Prof. Dr. David Berge
Profil
Forschungsthemen6
Beiträge der Humboldt-Universität zu Berlin zu einer erfolgreichen Inbetriebnahme des CTA-Observatoriums
Quelle ↗Förderer: Bundesministerium für Forschung, Technologie und Raumfahrt Zeitraum: 07/2020 - 06/2023 Projektleitung: Prof. Dr. David Berge
Eingrenzung von Modellen für hadronische Wechselwirkungen unter kombinierter Verwendung von Daten des LHC und atmosphärischer Teilchenschauer
Quelle ↗Förderer: DFG Sachbeihilfe Zeitraum: 02/2025 - 02/2028 Projektleitung: Ph. D. Robert Daniel Parsons, Prof. Dr. David Berge
Experimentelle und theoretische Untersuchungen zu schweren Quarks und zu möglichen Erweiterungen des Standardmodells im Rahmen des ATLAS-Experiments
Quelle ↗Förderer: Bundesministerium für Forschung, Technologie und Raumfahrt Zeitraum: 01/2019 - 06/2021 Projektleitung: Prof. Dr. David Berge
Helmholtz-Weizmann International Research School for Multimessenger Astronomy
Quelle ↗Förderer: Helmholtz-Gemeinschaft Zeitraum: 02/2019 - 12/2025 Projektleitung: Prof. Dr. David Berge
MeVCube - eine neuartige Compton Kamera zur Messung von Gammastrahlung fuer astrophysikalische und terrestrische Anwendungen.
Quelle ↗Förderer: DFG Sachbeihilfe Zeitraum: 12/2021 - 12/2024 Projektleitung: Prof. Dr. David Berge
Vorbereitungen für CTA: Beiträge der Humboldt-Universität zu Berlin zur Inbetriebnahme des CTA-Observatoriums
Quelle ↗Förderer: Bundesministerium für Forschung, Technologie und Raumfahrt Zeitraum: 07/2023 - 06/2026 Projektleitung: Prof. Dr. David Berge
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Publikationen25
Top 25 nach Zitationen — Quelle: OpenAlex (BAAI/bge-m3 embedded für Matching).
Astronomy and Astrophysics · 851 Zitationen · DOI
Context.The Crab nebula was observed with the HESS stereoscopic Cherenkov-telescope array between October 2003 and January 2005 for a total of 22.9 h (after data quality selection). This period of time partly overlapped with the commissioning phase of the experiment; observations were made with three operational telescopes in late 2003 and with the complete 4 telescope array in January–February 2004 and October 2004–January 2005.
The Astrophysical Journal · 556 Zitationen · DOI
International audience
Nature · 550 Zitationen · DOI
Nature · 512 Zitationen · DOI
Nature · 496 Zitationen · DOI
Astronomy and Astrophysics · 433 Zitationen · DOI
We present the results of the most comprehensive survey of the Galactic plane in very high-energy (VHE) γ -rays, including a public release of Galactic sky maps, a catalog of VHE sources, and the discovery of 16 new sources of VHE γ -rays. The High Energy Spectroscopic System (H.E.S.S.) Galactic plane survey (HGPS) was a decade-long observation program carried out by the H.E.S.S. I array of Cherenkov telescopes in Namibia from 2004 to 2013. The observations amount to nearly 2700 h of quality-selected data, covering the Galactic plane at longitudes from ℓ = 250° to 65° and latitudes | b |≤ 3°. In addition to the unprecedented spatial coverage, the HGPS also features a relatively high angular resolution (0.08° ≈ 5 arcmin mean point spread function 68% containment radius), sensitivity (≲1.5% Crab flux for point-like sources), and energy range (0.2–100 TeV). We constructed a catalog of VHE γ -ray sources from the HGPS data set with a systematic procedure for both source detection and characterization of morphology and spectrum. We present this likelihood-based method in detail, including the introduction of a model component to account for unresolved, large-scale emission along the Galactic plane. In total, the resulting HGPS catalog contains 78 VHE sources, of which 14 are not reanalyzed here, for example, due to their complex morphology, namely shell-like sources and the Galactic center region. Where possible, we provide a firm identification of the VHE source or plausible associations with sources in other astronomical catalogs. We also studied the characteristics of the VHE sources with source parameter distributions. 16 new sources were previously unknown or unpublished, and we individually discuss their identifications or possible associations. We firmly identified 31 sources as pulsar wind nebulae (PWNe), supernova remnants (SNRs), composite SNRs, or gamma-ray binaries. Among the 47 sources not yet identified, most of them (36) have possible associations with cataloged objects, notably PWNe and energetic pulsars that could power VHE PWNe.
Astronomy and Astrophysics · 408 Zitationen · DOI
We report the detection of a point-like source of very high energy (VHE) -rays coincident within 1 of Sgr A * , obtained with the HESS array of Cherenkov telescopes. The -rays exhibit a power-law energy spectrum with a spectral index of -2.2 0.09 0.15 and a flux above the 165 GeV threshold of (1.82 0.22) 10 -7 m -2 s -1 . The measured flux and spectrum differ substantially from recent results reported in particular by the CANGAROO collaboration.
Astronomy and Astrophysics · 355 Zitationen · DOI
We report the discovery of very-high-energy (VHE) -ray emission of the binary system PSR B1259-63/SS 2883 of a radio pulsar orbiting a massive, luminous Be star in a highly eccentric orbit. The observations around the 2004 periastron passage of the pulsar were performed with the four 13 m Cherenkov telescopes of the HESS experiment, recently installed in Namibia and in full operation since December 2003. Between February and June 2004, a -ray signal from the binary system was detected with a total significance above 13. The flux was found to vary significantly on timescales of days which makes PSR B1259-63 the first variable galactic source of VHE -rays observed so far. Strong emission signals were observed in pre-and post-periastron phases with a flux minimum around periastron, followed by a gradual flux decrease in the months after. The measured time-averaged energy spectrum above a mean threshold energy of 380 GeV can be fitted by a simple power law F 0 (E/1 TeV) - with a photon index = 2.7 0.2 stat 0.2 sys and flux normalisation F 0 = (1.3 0.1 stat 0.3 sys ) 10 -12 TeV -1 cm -2 s -1 . This detection of VHE -rays provides unambiguous evidence for particle acceleration to multi-TeV energies in the binary system. In combination with coeval observations of the X-ray synchrotron emission by the RXTE and INTEGRAL instruments, and assuming the VHE -ray emission to be produced by the inverse Compton mechanism, the magnetic field strength can be directly estimated to be of the order of 1 G.
Astronomy and Astrophysics · 345 Zitationen · DOI
Context.Ground based Cherenkov telescope systems measure astrophysical γ-ray emission against a background of cosmic-ray induced air showers. The subtraction of this background is a major challenge for the extraction of spectra and morphology of γ-ray sources.
Science · 345 Zitationen · DOI
X-ray binaries are composed of a normal star in orbit around a neutron star or stellar-mass black hole. Radio and x-ray observations have led to the presumption that some x-ray binaries called microquasars behave as scaled-down active galactic nuclei. Microquasars have resolved radio emission that is thought to arise from a relativistic outflow akin to active galactic nuclei jets, in which particles can be accelerated to large energies. Very high energy gamma-rays produced by the interactions of these particles have been observed from several active galactic nuclei. Using the High Energy Stereoscopic System, we find evidence for gamma-ray emission of >100 gigaelectron volts from a candidate microquasar, LS 5039, showing that particles are also accelerated to very high energies in these systems.
Astronomy and Astrophysics · 328 Zitationen · DOI
Aims.We present deep HESS observations of the supernova remnant (SNR) RX J1713.7-3946. Combining data of three years – from 2003 to 2005 – we obtain significantly increased statistics and energy coverage as compared to earlier 2003 and 2004 results.
Astronomy and Astrophysics · 313 Zitationen · DOI
Aims.We present results from deep observations of the Galactic shell-type supernova remnant (SNR) RX J1713.7-3946 (also known as G347.3-0.5) conducted with the complete HESS array in 2004.Methods.Detailed morphological and spatially resolved spectral studies reveal the very-high-energy (VHE – Energies GeV) gamma-ray aspects of this object with unprecedented precision. Since this is the first in-depth analysis of an extended VHE gamma-ray source, we present a thorough discussion of our methodology and investigations of possible sources of systematic errors.Results.Gamma rays are detected throughout the whole SNR. The emission is found to resemble a shell structure with increased fluxes from the western and northwestern parts. The differential gamma-ray spectrum of the whole SNR is measured over more than two orders of magnitude, from 190 GeV to 40 TeV, and is rather hard with indications for a deviation from a pure power law at high energies. Spectra have also been determined for spatially separated regions of RX J1713.7-3946. The flux values vary by more than a factor of two, but no significant change in spectral shape is found. There is a striking correlation between the X-ray and the gamma-ray image. Radial profiles in both wavelength regimes reveal the same shape almost everywhere in the region of the SNR.Conclusions.The VHE gamma-ray emission of RX J1713.7-3946 is phenomenologically discussed for two scenarios, one where the gamma rays are produced by VHE electrons via Inverse Compton scattering and one where the gamma rays are due to neutral pion decay from proton-proton interactions. In conjunction with multi-wavelength considerations, the latter case is favoured. However, no decisive conclusions can yet be drawn regarding the parent particle population dominantly responsible for the gamma-ray emission from RX J1713.7-3946.
Physical Review Letters · 308 Zitationen · DOI
The inner region of the Milky Way halo harbors a large amount of dark matter (DM). Given its proximity, it is one of the most promising targets to look for DM. We report on a search for the annihilations of DM particles using γ-ray observations towards the inner 300 pc of the Milky Way, with the H.E.S.S. array of ground-based Cherenkov telescopes. The analysis is based on a 2D maximum likelihood method using Galactic Center (GC) data accumulated by H.E.S.S. over the last 10 years (2004-2014), and does not show any significant γ-ray signal above background. Assuming Einasto and Navarro-Frenk-White DM density profiles at the GC, we derive upper limits on the annihilation cross section ⟨σv⟩. These constraints are the strongest obtained so far in the TeV DM mass range and improve upon previous limits by a factor 5. For the Einasto profile, the constraints reach ⟨σv⟩ values of 6×10^{-26} cm^{3} s^{-1} in the W^{+}W^{-} channel for a DM particle mass of 1.5 TeV, and 2×10^{-26} cm^{3} s^{-1} in the τ^{+}τ^{-} channel for a 1 TeV mass. For the first time, ground-based γ-ray observations have reached sufficient sensitivity to probe ⟨σv⟩ values expected from the thermal relic density for TeV DM particles.
Science · 287 Zitationen · DOI
Very high energy gamma-rays probe the long-standing mystery of the origin of cosmic rays. Produced in the interactions of accelerated particles in astrophysical objects, they can be used to image cosmic particle accelerators. A first sensitive survey of the inner part of the Milky Way with the High Energy Stereoscopic System (HESS) reveals a population of eight previously unknown firmly detected sources of very high energy gamma-rays. At least two have no known radio or x-ray counterpart and may be representative of a new class of "dark" nucleonic cosmic ray sources.
Astronomy and Astrophysics · 281 Zitationen · DOI
Aims. Observations of shell-type supernova remnants (SNRs) in the GeV to multi-TeV γ-ray band, coupled with those at millimetre radio wavelengths, are motivated by the search for cosmic-ray accelerators in our Galaxy. The old-age mixed-morphology SNR W 28 (distance ~2 kpc) is a prime target due to its interaction with molecular clouds along its northeastern boundary and other clouds situated nearby.
3.9 day orbital modulation in the TeV <i>γ</i>-ray flux and spectrum from the X-ray binary LS 5039
2006Astronomy and Astrophysics · 261 Zitationen · DOI
Aims. LS 5039 is a High Mass X-ray Binary (HMXRB) comprising a compact object in an eccentric 3.9 day orbit around a massive O6.5V star. Observations at energies above 0.1 TeV (1011 eV) by the High Energy Stereoscopic System (HESS) in 2004 revealed that LS 5039 is a source of Very High Energy (VHE) γ-rays and hence, is able to accelerate particles to multi-TeV energies. Deeper observations by HESS were carried out in 2005 in an effort to probe further the high energy astrophysics taking place. In particular, we have searched for orbital modulation of the VHE γ-ray flux, which if detected, would yield new information about the complex variation in γ-ray absorption and production within X-ray binary systems.
Physical Review Letters · 212 Zitationen · DOI
The detection of gamma rays from the source HESS J1745-290 in the Galactic Center (GC) region with the High Energy Spectroscopic System (HESS) array of Cherenkov telescopes in 2004 is presented. After subtraction of the diffuse gamma-ray emission from the GC ridge, the source is compatible with a point source with spatial extent less than 1.2;{'}(stat) (95% C.L.). The measured energy spectrum above 160 GeV is compatible with a power law with photon index of 2.25+/-0.04(stat)+/-0.10(syst) and no significant flux variation is detected. It is finally found that the bulk of the very high energy emission must have non-dark-matter origin.
Astronomy and Astrophysics · 195 Zitationen · DOI
The Vela supernova remnant (SNR) is a complex region containing a number of sources of non-thermal radiation. The inner section of this SNR, within 2 degrees of the pulsar PSR B0833-45, has been observed by the HESS γ-ray atmospheric Cherenkov detector in 2004 and 2005. A strong signal is seen from an extended region to the south of the pulsar, within an integration region of radius around the position (, J2000.0). The excess coincides with a region of hard X-ray emission seen by the ROSAT and ASCA satellites. The observed energy spectrum of the source between 550 GeV and 65 TeV is well fit by a power law function with photon index and an exponential cutoff at an energy of TeV. The integral flux above 1 TeV is . This result is the first clear measurement of a peak in the spectral energy distribution from a VHE γ-ray source, likely related to inverse Compton emission. A fit of an Inverse Compton model to the HESS spectral energy distribution gives a total energy in non-thermal electrons of ~ erg between 5 TeV and 100 TeV, assuming a distance of 290 parsec to the pulsar. The best fit electron power law index is 2.0, with a spectral break at 67 TeV.
The Astrophysical Journal · 188 Zitationen · DOI
The shell-type supernova remnant RX J0852.0-4622 was observed with the High Energy Stereoscopic System (H.E.S.S.) of atmospheric Cerenkov telescopes between 2004 December and 2005 May for a total observation time of 33 hr, above an average gamma-ray energy threshold of 250 GeV. The angular resolution of ∼0.06° (for events triggering three or four telescopes) and the large field of view of H.E.S.S. (5° diameter) are well adapted to studying the morphology of the object in very high energy gamma rays, which exhibits a remarkably thin shell very similar to the features observed in the radio range and in X-rays. The spectral analysis of the source from 300 GeV to 20 TeV is also presented. Finally, the possible origins of the very high energy gamma-ray emission (inverse Compton scattering by electrons or the decay of neutral pions produced by proton interactions) are discussed, on the basis of morphological and spectral features obtained at different wavelengths. © 2007. The American Astronomical Society. All rights reserved.
Astronomy and Astrophysics · 186 Zitationen · DOI
Aims.We present results from deep γ-ray observations of the Galactic pulsar wind nebula HESS J1825–137 performed with the HESS array.
Astronomy and Astrophysics · 184 Zitationen · DOI
We report the detection of TeV -rays from the shell-type supernova remnant RX J0852.0-4622 with data of 3.2 h of live time recorded with HESS in February 2004. An excess of (700 60) events from the whole remnant with a significance of 12 was found. The observed emission region is clearly extended with a radius of the order of 1 and the spatial distribution of the signal correlates with X-ray observations. The spectrum in the energy range between 500 GeV and 15 TeV is well described by a power law with a photon index of = 2.1 0.1 stat 0.2 syst and a differential flux at 1 TeV of 1 TeV = (2.1 0.2 stat 0.6 syst ) 10 -11 cm -2 s -1 TeV -1 . The integral flux above 1 TeV was measured to be (E > 1 TeV) = (1.9 0.3 stat 0.6 syst ) 10 -11 cm -2 s -1 , which is at the level of the flux of the Crab nebula at these energies. More data are needed to draw firm conclusions on the magnetic field in the remnant and the type of the particle population creating the TeV -rays.
Astronomy and Astrophysics · 155 Zitationen · DOI
The high-frequency peaked BL Lac PKS 2155-304 at redshift z=0.117 has been detected with high significance (~45sigma) at energies greater than 160 GeV, using the H.E.S.S. stereoscopic array of imaging air-Cherenkov telescopes in Namibia. A strong signal is found in each of the data sets corresponding to the dark periods of July and October, 2002, and June-September, 2003. The observed flux of VHE gamma rays shows variability on time scales of months, days, and hours. The monthly-averaged integral flux above 300 GeV varies between 10% and 60% of the flux observed from the Crab Nebula. Energy spectra are measured for these individual periods of data taking and are characterized by a steep power law with a time-averaged photon index of Gamma=3.32±0.06. An improved chi2 per degree of freedom is found when either a power law with an exponential cutoff energy or a broken power law are fit to the time-averaged energy spectrum. However, the significance of the improvement is marginal (~2sigma). The suggested presence of features in the energy spectrum may be intrinsic to the emission from the blazar, or an indication of absorption of TeV gamma rays by the extragalactic infrared background light
Physical Review Letters · 144 Zitationen · DOI
Spectral lines are among the most powerful signatures for dark matter (DM) annihilation searches in very-high-energy γ rays. The central region of the Milky Way halo is one of the most promising targets given its large amount of DM and proximity to Earth. We report on a search for a monoenergetic spectral line from self-annihilations of DM particles in the energy range from 300 GeV to 70 TeV using a two-dimensional maximum likelihood method taking advantage of both the spectral and spatial features of the signal versus background. The analysis makes use of Galactic center observations accumulated over ten years (2004-2014) with the H.E.S.S. array of ground-based Cherenkov telescopes. No significant γ-ray excess above the background is found. We derive upper limits on the annihilation cross section ⟨σv⟩ for monoenergetic DM lines at the level of 4×10^{-28} cm^{3} s^{-1} at 1 TeV, assuming an Einasto DM profile for the Milky Way halo. For a DM mass of 1 TeV, they improve over the previous ones by a factor of 6. The present constraints are the strongest obtained so far for DM particles in the mass range 300 GeV-70 TeV. Ground-based γ-ray observations have reached sufficient sensitivity to explore relevant velocity-averaged cross sections for DM annihilation into two γ-ray photons at the level expected from the thermal relic density for TeV DM particles.
Astroparticle Physics · 139 Zitationen · DOI
Astronomy and Astrophysics · 137 Zitationen · DOI
Context.The blazar 1ES 1101-232 was observed with the High Energy Stereoscopic System (HESS) of Atmospheric Cherenkov Telescopes (ACT) in 2004 and 2005, for a live time of 43 h. VHE (E > 1011 eV) γ-rays were detected for the first time from this object.
Kooperationen8
Bestätigte Forscher↔Partner-Paare aus HU-FIS — Gold-Standard-Positive für das Matching.
MeVCube - eine neuartige Compton Kamera zur Messung von Gammastrahlung fuer astrophysikalische und terrestrische Anwendungen.
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Vorbereitungen für CTA: Beiträge der Humboldt-Universität zu Berlin zur Inbetriebnahme des CTA-Observatoriums
university
Vorbereitungen für CTA: Beiträge der Humboldt-Universität zu Berlin zur Inbetriebnahme des CTA-Observatoriums
university
Vorbereitungen für CTA: Beiträge der Humboldt-Universität zu Berlin zur Inbetriebnahme des CTA-Observatoriums
university
Vorbereitungen für CTA: Beiträge der Humboldt-Universität zu Berlin zur Inbetriebnahme des CTA-Observatoriums
university
Vorbereitungen für CTA: Beiträge der Humboldt-Universität zu Berlin zur Inbetriebnahme des CTA-Observatoriums
university
Vorbereitungen für CTA: Beiträge der Humboldt-Universität zu Berlin zur Inbetriebnahme des CTA-Observatoriums
university
Vorbereitungen für CTA: Beiträge der Humboldt-Universität zu Berlin zur Inbetriebnahme des CTA-Observatoriums
university
Stammdaten
Identität, Organisation und Kontakt aus HU-FIS.
- Name
- Prof. Dr. David Berge
- Titel
- Prof. Dr.
- Fakultät
- Mathematisch-Naturwissenschaftliche Fakultät
- Institut
- Institut für Physik
- Arbeitsgruppe
- Experimentelle Teilchen- und Astroteilchenphysik (S)
- Telefon
- +49 +49 33762-77291
- HU-FIS-Profil
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- 26.4.2026, 01:02:37