Probing the ATIC peak in the cosmic-ray electron spectrum with H.E.S.S.

Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Almeida, U. Barres de; Bazer‐Bachi, A. R.; Becherini, Y.; Behera, B.; Bernlöhr, K.; Bochow, A.; Boisson, C.; Bolmont, J.; Borrel, V.; Brucker, J.; Brun, F.; Brun, P.; Bühler, R.; Bulik, T.; Büsching, I.; Boutelier, T.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C. G.; Cheesebrough, A.; Chounet, L.‐M.; Coignet, G.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; Dickinson, H. J.; Djannati‐Ataï, A.; Domainko, W.; Drury, L. O’c.; Dubois, F.; Dubus, G.; Dyks, J.; Dyrda, M.; Egberts, K.; Emmanoulopoulos, D.; Espigat, P.; Farnier, C.; Feinstein, F.; Fiaßon, A.; Förster, A.; Fontaine, G.; Fusling, M.; Gabici, S.; Gallant, Y. A.; Gérard, L.; Gerbig, D.; Giebels, B.; Glicenstein, J.-F.; Glück, B.; Goret, P.; Göring, D.; Hauser, D.; Hauser, M.; Heinz, Sebastian; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Holleran, M.; Hoppe, S.; Horns, D.; Jachołkowska, A.; Jager, O. C. de; Jahn, C.; Jung, I.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Kendziorra, E.; Kerschhaggl, M.; Khangulyan, D.; Khélifi, B.; Keogh, D.; Kluźniak, W.; Kneiske, T.; Komin, Nu.; Kosack, K.; Kossakowski, R.; Lamanna, G.; Lenain, J.‐P.; Löhse, T.; Marandon, V.; Martin, Jean‐Michel; Martineau‐Huynh, O.; Marcowith, A.; Masbou, J.; Maurin, D.; McComb, T. J. L.; Medina, M. C.; Moderski, R.; Moulin, Emmanuel; Naumann-Godó, M.; Naurois, M. de; Nedbal, D.; Nekrassov, D.; Nicholas, B.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Olive, J.‐F.; ̃na, E. de O; Orford, K. J.; Ostrowski, M.; Panter, M.; Arribas, M. Paz; Pedaletti, G.; Pelletier, G.; Petrucci, P.-O.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raubenheimer, Britt; Raue, M.; Rayner, S. M.; Reimer, O.; Renaud, M.; Rieger, F.; Ripken, J.; Rob, L.; Rosier‐Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; ̈ock, F.M. Sch; Schröder, R.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Skilton, J. L.; Sol, H.; Spangler, D.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Superina, G.; Szostek, A.; Tam, P. H. T.; Tavernet, J.‐P.; Terrier, R.; Tibolla, O.; Tluczykont, M.; Eldik, C. van; Vasileiadis, G.; Venter, C.; Venter, L.; Vialle, J. P.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Wagner, S. J.; Ward, M. J.; Zdziarski, A. A.; Zech, A.

doi:10.1051/0004-6361/200913323

Cited by 448 publications

(378 citation statements)

References 14 publications

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“…(Aharonian et al 2008(Aharonian et al , 2009, Fermi-LAT (Abdo et al 2009b;Ackermann et al 2010), PAMELA (Adriani et al 2011). The data are taken from the CR database described in 13 .…”

Section: Electron and Positron Datamentioning

confidence: 99%

The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements

Strong

Orlando

Jaffe

2011

A&A

195

249

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Aims. We exploit synchrotron radiation to constrain the low-energy interstellar electron spectrum, using various radio surveys and connecting with electron data from Fermi-LAT and other experiments. Methods. The GALPROP programme for cosmic-ray propagation, gamma-ray and synchrotron radiation is used. Secondary electrons and positrons are included. Propagation models based on cosmic-ray and gamma-ray data are tested against synchrotron data from 22 MHz to 94 GHz. Results. The synchrotron data confirm the need for a low-energy break in the cosmic-ray electron injection spectrum. The interstellar spectrum below a few GeV has to be lower than standard models predict, and this suggests less solar modulation than usually assumed. Reacceleration models are more difficult to reconcile with the synchrotron constraints. We show that secondary leptons are important for the interpretation of synchrotron emission. We also consider a cosmic-ray propagation origin for the low-energy break. Conclusions. Exploiting the complementary information on cosmic rays and synchrotron gives unique and essential constraints on electrons, and has implications for gamma rays. This connection is especially relevant now in view of the ongoing Planck and Fermi missions.

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“…(Aharonian et al 2008(Aharonian et al , 2009, Fermi-LAT (Abdo et al 2009b;Ackermann et al 2010), PAMELA (Adriani et al 2011). The data are taken from the CR database described in 13 .…”

Section: Electron and Positron Datamentioning

confidence: 99%

The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements

Strong

Orlando

Jaffe

2011

A&A

195

249

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“…Decay Over the last couple of years, a lot of attention has been given to the decaying DM as a possible explanation of the flux excesses of high-energy positrons and electrons measured by PAMELA [50], Fermi -LAT [51], H.E.S.S [52] and AMS-02 [53]. The needed DM particle lifetime in such a case, τ χ > 10 26 s, is much longer than the age of the Universe, so that the slow decay does not significantly reduce the overall DM abundance and, therefore, there is no contradiction with the astrophysical and cosmological observations.…”

Section: Secondary Photons From Final State Standard Model Particlesmentioning

confidence: 99%

Optimized Dark Matter Searches in Deep Observations of Segue 1 with MAGIC

Aleksić

2016

Springer Theses

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Abstract. We present the results of stereoscopic observations of the satellite galaxy Segue 1 with the MAGIC Telescopes, carried out between 2011 and 2013. With almost 160 hours of good-quality data, this is the deepest observational campaign on any dwarf galaxy performed so far in the very high energy range of the electromagnetic spectrum. We search this large data sample for signals of dark matter particles in the mass range between 100 GeV and 20 TeV. For this we use the full likelihood analysis method, which provides optimal sensitivity to characteristic gamma-ray spectral features, like those expected from dark matter annihilation or decay. In particular, we focus our search on gamma-rays produced from different final state Standard Model particles, annihilation with internal bremsstrahlung, monochromatic lines and box-shaped signals. Our results represent the most stringent constraints to the annihilation cross-section or decay lifetime obtained from observations of satellite galaxies, for masses above few hundred GeV. In particular, our strongest limit (95% confidence level) corresponds to a ∼500 GeV dark matter particle annihilating into τ + τ − , and is of order σ ann v ≃ 1.2×10 −24 cm 3 s −1 -a factor ∼40 above the σ ann v thermal value.

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“…Both Fermi ) and H.E.S.S. (Aharonian et al 2008(Aharonian et al , 2009) have measured the cosmic ray e − + e + spectrum. Unlike Fermi/LAT, the telescopes from H.E.S.S.…”

Section: Cross Calibration Of Iacts and Fermimentioning

confidence: 99%

The Crab Nebula as a standard candle in very high-energy astrophysics

Meyer

Horns

Zechlin

2010

A&A

Self Cite

207

212

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The continuum high-energy gamma-ray emission between 1 GeV and 10 5 GeV from the Crab Nebula has been measured for the first time in overlapping energy bands by the Fermi large-area telescope (Fermi/LAT) below ≈100 GeV and by ground-based imaging air Cherenkov telescopes (IACTs) above ≈60 GeV. To follow up on the phenomenological approach suggested by Hillas et al. (1998), the broad band spectral and spatial measurement (from radio to low-energy gamma-rays <1 GeV) is used to extract the shape of the electron spectrum. While this model per construction provides an excellent description of the data at energies <1 GeV, the predicted inverse Compton component matches the combined Fermi/LAT and IACT measurements remarkably well after including all relevant seed photon fields and fitting the average magnetic field to B = (124 ± 6 (stat.) +15 −6 (sys.)) μG. The close match of the resulting broad band inverse Compton component with the combined Fermi/LAT and IACTs data is used to derive instrument specific energy-calibration factors. These factors can be used to combine data from Fermi/LAT and IACTs without suffering from systematic uncertainties on the common energy scale. As a first application of the cross calibration, we derive an upper limit to the diffuse gamma-ray emission between 250 GeV and 1 TeV based upon the combined measurements of Fermi/LAT and the H.E.S.S. groundbased Cherenkov telescopes. Finally, the predictions of the magneto-hydrodynamic flow model of Kennel & Coroniti (1984) are compared to the measured SED.

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Probing the ATIC peak in the cosmic-ray electron spectrum with H.E.S.S.

Cited by 448 publications

References 14 publications

The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements

The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements

Optimized Dark Matter Searches in Deep Observations of Segue 1 with MAGIC

The Crab Nebula as a standard candle in very high-energy astrophysics

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