The Anti Matter Spectrometer (AMS-02): a Particle Physics Detector In Space

Battiston, R.

doi:10.1016/j.nuclphysbps.2006.12.091

Cited by 8 publications

(2 citation statements)

References 19 publications

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“…Tighter constraints are expected to be possible with future PAMELA data, and hopefully with AMS2 (Battiston 2007). The current uncertainty in those parameters leads to large theoretical errors in secondary positrons ) and therefore electrons, as reviewed in Sect.…”

Section: Review Of the Propagation Parametersmentioning

confidence: 95%

Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes

Delahaye

Lavalle

Lineros

et al. 2010

A&A

202

334

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Context. The so-called excess of cosmic ray (CR) positrons observed by the PAMELA satellite up to 100 GeV has led to many interpretation attempts, from standard astrophysics to a possible exotic contribution from dark matter annihilation or decay. The Fermi data subsequently obtained about CR electrons and positrons in the range 0.02-1 TeV, and HESS data above 1 TeV have provided additional information about the leptonic content of local Galactic CRs. Aims. We analyse predictions of the CR lepton fluxes at the Earth of both secondary and primary origins, evaluate the theoretical uncertainties, and determine their level of consistency with respect to the available data. Methods. For propagation, we use a relativistic treatment of the energy losses for which we provide useful parameterizations. We compute the secondary components by improving on the method that we derived earlier for positrons. For primaries, we estimate the contributions from astrophysical sources (supernova remnants and pulsars) by considering all known local objects within 2 kpc and a smooth distribution beyond. Results. We find that the electron flux in the energy range 5-30 GeV is well reproduced by a smooth distant distribution of sources with index γ ∼ 2.3−2.4, while local sources dominate the flux at higher energy. For positrons, local pulsars have an important effect above 5-10 GeV. Uncertainties affecting the source modeling and propagation are degenerate and each translates into about one order of magnitude error in terms of local flux. The spectral shape at high energy is weakly correlated with the spectral indices of local sources, but more strongly with the hierarchy in their distance, age and power. Despite the large theoretical errors that we describe, our global and self-consistent analysis can explain all available data without over-tuning the parameters, and therefore without the need to consider any exotic physics. Conclusions. Though a standard paradigm of Galactic CRs is well established, our results show that we can hardly talk about any standard model of CR leptons, because of the very large theoretical uncertainties. Our analysis provides details about the impact of these uncertainties, thereby sketching a roadmap for future improvements.

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Section: Review Of the Propagation Parametersmentioning

confidence: 95%

Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes

Delahaye

Lavalle

Lineros

et al. 2010

A&A

202

334

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“…This is crucial for the background calculation (standard antimatter production) in order to confirm/support any claim of an excess. Besides, AMS-02 should be launched in the coming years, and provide additional crucial information on GCR propagation by measuring the radioactive species (Battiston 2007).…”

Section: Introductionmentioning

confidence: 99%

Full calculation of clumpiness boost factors for antimatter cosmic rays in the light of ${\Lambda}$CDM N-body simulation results

Lavalle¹,

Yuan

Maurin³

et al. 2007

A&A

147

183

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Context. Anti-proton and positron Galactic cosmic ray spectra are among the key targets for indirect detection of dark matter. The boost factors, corresponding to an enhancement of the signal, and linked to the clumpiness properties of the dark matter distribution, have been taken as high as thousands in the past. The dramatic impact of these boost factors for indirect detection of antiparticles, for instance with the PAMELA satellite or the coming AMS-02 experiment, asks for their detailed calculation. Aims. We take into account the state-of-the-art results of high resolution N-body dark matter simulations to calculate the most likely energy dependent boost factors, which are linked to the cosmic ray propagation properties, for anti-protons and positrons. The results from extreme, but still possible, configurations of the clumpy dark matter component are also discussed. Methods. Starting from the mass and space distributions of sub-halos, the anti-proton and positron propagators are used to calculate the mean value and the variance of the boost factor for the primary fluxes. We take advantage of the statistical method introduced in Lavalle et al. (2007) and cross-check the results with Monte Carlo computations. Results. By spanning some extreme configurations of sub-halo and propagation properties, we find that the average contribution of the clumps is negligible compared to that of the smooth dark matter component. Dark matter clumps do not lead to enhancement of the signals, unless they are taken with some extreme (unexpected) properties. This result is independent of the nature of the selfannihilating dark matter candidate considered, and provides precise estimates of the theoretical and the statistical uncertainties of the antimatter flux from sub-halos. Conclusions. Spectral distortions can still be expected in antimatter flux measurements, but scenarios invoking large and even mild clumpiness boost factors are strongly disfavoured by our analysis. Some very extreme configurations could still lead to large enhancements, e.g. (i) very small clumps with masses < ∼ 10 −6 M following a M −α mass distribution with α > ∼ 2, highly concentrated with internal r −β profiles with β > ∼ 1.5, and spatially distributed according to the smooth component; or (ii) a big sub-halo of mass > ∼ 0 7 M within a distance of < ∼ 1 kpc from the Earth. However, they are very unlikely from either theoretical or statistical arguments.

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Spaceborne Experiments

Battiston¹

2020

Particle Physics Reference Library

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The Universe is the ultimate laboratory to understand the laws of nature. Under the action of the fundamental forces, lasting infinitesimal times or billion of years, matter and energy reach most extreme conditions. Using sophisticated instruments capable to select the signals reaching us from the depths of space and of time, we are able to extract information otherwise not obtainable with the most sophisticated ground based experiments. The results of these observations deeply influence the way we today look at the Universe and try to understand it. During hundreds of thousands of years we have observed the sky only using our eyes, accessing in this way only the very small part of the electromagnetic radiation which is able to traverse the atmosphere, the visible light. The first telescope observations by Galileo in 1609, which dramatically changed our understanding of the solar system, yet were based only on the visible part of the electromagnetic spectrum. Only during the second half of the twentieth century we started to access wider parts of the spectrum. After the end of the war, using the new radar related technology, the scientists developed the radio telescopes to record the first radio images of the galaxy. But only in the 60's, with the advent of the first man made satellites, we began to access the much wider e.m. spectrum, including infrared, UV, X-ray and γ-ray radiation. A similar situation happened with the charged cosmic radiation. Cosmic Rays, discovered by Hess in 1912 [1] using electrometers operated on atmospheric balloons, for about 40 years were the subject of very intense studies. The discovery of a realm of new particles using CR experiments, gave birth to particle physics

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The Anti Matter Spectrometer (AMS-02): a Particle Physics Detector In Space

Cited by 8 publications

References 19 publications

Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes

Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes

Full calculation of clumpiness boost factors for antimatter cosmic rays in the light of ${\Lambda}$CDM N-body simulation results

Spaceborne Experiments

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