ORCID Profile
0000-0002-5401-0744
Current Organisations
Deutsches Elektronen-Synchrotron Standort Zeuthen
,
Institut d'Estudis Espacials
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Publications
The population of TeV pulsar wind nebulae in the H.E.S.S. Galactic Plane Survey
Publisher: EDP Sciences
Date: 04-2018
DOI: 10.1051/0004-6361/201629377
Abstract: The nine-year H.E.S.S. Galactic Plane Survey (HGPS) has yielded the most uniform observation scan of the inner Milky Way in the TeV gamma-ray band to date. The sky maps and source catalogue of the HGPS allow for a systematic study of the population of TeV pulsar wind nebulae found throughout the last decade. To investigate the nature and evolution of pulsar wind nebulae, for the first time we also present several upper limits for regions around pulsars without a detected TeV wind nebula. Our data exhibit a correlation of TeV surface brightness with pulsar spin-down power Ė . This seems to be caused both by an increase of extension with decreasing Ė , and hence with time, compatible with a power law R PWN ( Ė ) ~ Ė −0.65±0.20 , and by a mild decrease of TeV gamma-ray luminosity with decreasing Ė , compatible with L 1−10 TeV ~ Ė 0.59±0.21 . We also find that the offsets of pulsars with respect to the wind nebula centre with ages around 10 kyr are frequently larger than can be plausibly explained by pulsar proper motion and could be due to an asymmetric environment. In the present data, it seems that a large pulsar offset is correlated with a high apparent TeV efficiency L 1−10 TeV ∕ Ė . In addition to 14 HGPS sources considered firmly identified pulsar wind nebulae and 5 additional pulsar wind nebulae taken from literature, we find 10 HGPS sources that are likely TeV pulsar wind nebula candidates. Using a model that subsumes the present common understanding of the very high-energy radiative evolution of pulsar wind nebulae, we find that the trends and variations of the TeV observables and limits can be reproduced to a good level, drawing a consistent picture of present-day TeV data and theory.
Discovery of hard-spectrumγ-ray emission from the BL Lacertae object 1ES 0414+009
Publisher: EDP Sciences
Date: 02-2012
H.E.S.S. Follow-up Observations of GRB 221009A
Publisher: American Astronomical Society
Date: 03-2023
Abstract: GRB 221009A is the brightest gamma-ray burst (GRB) ever detected. To probe the very-high-energy (VHE GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hr after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nights after the initial GRB detection, after applying atmospheric corrections. The combined observations yield an integral energy flux upper limit of Φ UL 95 % = 9.7 × 10 − 12 erg cm − 2 s − 1 above E thr = 650 GeV. The constraints derived from the H.E.S.S. observations complement the available multiwavelength data. The radio to X-ray data are consistent with synchrotron emission from a single electron population, with the peak in the spectral energy distribution occurring above the X-ray band. Compared to the VHE-bright GRB 190829A, the upper limits for GRB 221009A imply a smaller gamma-ray to X-ray flux ratio in the afterglow. Even in the absence of a detection, the H.E.S.S. upper limits thus contribute to the multiwavelength picture of GRB 221009A, effectively ruling out an IC-dominated scenario.
Framing the private land conservation conversation: Strategic framing of the benefits of conservation participation could increase landholder engagement
Publisher: Elsevier BV
Date: 07-2016
ERRATUM: “SEARCH FOR DARK MATTER ANNIHILATION SIGNALS FROM THE FORNAX GALAXY CLUSTER WITH H.E.S.S.” (2012, ApJ, 750, 123)
Publisher: American Astronomical Society
Date: 13-02-2014
H.E.S.S. observations of the Crab during its March 2013 GeV gamma-ray flare
Publisher: EDP Sciences
Date: 02-2014
Observations of 54 Active Galactic Nuclei with the HEGRA system of Cherenkov telescopes
Publisher: EDP Sciences
Date: 22-06-2004
Multiband study of RX J0838−2827 and XMM J083850.4−282759: a new asynchronous magnetic cataclysmic variable and a candidate transitional millisecond pulsar
Publisher: Oxford University Press (OUP)
Date: 11-08-2017
H.E.S.S. constraints on dark matter annihilations towards the sculptor and carina dwarf galaxies
Publisher: Elsevier BV
Date: 03-2011
Search for Photon-Linelike Signatures from Dark Matter Annihilations with H.E.S.S.
Publisher: American Physical Society (APS)
Date: 22-01-2013
Design concepts for the Cherenkov Telescope Array CTA: an advanced facility for ground-based high-energy gamma-ray astronomy
Publisher: Springer Science and Business Media LLC
Date: 23-11-2011
PKS 2005-489 at VHE: four years of monitoring with HESS and simultaneous multi-wavelength observations
Publisher: EDP Sciences
Date: 02-2010
SEARCH FOR DARK MATTER ANNIHILATION SIGNALS FROM THE FORNAX GALAXY CLUSTER WITH H.E.S.S.
Publisher: American Astronomical Society
Date: 24-04-2012
Commissioning and first tests of the MAGIC telescope
Publisher: Elsevier BV
Date: 02-2004
Discovery of TeVγ-ray emission from PKS 0447-439 and derivation of an upper limit on its redshift
Publisher: EDP Sciences
Date: 04-2013
Identification of HESS J1303−631 as a pulsar wind nebula throughγ-ray, X-ray, and radio observations
Publisher: EDP Sciences
Date: 19-11-2012
Search for extendedγ-ray emission around AGN with H.E.S.S. andFermi-LAT
Publisher: EDP Sciences
Date: 02-2014
Upper limits on very-high-energy gamma-ray emission from core-collapse supernovae observed with H.E.S.S.
Publisher: EDP Sciences
Date: 06-2019
DOI: 10.1051/0004-6361/201935242
Abstract: Young core-collapse supernovae with dense-wind progenitors may be able to accelerate cosmic-ray hadrons beyond the knee of the cosmic-ray spectrum, and this may result in measurable gamma-ray emission. We searched for gamma-ray emission from ten supernovae observed with the High Energy Stereoscopic System (H.E.S.S.) within a year of the supernova event. Nine supernovae were observed serendipitously in the H.E.S.S. data collected between December 2003 and December 2014, with exposure times ranging from 1.4 to 53 h. In addition we observed SN 2016adj as a target of opportunity in February 2016 for 13 h. No significant gamma-ray emission has been detected for any of the objects, and upper limits on the TeV gamma-ray flux of the order of ~10 −13 cm −2 s −1 are established, corresponding to upper limits on the luminosities in the range ~2 × 10 39 to ~1 × 10 42 erg s −1 . These values are used to place model-dependent constraints on the mass-loss rates of the progenitor stars, implying upper limits between ~2 × 10 −5 and ~2 × 10 −3 M ⊙ yr −1 under reasonable assumptions on the particle acceleration parameters.
VHEγ-ray emission of PKS 2155–304: spectral and temporal variability
Publisher: EDP Sciences
Date: 09-2010
Multi-wavelength observations of H 2356–309
Publisher: EDP Sciences
Date: 06-2010
A multiwavelength view of the flaring state of PKS 2155-304 in 2006
Publisher: EDP Sciences
Date: 03-2012
HESS J1818–154, a new composite supernova remnant discovered in TeV gamma rays and X-rays
Publisher: EDP Sciences
Date: 02-2014
TeV -ray observations of the young synchrotron-dominated SNRs G1.9+0.3 and G330.2+1.0 with H.E.S.S.
Publisher: Oxford University Press (OUP)
Date: 02-05-2014
DOI: 10.1093/MNRAS/STU459
Revisiting the Westerlund 2 field with the HESS telescope array
Publisher: EDP Sciences
Date: 30-11-2010
HESS J1640-465 - an exceptionally luminous TeV -ray supernova remnant
Publisher: Oxford University Press (OUP)
Date: 11-02-2014
DOI: 10.1093/MNRAS/STU139
Discovery of variable VHEγ-ray emission from the binary system 1FGL J1018.6–5856
Publisher: EDP Sciences
Date: 05-2015
Very high energy γ-ray observations of the binary PSR B1259-63/SS2883 around the 2007 Periastron
Publisher: EDP Sciences
Date: 03-09-2009
TeV gamma-ray observations of SS-433 and a survey of the surrounding field with the HEGRA IACT-System
Publisher: EDP Sciences
Date: 29-07-2005
HESS upper limits on very high energy gamma-ray emission from the microquasar GRS 1915+105
Publisher: EDP Sciences
Date: 04-11-2009
Black hole lightning due to particle acceleration at subhorizon scales
Publisher: American Association for the Advancement of Science (AAAS)
Date: 28-11-2014
Abstract: Supermassive black holes with masses of millions to billions of solar masses are commonly found in the centers of galaxies. Astronomers seek to image jet formation using radio interferometry but still suffer from insufficient angular resolution. An alternative method to resolve small structures is to measure the time variability of their emission. Here we report on gamma-ray observations of the radio galaxy IC 310 obtained with the MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes, revealing variability with doubling time scales faster than 4.8 min. Causality constrains the size of the emission region to be smaller than 20% of the gravitational radius of its central black hole. We suggest that the emission is associated with pulsar-like particle acceleration by the electric field across a magnetospheric gap at the base of the radio jet.
The Crab Nebula and Pulsar between 500 GeV and 80 TeV: Observations with the HEGRA Stereoscopic Air Cerenkov Telescopes
Publisher: American Astronomical Society
Date: 20-10-2004
DOI: 10.1086/423931
A new SNR with TeV shell-type morphology: HESS J1731-347
Publisher: EDP Sciences
Date: 16-06-2011
Constraints on the gamma-ray emission from the cluster-scale AGN outburst in the Hydra A galaxy cluster
Publisher: EDP Sciences
Date: 09-2012
Discovery of VHE emission towards the Carina arm region with the H.E.S.S. telescope array: HESS J1018–589
Publisher: EDP Sciences
Date: 18-04-2012
HESS and Fermi-LAT discovery of γ-rays from the blazar 1ES 1312−423
Publisher: Oxford University Press (OUP)
Date: 08-2013
Search for very-high-energyγ-ray emission from Galactic globular clusters with H.E.S.S.
Publisher: EDP Sciences
Date: 13-02-2013
Erratum: HESS J1640-465 - an exceptionally luminous TeV -ray supernova remnant
Publisher: Oxford University Press (OUP)
Date: 03-06-2014
DOI: 10.1093/MNRAS/STU826
Detection of very-high-energyγ-ray emission from the vicinity of PSR B1706–44 and G 343.1–2.3 with H.E.S.S.
Publisher: EDP Sciences
Date: 17-03-2011
H.E.S.S. discovery of VHEγ-rays from the quasar PKS 1510−089
Publisher: EDP Sciences
Date: 06-2013
Discovery and follow-up studies of the extended, off-plane, VHE gamma-ray source HESS J1507-622
Publisher: EDP Sciences
Date: 30-11-2010
Search for TeV Gamma-ray Emission from GRB 100621A, an extremely bright GRB in X-rays, with H.E.S.S.
Publisher: EDP Sciences
Date: 23-04-2014
Discovery of high and very high-energy emission from the BL Lacertae object SHBL J001355.9–185406
Publisher: EDP Sciences
Date: 06-2013
Measurement of the extragalactic background light imprint on the spectra of the brightest blazars observed with H.E.S.S.
Publisher: EDP Sciences
Date: 15-01-2013
The extended X–ray emission around RRAT J1819–1458
Publisher: Cambridge University Press (CUP)
Date: 08-2012
DOI: 10.1017/S1743921312023800
Abstract: We present new imaging and spectral analysis of the recently discovered extended X–ray emission around the high-magnetic-field rotating radio transient RRAT J1819–1458. We used two Chandra observations, taken on 2008 May 31 and 2011 May 28. The diffuse X–ray emission was detected with a significance of ~19σ in the image obtained by combining the two observations. Long-term spectral variability has not been observed. Possible scenarios for the origin of this diffuse X–ray emission, further detailed in Camero–Arranz et al . (2012), are here discussed.
H.E.S.S. andSuzakuobservations of the Vela X pulsar wind nebula
Publisher: EDP Sciences
Date: 07-2019
DOI: 10.1051/0004-6361/201935458
Abstract: Context. Pulsar wind nebulae (PWNe) represent the most prominent population of Galactic very-high-energy gamma-ray sources and are thought to be an efficient source of leptonic cosmic rays. Vela X is a nearby middle-aged PWN, which shows bright X-ray and TeV gamma-ray emission towards an elongated structure called the cocoon. Aims. Since TeV emission is likely inverse-Compton emission of electrons, predominantly from interactions with the cosmic microwave background, while X-ray emission is synchrotron radiation of the same electrons, we aim to derive the properties of the relativistic particles and of magnetic fields with minimal modelling. Methods. We used data from the Suzaku XIS to derive the spectra from three compact regions in Vela X covering distances from 0.3 to 4 pc from the pulsar along the cocoon. We obtained gamma-ray spectra of the same regions from H.E.S.S. observations and fitted a radiative model to the multi-wavelength spectra. Results. The TeV electron spectra and magnetic field strengths are consistent within the uncertainties for the three regions, with energy densities of the order 10 −12 erg cm −3 . The data indicate the presence of a cutoff in the electron spectrum at energies of ~ 100 TeV and a magnetic field strength of ~6 μ G. Constraints on the presence of turbulent magnetic fields are weak. Conclusions. The pressure of TeV electrons and magnetic fields in the cocoon is dynamically negligible, requiring the presence of another dominant pressure component to balance the pulsar wind at the termination shock. Sub-TeV electrons cannot completely account for the missing pressure, which may be provided either by relativistic ions or from mixing of the ejecta with the pulsar wind. The electron spectra are consistent with expectations from transport scenarios dominated either by advection via the reverse shock or by diffusion, but for the latter the role of radiative losses near the termination shock needs to be further investigated in the light of the measured cutoff energies. Constraints on turbulent magnetic fields and the shape of the electron cutoff can be improved by spectral measurements in the energy range ≳ 10 keV.
Detection of gamma rays from a starburst galaxy
Publisher: American Association for the Advancement of Science (AAAS)
Date: 20-11-2009
Abstract: Cosmic rays are thought to be accelerated in the shock waves produced by supernova explosions and can generate gamma rays when they interact with interstellar particles and radiation. Starburst galaxies, with their increased star formation rates, increased stellar explosion rates, and high densities of gas and radiation fields, are considered to be promising sources of gamma-ray emission. Using the High Energy Stereoscopic System (H.E.S.S) array of telescopes, Acero et al. (p. 1080 , published online 24 September) report the detection of gamma rays from one of the closest starburst galaxies, NGC 253. NGC 253 is a spiral galaxy, similar to our own Galaxy, except that its nucleus is undergoing an episode of intense star formation. The H.E.S.S. findings confirm that cosmic-ray acceleration is indeed efficient in starburst galaxies and open up new ways to understand cosmic-ray acceleration.
Discovery of the VHE gamma-ray source HESS J1832-093 in the vicinity of SNR G22.7-0.2
Publisher: Oxford University Press (OUP)
Date: 18-11-2014
Simultaneous multiwavelength observations of the second exceptional γ-ray flare of PKS 2155-304 in July 2006
Publisher: EDP Sciences
Date: 15-06-2009
A very-high-energy component deep in the γ-ray burst afterglow
Publisher: Springer Science and Business Media LLC
Date: 20-11-2019
DOI: 10.1038/S41586-019-1743-9
Abstract: Gamma-ray bursts (GRBs) are brief flashes of γ-rays and are considered to be the most energetic explosive phenomena in the Universe
Discovery of VHEγ-rays from the BL Lacertae object PKS 0548–322
Publisher: EDP Sciences
Date: 10-2010
Constraints on particle acceleration in SS433/W50 from MAGIC and H.E.S.S. observations
Publisher: EDP Sciences
Date: 04-2018
DOI: 10.1051/0004-6361/201731169
Abstract: Context. The large jet kinetic power and non-thermal processes occurring in the microquasar SS 433 make this source a good candidate for a very high-energy (VHE) gamma-ray emitter. Gamma-ray fluxes above the sensitivity limits of current Cherenkov telescopes have been predicted for both the central X-ray binary system and the interaction regions of SS 433 jets with the surrounding W50 nebula. Non-thermal emission at lower energies has been previously reported, indicating that efficient particle acceleration is taking place in the system. Aim. We explore the capability of SS 433 to emit VHE gamma rays during periods in which the expected flux attenuation due to periodic eclipses ( P orb ~ 13.1 days) and precession of the circumstellar disk ( P pre ~ 162 days) periodically covering the central binary system is expected to be at its minimum. The eastern and western SS 433/W50 interaction regions are also examined using the whole data set available. We aim to constrain some theoretical models previously developed for this system with our observations. Methods. We made use of dedicated observations from the Major Atmospheric Gamma Imaging Cherenkov telescopes (MAGIC) and High Energy Spectroscopic System (H.E.S.S.) of SS 433 taken from 2006 to 2011. These observation were combined for the first time and accounted for a total effective observation time of 16.5 h, which were scheduled considering the expected phases of minimum absorption of the putative VHE emission. Gamma-ray attenuation does not affect the jet/medium interaction regions. In this case, the analysis of a larger data set amounting to ~40–80 h, depending on the region, was employed. Results. No evidence of VHE gamma-ray emission either from the central binary system or from the eastern/western interaction regions was found. Upper limits were computed for the combined data set. Differential fluxes from the central system are found to be ≲ 10 −12 –10 −13 TeV −1 cm −2 s −1 in an energy interval ranging from ~few × 100 GeV to ~few TeV. Integral flux limits down to ~ 10 −12 –10 −13 ph cm −2 s −1 and ~ 10 −13 –10 −14 ph cm −2 s −1 are obtainedat 300 and 800 GeV, respectively. Our results are used to place constraints on the particle acceleration fraction at the inner jetregions and on the physics of the jet/medium interactions. Conclusions. Our findings suggest that the fraction of the jet kinetic power that is transferred to relativistic protons must be relatively small in SS 433, q p ≤ 2.5 × 10 −5 , to explain the lack of TeV and neutrino emission from the central system. At the SS 433/W50 interface, the presence of magnetic fields ≳10 μ G is derived assuming a synchrotron origin for the observed X-ray emission. This also implies the presence of high-energy electrons with E e − up to 50 TeV, preventing an efficient production of gamma-ray fluxes in these interaction regions.
Discovery of VHEγ-ray emission and multi-wavelength observations of the BL Lacertae object 1RXS J101015.9 − 311909
Publisher: EDP Sciences
Date: 06-2012
Very-high-energy gamma-ray emission from the direction of the Galactic globular cluster Terzan 5
Publisher: EDP Sciences
Date: 07-2011
HESS observations of the Carina nebula and its enigmatic colliding wind binary Eta Carinae
Publisher: Oxford University Press (OUP)
Date: 12-06-2012
Constraints on the multi-TeV particle population in the Coma galaxy cluster with HESS observations
Publisher: EDP Sciences
Date: 04-06-2009
Probing the extent of the non-thermal emission from the Vela X region at TeV energies with H.E.S.S.
Publisher: EDP Sciences
Date: 16-11-2012
SPECTRAL ANALYSIS AND INTERPRETATION OF THE γ-RAY EMISSION FROM THE STARBURST GALAXY NGC 253
Publisher: American Astronomical Society
Date: 13-09-2012
Detection of very high energy radiation from HESS J1908+063 confirms the Milagro unidentified source MGRO J1908+06
Publisher: EDP Sciences
Date: 29-04-2009
Flux upper limits for 47 AGN observed with H.E.S.S. in 2004−2011
Publisher: EDP Sciences
Date: 28-03-2014
Discovery of extended VHEγ-ray emission from the vicinity of the young massive stellar cluster Westerlund 1
Publisher: EDP Sciences
Date: 2012
Very high energy gamma-ray observations of the galaxy clusters Abell 496 and Abell 85 with HESS
Publisher: EDP Sciences
Date: 22-12-2008
The extended X-ray emission around RRAT J1819−1458
Publisher: Oxford University Press (OUP)
Date: 04-01-2013
DOI: 10.1093/MNRAS/STS531
Localizing the VHE γ-ray source at the Galactic Centre
Publisher: Oxford University Press (OUP)
Date: 03-2010
Discovery of the source HESS J1356-645 associated with the young and energetic PSR J1357-6429
Publisher: EDP Sciences
Date: 09-2011
Constraints on the emission region of 3C 279 during strong flares in 2014 and 2015 through VHE γ-ray observations with H.E.S.S.
Publisher: EDP Sciences
Date: 07-2019
DOI: 10.1051/0004-6361/201935704
Abstract: The flat spectrum radio quasar 3C 279 is known to exhibit pronounced variability in the high-energy (100 MeV E 100 GeV) γ -ray band, which is continuously monitored with Fermi -LAT. During two periods of high activity in April 2014 and June 2015 target-of-opportunity observations were undertaken with the High Energy Stereoscopic System (H.E.S.S.) in the very-high-energy (VHE, E 100 GeV) γ -ray domain. While the observation in 2014 provides an upper limit, the observation in 2015 results in a signal with 8.7 σ significance above an energy threshold of 66 GeV. No VHE variability was detected during the 2015 observations. The VHE photon spectrum is soft and described by a power-law index of 4.2 ± 0.3. The H.E.S.S. data along with a detailed and contemporaneous multiwavelength data set provide constraints on the physical parameters of the emission region. The minimum distance of the emission region from the central black hole was estimated using two plausible geometries of the broad-line region and three potential intrinsic spectra. The emission region is confidently placed at r ≳ 1.7 × 10 17 cm from the black hole, that is beyond the assumed distance of the broad-line region. Time-dependent leptonic and lepto-hadronic one-zone models were used to describe the evolution of the 2015 flare. Neither model can fully reproduce the observations, despite testing various parameter sets. Furthermore, the H.E.S.S. data were used to derive constraints on Lorentz invariance violation given the large redshift of 3C 279 .
Probing the ATIC peak in the cosmic-ray electron spectrum with H.E.S.S.
Publisher: EDP Sciences
Date: 21-10-2009
H.E.S.S. OBSERVATIONS OF THE GLOBULAR CLUSTERS NGC 6388 AND M15 AND SEARCH FOR A DARK MATTER SIGNAL
Publisher: American Astronomical Society
Date: 08-06-2011
Search for Lorentz Invariance breaking with a likelihood fit of the PKS 2155-304 flare data taken on MJD 53944
Publisher: Elsevier BV
Date: 04-2011
Constraints on axionlike particles with H.E.S.S. from the irregularity of the PKS2155 −
Publisher:
American Physical Society (APS)
Date:
20-11-2013
Publisher: American Physical Society (APS)
Date: 20-11-2013
Observations of 14 young open star clusters with the HEGRA system of Cherenkov telescopes
Publisher: EDP Sciences
Date: 17-07-2006
Discovery of gamma-ray emission from the extragalactic pulsar wind nebula N 157B with H.E.S.S.
Publisher: EDP Sciences
Date: 29-08-2012
The high-energyγ-ray emission of AP Librae
Publisher: EDP Sciences
Date: 10-12-2014
HESS upper limit on the very high energy γ-ray emission from the globular cluster 47 Tucanae
Publisher: EDP Sciences
Date: 25-03-2009
Relationship between Intervention Dose and Outcomes in Living Well with Diabetes—A Randomized Trial of a Telephone-Delivered Lifestyle-Based Weight Loss Intervention
Publisher: SAGE Publications
Date: 11-2015
DOI: 10.4278/AJHP.140206-QUAN-62
Abstract: To examine associations of intervention dose with weight, physical activity, glycemic control, and diet outcomes in a randomized trial of a telephone counseling intervention. Study design was a secondary analysis of intervention group. Study setting was primary care practices in a disadvantaged community in Australia. Participants were adult patients with type 2 diabetes (n = 151). Up to 27 telephone counseling calls were made during 18 months. Intervention dose was assessed as the number of calls completed (in tertile categories). Primary outcomes were weight and HbA1c, and moderate to vigorous intensity physical activity via accelerometer. Secondary outcomes were dietary energy intake and diet quality via a validated questionnaire. Analyses employed were bivariate associations of call completion with sociodemographics, and confounder-adjusted linear mixed models for associations of call completion with outcomes (multiple imputation of missing data). Only previous diagnosis of depression/anxiety had a statistically significant (p= .008) association with call completion. Call completion was significantly associated with weight loss (p .001) but not the other outcomes (p .05). Relative to low call completion, mean weight loss (as a percentage of baseline weight) was greater in the high–call completion group by −3.3% (95% confidence interval, −5.0% to −1.5%). Increased dose of intervention was associated with greater weight loss. More needs to be done to retain patients for the duration of weight loss and behavior change interventions, particularly those with diabetes and comorbid depression, who were the most difficult to engage.
DISCOVERY OF VERY HIGH ENERGY γ-RAY EMISSION FROM CENTAURUS A WITH H.E.S.S.
Publisher: American Astronomical Society
Date: 19-03-2009
Spectrum and variability of the Galactic center VHE γ-ray source HESS J1745-290
Publisher: EDP Sciences
Date: 02-07-2009
H.E.S.S. observations of the binary system PSR B1259-63/LS 2883 around the 2010/2011 periastron passage
Publisher: EDP Sciences
Date: 03-2013
First detection of VHEγ-rays from SN 1006 by HESS
Publisher: EDP Sciences
Date: 06-2010
Search for a Dark Matter Annihilation Signal from the Galactic Center Halo with H.E.S.S.
Publisher: American Physical Society (APS)
Date: 18-04-2011
Discovery of very high energyγ-ray emission from the BL Lacertae object PKS 0301−243 with H.E.S.S.
Publisher: EDP Sciences
Date: 11-2013
Observation of the Monoceros Loop SNR region with the HEGRA system of IACTs
Publisher: EDP Sciences
Date: 26-03-2004
HESS J1943+213: a candidate extreme BL Lacertae object
Publisher: EDP Sciences
Date: 30-03-2011
Related Organisations
University Of Aberdeen
Location: United Kingdom of Great Britain and Northern Ireland
Related Funding Activities
No related grants have been discovered for Emma de Ona Wilhelmi.