find that the inner slope of the DM profile, γ, is very weakly constrained, showing no preference for a cored profile (γ 0) or a cuspy one (γ [1.0, 1.4]). Some combination of parameters can be, however, strongly constrained. For example the often used standard ρ 0 = 0.3 GeV/cm 3 , R 0 = 8.5 kpc is excluded at more than 4 σ. We release the full likelihood of our analysis in a tabular form over a multidimensional grid in the parameters characterizing the DM distribution, namely the scale radius R s , the scale density ρ s , the inner slope of the profile γ, and R 0 . The likelihood can be used to include the effect of the DM distribution uncertainty on the results of searches for an indirect DM signal in gamma-rays or neutrinos, from the Galactic Center (GC), or the Halo region surrounding it. As one example, we study the case of the GC excess in gamma rays. Further applications of our tabulated uncertainties in the DM distribution involve local DM searches, like direct detection and anti-matter observations, or global fits combining local and GC searches.

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Section: Introductionmentioning

confidence: 99%

Handling the uncertainties in the Galactic Dark Matter distribution for particle Dark Matter searches

Benito

Cuoco

Iocco

2019

J. Cosmol. Astropart. Phys.

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“…refs. [14,[26][27][28][29]. Constraints on Macros from considerations related to the growth of structures and the effects on astrophysical systems (like, e.g., galaxy clusters or other compact objects such as neutron stars and white dwarfs) can be found in [26,[30][31][32][33] (for other constraints on MDM, see also [25,[34][35][36][37]).…”

Section: Jcap07(2021)027mentioning

confidence: 99%

“…This is true provided that the diffusion time for a photon to cross the average separation between two Macros is small compared to the Hubble time, H −1 . In terms of the mass of Macros, this condition can be written as[27]…”

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confidence: 99%

Updated cosmological constraints on Macroscopic Dark Matter

Caloni

Gerbino

Lattanzi

2021

J. Cosmol. Astropart. Phys.

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We revise the cosmological phenomenology of Macroscopic Dark Matter (MDM) candidates, also commonly dubbed as Macros. A possible signature of MDM is the capture of baryons from the cosmological plasma in the pre-recombination epoch, with the consequent injection of high-energy photons in the baryon-photon plasma. By keeping a phenomenological approach, we consider two broad classes of MDM in which Macros are composed either of ordinary matter or antimatter. In both scenarios, we also analyze the impact of a non-vanishing electric charge carried by Macros. We derive constraints on the Macro parameter space from three cosmological processes: the change in the baryon density between the end of the Big Bang Nucleosynthesis (BBN) and the Cosmic Microwave Background (CMB) decoupling, the production of spectral distortions in the CMB and the kinetic coupling between charged MDM and baryons at the time of recombination. In the case of neutral Macros we find that the tightest constraints are set by the baryon density condition in most of the parameter space. For Macros composed of ordinary matter and with binding energy I, this leads to the following bound on the reduced cross-section: σX/M X ≲ 6.8 · 10-7(I/MeV)-1.56 cm2 g-1. Charged Macros with surface potential V X, instead, are mainly constrained by the tight coupling with baryons, resulting in σX/MX ≲ 2 · 10-11(|V X|/MeV)-2cm2 g-1. Finally, we show that future CMB spectral distortions experiments, like PIXIE and SuperPIXIE, would have the sensitivity to probe larger regions of the parameter space: this would allow either for a possible evidence or for an improvement of the current bounds on Macros as dark matter candidates.

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“…As the viable parameter space for WIMP-like dark matter shrinks following null measurements from sensitive direct detection experiments developed over the past decades, the scope of DM direct detection searches has broadened. Candidates include sub-GeV dark matter [1][2][3][4][5][6][7][8][9][10][11][12], superheavy dark matter [13][14][15][16][17][18][19] and macro dark matter [20][21][22][23]. However, the WIMP family still includes many viable candidates that remain out of reach from the current generation of experiments.…”

Section: Introductionmentioning

confidence: 99%

Pushing the frontier of WIMPy inelastic dark matter: journey to the end of the periodic table

Song,

Nagorny,

Vincent

2021

Preprint

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We explore the reach of low-background experiments made of small quantities of heavy nuclear isotopes in probing the parameter space of inelastic dark matter that is kinematically inaccessible to classic direct detection experiments. Through inelastic scattering with target nuclei, dark matter can yield a signal either via nuclear recoil or nuclear excitation. We present new results based on this approach, using data from low-energy gamma quanta searches in low-background experiments with Hf and Os metal samples, and measurements with CaWO4 and PbWO4 crystals as scintillating bolometers. We place novel bounds on WIMPy inelastic dark matter up to mass splittings of about 640 keV, and provide forecasts for the reach of future experiments.

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Charge constraints of macroscopic dark matter

Cited by 10 publications

References 43 publications

Handling the uncertainties in the Galactic Dark Matter distribution for particle Dark Matter searches

Handling the uncertainties in the Galactic Dark Matter distribution for particle Dark Matter searches

Updated cosmological constraints on Macroscopic Dark Matter

Pushing the frontier of WIMPy inelastic dark matter: journey to the end of the periodic table

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