Relevant bibliographies by topics / TeV gamma ray astrophysics

Academic literature on the topic 'TeV gamma ray astrophysics'

Author: Grafiati
Published: 10 December 2022
Last updated: 29 January 2023

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Journal articles on the topic "TeV gamma ray astrophysics"

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SINNIS, GUS. "TeV ASTROPHYSICS WITH THE MILAGRO AND HAWC OBSERVATORIES." International Journal of Modern Physics D 22, no. 11 (September 2013): 1360010. http://dx.doi.org/10.1142/s0218271813600109.

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Ground-based gamma-ray astronomy has historically implemented two dramatically different techniques. One method employs Imaging Atmospheric Cherenkov Telescope(s) (IACT) that detect the Cherenkov light generated in the atmosphere by extensive air showers. The other method employs particle detectors that directly detect the particles that reach ground level — known as Extensive Air Shower (EAS) arrays. Until recently, the IACT method had been the only technique to yield solid detections of TeV gamma-ray sources. Utilizing water Chernkov technology, Milagro, was the first EAS array to discover new gamma-ray sources and demonstrated the power of and need for an all-sky high duty cycle instrument in the TeV energy regime. The transient nature of many TeV sources, the enormous number of potential sources, and the existence of TeV sources that encompass large angular areas all point to the need for an all-sky, high duty-factor instrument with even greater sensitivity than Milagro. The High Altitude Water Cherenkov (HAWC) Observatory will be over an order of magnitude more sensitive than Milagro. In this paper we will discuss the results from Milagro and the design of the HAWC instrument and its experimental sensitivity.
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Cui, Wei. "TeV gamma-ray astronomy." Research in Astronomy and Astrophysics 9, no. 8 (July 24, 2009): 841–60. http://dx.doi.org/10.1088/1674-4527/9/8/001.

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Tanimori, Toru. "Sub-TeV Gamma-Ray Astrophysics Using Large Air Čerenkov Telescopes." Progress of Theoretical Physics Supplement 143 (2001): 78–98. http://dx.doi.org/10.1143/ptps.143.78.

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Dubus, Guillaume, Nicolas Guillard, Pierre-Olivier Petrucci, and Pierrick Martin. "Sizing up the population of gamma-ray binaries." Astronomy & Astrophysics 608 (December 2017): A59. http://dx.doi.org/10.1051/0004-6361/201731084.

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Context. Gamma-ray binaries are thought to be composed of a young pulsar in orbit around a massive O or Be star with their gamma-ray emission powered by pulsar spin-down. The number of such systems in our Galaxy is not known. Aims. We aim to estimate the total number of gamma-ray binaries in our Galaxy and to evaluate the prospects for new detections in the GeV and TeV energy range, taking into account that their gamma-ray emission is modulated on the orbital period. Methods. We modelled the population of gamma-ray binaries and evaluated the fraction of detected systems in surveys with the Fermi-LAT (GeV), H.E.S.S., HAWC and CTA (TeV) using observation-based and synthetic template light curves. Results. The detected fraction depends more on the orbit-average flux than on the light-curve shape. Our best estimate for the number of gamma-ray binaries is 101\hbox{$_{-52}^{+89}$} systems. A handful of discoveries are expected by pursuing the Fermi-LAT survey. Discoveries in TeV surveys are less likely. However, this depends on the relative amounts of power emitted in GeV and TeV domains. There could be as many as ≈ 200 HESS J0632+057-like systems with a high ratio of TeV to GeV emission compared to other gamma-ray binaries. Statistics allow for as many as three discoveries in five years of HAWC observations and five discoveries in the first two years of the CTA Galactic Plane survey. Conclusions. We favour continued Fermi-LAT observations over ground-based TeV surveys to find new gamma-ray binaries. Gamma-ray observations are most sensitive to short orbital period systems with a high spin-down pulsar power. Radio pulsar surveys (SKA) are likely to be more efficient in detecting long orbital period systems, providing a complementary probe into the gamma-ray binary population.
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Noda, Koji, and Robert Daniel Parsons. "Gamma-Ray Bursts at TeV Energies: Observational Status." Galaxies 10, no. 1 (January 5, 2022): 7. http://dx.doi.org/10.3390/galaxies10010007.

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Gamma-ray bursts (GRBs) are some of the most energetic events in the Universe and are potential sites of cosmic ray acceleration up to the highest energies. GRBs have therefore been a target of interest for very high energy gamma-ray observatories for many years, leading to the recent discovery of a number of bursts with photons reaching energies above 100 GeV. We summarize the GRB observational campaigns of the current generation of very high energy gamma-ray observatories as well as describing the observations and properties of the GRBs discovered so far. We compare the properties of the very high energy bursts to the total GRB distribution and make predictions for the next generation of very high energy gamma-ray observations.
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Neronov, A., and D. Semikoz. "Galactic diffuse gamma-ray emission at TeV energy." Astronomy & Astrophysics 633 (January 2020): A94. http://dx.doi.org/10.1051/0004-6361/201936368.

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Context. Measuring the diffuse Galactic γ-ray flux in the TeV range is difficult for ground-based γ-ray telescopes because of the residual cosmic-ray background, which is higher than the γ-ray flux by several orders of magnitude. Its detection is also challenging for space-based telescopes because of low signal statistics. Aims. We characterise the diffuse TeV flux from the Galaxy using decade-long exposures of the Fermi Large Area Telescope. Methods. Considering that the level of diffuse Galactic emission in the TeV band approaches the level of residual cosmic-ray background, we estimated the level of residual cosmic-ray background in the SOURCEVETO event selection and verified that the TeV diffuse Galactic emission flux is well above the residual cosmic-ray background up to high Galactic latitude regions. Results. We study spectral and imaging properties of the diffuse TeV signal from the Galactic plane. We find much stronger emission from the inner Galactic plane than in previous HESS telescope estimates (lower bound). We also find a significant difference in the measurement of the Galactic longitude and latitude profiles of the signal measured by Fermi and HESS. These discrepancies are presumably explained by the fact that regions of background estimate in HESS have non-negligible γ-ray flux. Comparing Fermi measurements with those of ARGO-YBJ, we find better agreement, with the notable exception of the Cygnus region, where we find much higher flux (by a factor 1.5). We also measure the TeV diffuse emission spectrum up to high Galactic latitude and show that the spectra of different regions of the sky have spectral slopes consistent with Γ = 2.34 ± 0.04, which is harder than the slope of the locally observed spectrum of cosmic rays with energies 10–100 TeV, which produce TeV diffuse emission on their way through the interstellar medium. We discuss the possible origin of the hard slope of the TeV diffuse emission. Conclusions. Fermi/LAT provides reliable measurements of the diffuse Galactic emission spectrum in the TeV range, which are almost background free at low Galactic latitudes. The diffuse flux becomes comparable to the residual cosmic-ray background at Galactic latitudes |b| > 50°. Its measurement in these regions might suffer from systematic uncertainty stemming from the uncertainty of our phenomenological model of the residual cosmic-ray background in the Pass 8 Fermi/LAT data.
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Huang, Tian-Qi, and Zhuo Li. "Constraints on Hadronic Contributions to LHAASO Sources with Neutrino Observations." Astrophysical Journal 925, no. 1 (January 1, 2022): 85. http://dx.doi.org/10.3847/1538-4357/ac423d.

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Abstract The Large High Altitude Air Shower Observatory (LHAASO) detected 12 gamma-ray sources above 100 TeV, which are the possible origins of Galactic cosmic-rays. We summarize the neutrino measurements by IceCube and ANTARES in the vicinity of LHAASO sources to constrain the contribution of hadronic gamma-rays in these sources. We find that the current observations constrain hadronic gamma-rays to contribute no more than ∼60% of the gamma-rays from the Crab Nebula. Gamma-rays from two LHAASO sources, LHAASO J1825−1326 and LHAASO J1907+0626, are dominated by leptonic components up to ∼200 TeV, under the hypotheses in the analysis by IceCube. The uncertainties of the constraint on the hadronic gamma-ray emission are discussed. We also constrain the total 100 TeV gamma-ray emission from TeV pulsar wind nebulae by relying on the remarkable sensitivity of LHAASO at that energy.
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Shimono, Naoya, Tomonori Totani, and Takahiro Sudoh. "Prospects of newly detecting nearby star-forming galaxies by the Cherenkov Telescope Array." Monthly Notices of the Royal Astronomical Society 506, no. 4 (July 27, 2021): 6212–22. http://dx.doi.org/10.1093/mnras/stab2118.

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ABSTRACT Prospects of the Cherenkov Telescope Array (CTA) for the study of very high energy gamma-ray emission from nearby star-forming galaxies are investigated. In the previous work, we constructed a model to calculate luminosity and energy spectrum of pion-decay gamma-ray emission produced by cosmic ray interaction with the interstellar medium (ISM), from four physical quantities of galaxies [star formation rate (SFR), gas mass, stellar mass, and effective radius]. The model is in good agreement with the observed GeV–TeV emission of several nearby galaxies. Applying this model to nearby galaxies that are not yet detected in TeV (mainly from the KINGFISH catalogue), their hadronic gamma-ray luminosities and spectra are predicted. We identify galaxies of the highest chance of detection by CTA, including NGC 5236, M33, NGC 6946, and IC 342. Concerning gamma-ray spectra, NGC 1482 is particularly interesting because our model predicts that this galaxy is close to the calorimetric limit and its gamma-ray spectral index in GeV–TeV is close to that of cosmic ray protons injected into ISM. Therefore, this galaxy may be detectable by CTA even though its GeV flux is below the Fermi Large Area Telescope sensitivity limit. In the TeV regime, most galaxies are not in the calorimetric limit, and the predicted TeV flux is lower than that assuming a simple relation between the TeV luminosity and SFR of M82 and NGC 253, typically by a factor of 15. This means that a more sophisticated model beyond the calorimetric limit assumption is necessary to study TeV emission from star-forming galaxies.
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Topchiev, N. P., A. M. Galper, I. V. Arkhangelskaja, A. I. Arkhangelskiy, A. V. Bakaldin, I. V. Chernysheva, O. D. Dalkarov, et al. "High-energy gamma- and cosmic-ray observations with future space-based GAMMA-400 gamma-ray telescope." EPJ Web of Conferences 208 (2019): 14004. http://dx.doi.org/10.1051/epjconf/201920814004.

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The future space-based GAMMA-400 gamma-ray telescope will be installed on the Navigator platform of the Russian Astrophysical Observatory. A highly elliptical orbit will provide observations for 7-10 years of many regions of the celestial sphere continuously for a long time (~ 100 days). GAMMA-400 will measure gamma-ray fluxes in the energy range from ~ 20 MeV to several TeV and electron + positron fluxes up to ~ 20 TeV. GAMMA-400 will have an excellent separation of gamma rays from the background of cosmic rays and electrons + positrons from protons and an unprecedented angular (~ 0.01° at Eγ = 100 GeV) and energy (~ 1% at Eγ = 100 GeV) resolutions better than for Fermi-LAT, as well as ground-based facilities, by a factor of 5-10. Observations of GAMMA-400 will provide new fundamental data on discrete sources and spectra of gamma-ray emission and electrons + positrons, as well as the nature of dark matter.
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Carramiñana, Alberto. "Black hole astrophysics with HAWC, the High Altitude Water Cherenkov γ-ray observatory." Proceedings of the International Astronomical Union 12, S324 (September 2016): 309–16. http://dx.doi.org/10.1017/s1743921317002289.

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AbstractThe HAWC gamma-ray observatory is a wide field of view and high duty cycle γ-ray detector investigating the 0.1 - 100 TeV energy range. It has detected supermassive black holes in the near Universe, and is seeking to detect black hole related objects like gamma-ray bursts, Galactic binary systems, primordial black holes and gravitational wave mergers. Daily light curves of the BL Lac objects Mrk 421 and Mrk 501 are presented here, together with a compilation of studies of black hole related objects.
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Dissertations / Theses on the topic "TeV gamma ray astrophysics"

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Bowden, Christopher Charles Geoffrey. "A search for TeV gamma ray emission from X-ray binary stars." Thesis, Durham University, 1993. http://etheses.dur.ac.uk/5631/.

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This work is concerned with the detection of pulsed TeV gamma ray emission from a number of X-ray binary systems by the use of the atmospheric Cerenkov technique. Chapters 1 and 2 give an overview of the development of gamma ray astronomy, with emphasis placed on progress made in the detection of TeV gamma rays by their Cerenkov radiation in the atmosphere. Chapters 3 and 4 describe the University of Durham atmospheric Cerenkov telescopes, which were used to make the observations reported in this work, and the standard data processing and analysis procedures adopted. The main part of the thesis deals with the application of these techniques to observations of five X-ray binaries. After a review of the properties of such objects in Chapter 5, Chapters 6 and 7 deal specifically with the results for two of the systems considered to be among the most likely candidates to give a detectable TeV photon flux; Centaurus X-3 and Vela X-1. A study of all data recorded on Cen X-3 over the course of six years suggests the presence of a weak gamma ray flux pulsed at the X-ray period. Previous reports of stronger emission near the ascending node of the orbit are confirmed here. For Vela X-1, the analysis of a dataset recorded during a single dark moon interval reveals evidence for two short outbursts of pulsed TeV gamma ray emission. Chapter 8 reports the series of observations made of SMC X-1, 4U1626-67 and X0G21-72, and upper limits are placed on the TeV gamma ray emission from each. Finally, the results reported here are compared with the predictions of a number of theoretical models, some of which are found to give good agreement with the limits and detections derived in this work. A discussion of the status of this field and future observational prospects is also given.
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Zhou, Hao. "Search for TeV gamma-ray sources in the galactic plane with the HAWC observatory." Thesis, Michigan Technological University, 2016. http://pqdtopen.proquest.com/#viewpdf?dispub=10004778.

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Cosmic rays, with an energy density of ∼ 1eVcm–3, play an important role in the evolution of our Galaxy. Very high energy (TeV) gamma rays provide unique information about the acceleration sites of Galactic cosmic rays. The High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory is an all-sky surveying instrument sensitive to gamma rays from 100,GeV to 100,TeV with a 2steradian instantaneous field of view and a duty cycle of >95%. The array is located in Sierra Negra, Mexico at an elevation of 4,100m and was inaugurated in March 2015. Thanks to its modular design, science operation began in Summer 2013 with one third of the array. Using this data, a survey of the inner Galaxy region of Galactic longitude l ∈ [+15°, +50°] and latitude b ∈ [–4°, +4°] is performed. To address the ambiguities arising from unresolved sources in the data, a maximum likelihood technique is used to identify point source candidates. Ten sources and candidate sources are identified in this analysis. Eight of these are associated with known TeV sources but not all have differential fluxes compatible with previous measurements. Three sources are detected with significances >5σ after accounting for statistical trials, and are associated with known TeV sources. With data taken with the full array and improved reconstruction algorithms, the significance on the Crab nebula increases from 3.1σ√day to 5.5σ√day, which allows more sensitive sky surveys and more precise spectral and morphological analyses on individual sources.

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Giebels, Berrie. "A contribution to gamma-ray astronomy of GeV-TeV Active Galaxies with Fermi and H.E.S.S." Habilitation à diriger des recherches, Ecole Polytechnique X, 2011. http://tel.archives-ouvertes.fr/tel-00672596.

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L'astronomie des rayons g de haute (E > 100MeV, HE) et de très haute énergie (E 100GeV, VHE) ont effectué des progrès considérables en moins d'une décennie. Le nombre de sources émettrices dans ce régime d'énergie a augmenté de plus d'un ordre de grandeur, de nouvelles classes d'émetteurs ont été découvertes et des nouvelles sous-classes ont été établies basées sur l'émission gamma, et les sources connues sont à présent résolues à des échelles spatiales ou temporelles sans précédent révélant de nouvelles propriétés. Les noyaux actifs de galaxie (AGN) sont l'une des classes d'émetteurs les plus énergétiques, dont le pic de puissance émis dans le spectre électromagnétique peut dans certains cas dépasser la capacité de mesure des instruments actuels, et dont l'investigation requiert la maîtrise simultanée du ciel g HE et VHE qu'apportent les expériences Cerenkov au sol (atmospheric Cerenkov telescope, ou ACT) et le satellite Fermi.
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Gabici, Stefano. "Gamma ray astronomy and the origin of galactic cosmic rays." Habilitation à diriger des recherches, Université Paris-Diderot - Paris VII, 2011. http://tel.archives-ouvertes.fr/tel-00719791.

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Diffusive shock acceleration operating at expanding supernova remnant shells is by far the most popular model for the origin of galactic cosmic rays. Despite the general consensus received by the model, an unambiguous and conclusive proof of the supernova remnant hypothesis is still missing. In this context, the recent developments in gamma ray astronomy provide us with precious insights into the problem of the origin of galactic cosmic rays, since production of gamma rays is expected both during the acceleration of cosmic rays at supernova remnant shocks and during their subsequent propagation in the interstellar medium. In particular, the recent detection of a number of supernova remnants at TeV energies nicely fits with the model, but it still does not constitute a conclusive proof of it, mainly due to the difficulty of disentangling the hadronic and leptonic contributions to the observed gamma ray emission. The main goal of my research is to search for an unambiguous and conclusive observational test for proving (or disproving) the idea that supernova remnants are the sources of galactic cosmic rays with energies up to (at least) the cosmic ray knee. Our present comprehension of the mechanisms of particle acceleration at shocks and of the propagation of cosmic rays in turbulent magnetic fields encourages beliefs that such a conclusive test might come from future observations of supernova remnants and of the Galaxy in the almost unexplored domain of multi-TeV gamma rays.
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Parent, Damien. "Observations de pulsars avec le Fermi Gamma-ray Space Telescope." Phd thesis, Université Sciences et Technologies - Bordeaux I, 2009. http://tel.archives-ouvertes.fr/tel-00461405.

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Le Large Area Telescope à bord du satellite Fermi, lancé le 11 juin 2008, est un télescope spatial observant l'univers des hautes énergies. L'instrument couvre l'intervalle en énergie de 20MeV à 300 GeV avec une sensibilité nettement améliorée et la capacité de localiser des sources ponctuelles. Il détecte les photons gamma par leur conversion en paire électron-positron, et mesure leur direction et leur énergie grâce à un trajectographe et un calorimètre. Cette thèse présente les courbes de lumières et les mesures spectrales résolues en phase des pulsars radio et gamma détectés par le LAT. La mesure des paramètres spectraux (flux, indice spectral, et énergie de coupure) dépend des fonctions de réponse de l'instrument (IRFs). Une méthode développée pour la validation en orbite de la surface ecace est présentée en utilisant le pulsar de Vela. Les efficacités des coupures entre les données du LAT et les données simulées sont comparées à chaque niveau de la rejection du fond. Les résultats de cette analyse sont propagés vers les IRFs pour évaluer les systématiques des mesures spectrales. La dernière partie de cette thèse présente les découvertes de nouveaux pulsars individuels tels que PSR J0205+6449, J2229+6114, et J1048-5832 à partir des données du LAT et des éphémérides radio et X. Des analyses temporelles et spectrales sont investies dans le but de contraindre les modèles d'émission gamma. Finalement, nous discutons les propriétés d'une large population de pulsars gamma détectés par le LAT, incluant les pulsars normaux et les pulsars milliseconde.
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Andersson, Tom. "Inverse Compton gamma-rays from Markarian 421 : A study of GeV and TeV emission from Mrk 421 based on Fermi-LAT and H.E.S.S. data." Thesis, Linnéuniversitetet, Institutionen för fysik och elektroteknik (IFE), 2016. http://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-57861.

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This thesis summarizes a senior project on the Active Galactic Nucleus (AGN) Markarian 421 (Mrk 421). Observations of Gev and TeV flux with Fermi Large Area Telescope (LAT) and High Energy Stereoscopic System (H.E.S.S.) were compared with previous reports and publications of flux analyses of the gamma-ray emission from Mrk 421. Power laws with exponential cutoffs made consistent fits to most SEDs in the GeV and TeV bands.
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Knödlseder, Jürgen. "The origin of 26Al in the Galaxy." Phd thesis, Université Paul Sabatier - Toulouse III, 1997. http://tel.archives-ouvertes.fr/tel-00145359.

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The history of recent galactic nucleosynthesis activity can be studied by
measurements of the 1.809 MeV gamma-ray line arising from the decay of
radioactive 26Al.
The COMPTEL telescope aboard the Compton Gamma-Ray Observatory, launched on
April 5, 1991, permits for the first time an extensive investigation of the
1.8 MeV radiation throughout the entire sky.
The aim of this thesis is to infer the galactic distribution of 26Al from
these measurements and to identify the dominant sources of this
radioactive isotope.

The first part of the thesis is dedicated to the reconstruction of
the 1.8 MeV intensity distribution from the measured data.
It is demonstrated that the use of conventional deconvolution
algorithms, like maximum likelihood or maximum entropy inversion,
leads to lumpy, noise-dominated intensity distributions.
Nevertheless, simulations can help to assess the uncertainties in the
reconstructed images, which permits the scientific exploitation of the
recovered skymaps.
Alternatively, a multiresolution approach is proposed, which largely
reduces the uncertainties in the reconstructed 1.8 MeV intensity
distribution.
In summary, 1.8 MeV emission is mainly concentrated towards the
galactic plane, which clearly demonstrates that the bulk of 26Al is of
galactic rather than local origin.
However, distinct emission features towards Cygnus, Carina, and the
Auriga-Camelopardalis-Perseus region are inconsistent with a smooth
galactic 1.8 MeV emission profile, pointing towards a massive star
origin of 26Al.

The second part of the thesis consists of a multi-wavelength
comparison of COMPTEL 1.8 MeV data which aims in the
identification of the origin of galactic 26Al.
For the comparison, a rigorous Bayesian analysis is applied, which
is the only consistent framework that allows inference based on the
comparison.
It turned out that the 1.8 MeV distribution follows very closely
the distribution of free electrons in the Galaxy which is traced by
thermal bremsstrahlung, observable in the microwave domain.
The similarity of the 1.8 MeV intensity distribution to the
thermal bremsstrahlung distribution implies a direct proportionality
between the 26Al and the massive star column densities, which strongly
supports that massive stars are the origin of galactic 26Al.
In particular, ONeMg-novae and AGB stars can be excluded as dominant
26Al sources since their galactic distribution is not expected to
correlate with the distribution of free electrons.

The correlation between 26Al and free electrons established, the
analysis of 1.8 MeV gamma-ray line emission can complement our knowledge
about star formation and the distribution of ionized gas throughout
the entire Galaxy.
While COMPTEL made the first step in providing the first all-sky map
in the light of the 1.809 MeV line, INTEGRAL, the next generation gamma-ray spectrometer, will allow a detailed study of current star formation
in the Galaxy.
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Rogers, Martin John. "Gamma-ray evidence for cosmic-ray sources." Thesis, Durham University, 1988. http://etheses.dur.ac.uk/6343/.

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The origin of cosmic-rays is one of the long-standing problems in astro physics. In recent years, strong evidence has been found that certain classes of object contain and are able to accelerate particles to high energies. In this thesis the origin problem is addressed in two different ways. Firstly, two different regions of the Galaxy are studied using γ-ray observations from the COSB satellite combined with atomic and molecular gas measurements. The Vela region contains a pulsar and a supernova remnant and is particularly valuable location for cosmic-ray studies because of its proximity, the association of the two objects, and the intensity of the γ -ray flux it produces. At greater longitudes, the region around the peculiar object η Carinae is also studied. It is rich in potential sources of cosmic rays including active stars and a spiral arm seen at a tangent at l ~ 282º .Analysis of the Vela region reveals strong evidence for cosmic ray production at all energies observed by COSB. The supernova remnant seems the most likely candidate, but the possibility of the pulsar itself producing some of the particles cannot be ruled out. The excess γ -ray emission from around η Carinae does not appear correlated with the active stars but seems to becoming predominantly from the spiral arm. This is the first time evidence has been presented for cosmic-ray acceleration by the spiral shock in a particular, known spiral arm which is observed as a feature in the gas. The γ -rays are produced in the gas clouds associated with this arm. The second approach to the cosmic-ray origin problem involves a model for cosmic-ray production in supernova remnants and is used in association with a Monte-Cailo simulation of their occurrence in the Galaxy. Unlike earlier models (Bhat et al 1987), the motion of the Sun is also taken into account and the supernova explosions occur mainly in spiral arms. The results are in the form of a time sequence of energy density values and tire compared in detail with (^10)Be results. It is found that the model accounts for the long-term rise in the concentration of this radioisotope and does not predict large excursions from the mean energy density that beset older models. Thus the cosmic ray production by supernova remnants seems to be consistent with the radioisotope data.
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Zabalza, de Torres Victor. "The keV-TeV connection in gamma-ray binaries." Doctoral thesis, Universitat de Barcelona, 2011. http://hdl.handle.net/10803/33649.

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Gamma-ray binaries are systems that comprise a young, massive star and a compact object that can be either a young pulsar or a black hole. They emit radiation from radio up to tens of TeV and show flux variability along the whole electromagnetic spectrum. For three of the four detected gamma-ray binaries, the nature of the compact object is unknown. In this thesis we present a study of gamma-ray binaries through three approaches that involve the simultaneous study of these sources in X-rays and very high energy (VHE) gamma-rays. We present the discovery of correlated X-ray and VHE gamma-ray emission from LS I +61 303. The correlations indicates that the emission from these two bands could be originated in the same parent particle population, and we explore this idea through the calculation of a radiative model. This model allows us to significantly constrain the physical properties of the non-thermal emitter in LS I +61 303. For those systems where the compact object is a young pulsar, the interaction between the stellar and pulsar winds will give rise to strong shocks. The shocked pulsar wind is the candidate location for non-thermal emission from these systems. The shocked stellar wind should give rise to a thermal X-ray spectrum, but no such features have been detected in the X-ray spectrum of gamma-ray binaries. We present a model of the thermal emission of the shocked stellar wind and use it to constrain the pulsar properties. We have applied this method to two X-ray observations of LS 5039 and have successfully constrained the pulsar spin-down luminosity. Finally, we present a search for VHE emission from Scorpius X-1 through a simultaneous X-ray and VHE gamma-ray campaign. The X-ray observations allowed us to select black-hole states where non-thermal X-ray emission has been detected. We did not find significant VHE emission in any of the black hole states, but the upper limits derived will prove useful in future modelling of the non-thermal emitter in the source.
Les binàries de raigs gamma són sistemes binaries formats per una estrella jove i massiva i un objecte compacte, que pot ser un púlsar jove o un forat negre, que emeten radiació fins a desenes de TeV i mostren variabilitat orbital en totes les bandes d'emissió, des de radio fins a raigs gamma. En el cas de tres de les quatre binàries de raigs gamma detectades avui dia, se'n desconeix la natura de l'objecte compacte. En aquesta tesi presentem un estudi de les binàries de raigs gamma mitjançant tres treballs complementaris que involucren l'estudi simultani d'aquestes fonts en raigs X i raigs gamma de molt alta energia. En primer lloc presentem el descobriment d'emissió en raigs X i raigs gamma de molt alta energia correlades en el temps al sistema LS I +61 303. Aquesta correlació ens indica que l'emissió en les dues bandes pot provenir d'una única població d'electrons, i ho confirmem mitjançant la realització d'un model teòric de radiació que ens permet restringir significativament les propietats físiques de l'emissor no tèrmic de la font. En cas que la font energètica dels sistemes sigui un púlsar, la interacció entre els vents de l'estrella i el púlsar dona lloc a una regió d'interacció on el vent xocat del púlsar accelera partícules i emet des de radio fins a raigs gamma. A l'espectre de raigs X, però, no es detecta l'emissió tèrmica del vent xocat de l'estrella, que s'escalfa fins a desenes de milers de graus. Això ens ha permès estudiar la forma de la regió d'interacció, determinada principalment per la potència del púlsar, i fer un càlcul teòric de l'emissió en raigs X tèrmics. Hem aplicat aquest model al sistema LS 5039 i hem pogut determinar la potència del púlsar, fet important per a la modelització de l'emissió no tèrmica de la font. Finalment, presentem la cerca d'emissió de raigs gamma provinent de sistemes binaris fins ara no detectats. Una campanya simultània en raigs X i raigs gamma ens va permetre seleccionar les dades de molt alta energia del microquàsar Sco X-1 en funció de l'estat d'acreció sobre l'objecte compacte. Tot i no detectar la font en raigs gamma, els límits superiors obtinguts permeten restringir les propietats físiques de Sco X-1 rellevants per a l'emissió en molt alta energia.
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10

Mannings, Vincent. "TeV gamma-ray emission from accreting binary pulsars." Thesis, Durham University, 1990. http://etheses.dur.ac.uk/6297/.

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The high-mass X-ray binary SMC X-1 has been observed during the interval 1986-1989 at a threshold γ-ray energy of 0.4 TeV using the University of Durham Mark III air Cerenkov telescope at Narrabri. The Cerenkov arrival time series recorded during these observations have been tested for periodicity at the contemporary pulse period of the SMC X-1 X-ray pulsar. This period analysis was performed using a new technique - introduced in the present work - which is designed for TeV γ-ray source candidates in binary systems and which simultaneously seeks evidence for pulsed TeV γ-ray emission and information on the location of the emission site within the binary. Results are also presented from the period analysis of data accumulated at Narrabri during observations of the low-mass X-ray binaries X0021.8-7221 (in the globular cluster 47 Tucanae) and GX 1+4. X-ray binaries as a class of TeV γ-ray source are considered and their properties compared. Previous models which invoke the interaction of beams of high-energy particles with material within the environment of a binary system are discussed. One of these models is adapted in the present work in order to propose a simple explanation of the narrow TeV 7-ray orbital light curve observed for the high-mass binary Centaurus X-3. The new model accounts for the γ-ray emission from Cen X-3 in terms of the collisions of ultrarelativistic protons with an accretion wake trailing the X-ray pulsar. This model, which incorporates the steering of charged particles in the magnetosphere of the massive primary star, is also applied to the Vela X-1 binary in order to investigate claims that TeV γ-ray outbursts observed during X-ray eclipse arise at particle collisions with the limb of the supergiant companion.
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Books on the topic "TeV gamma ray astrophysics"

1

Völk, Heinrich J., and Felix A. Aharonian, eds. TeV Gamma-Ray Astrophysics. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1.

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Connaughton, Valerie. Searches for Gamma-Ray Bursts at TeV energies. Dublin: University College Dublin, 1996.

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Gamma-ray bursts. Cambridge: Cambridge University Press, 2012.

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Bambi, Cosimo, and Andrea Santangelo, eds. Handbook of X-ray and Gamma-ray Astrophysics. Singapore: Springer Nature Singapore, 2022. http://dx.doi.org/10.1007/978-981-16-4544-0.

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Lessard, Rodney W. Observations of TeV gamma-rays from supernova remnants. Dublin: University College Dublin, 1996.

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Quinn, John Joseph. The discovery and properties of the TeV gamma-ray emission from Markarian 501. Dublin: University College Dublin, 1997.

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E, Turver K., and North Atlantic Treaty Organization. Scientific Affairs Division., eds. Very high energy gamma ray astronomy. Dordrecht: D. Reidel Pub. Co., 1987.

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Fichtel, Carl E. Gamma-ray astrophysics: New insight into the Universe. 2nd ed. Greenbelt, Md: National Aeronautics and Space Administration, Goddard Space Flight Center, 1997.

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McEnery, Julie E. TeV gamma-ray variability of the BL lacertae object markarian 421. Dublin: University College Dublin, 1997.

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Kahn, Steven Michael. High-energy spectroscopic astrophysics. Berlin: Springer, 2005.

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Book chapters on the topic "TeV gamma ray astrophysics"

1

Hurley, K. "Gamma-Ray Bursts and Very High Energy Gamma-Ray Astronomy." In TeV Gamma-Ray Astrophysics, 43–52. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_4.

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Weekes, Trevor C. "The Atmospheric Cherenkov Technique in Very High Energy Gamma-Ray Astronomy." In TeV Gamma-Ray Astrophysics, 1–15. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_1.

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Bloom, Elliott D. "GLAST." In TeV Gamma-Ray Astrophysics, 109–25. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_10.

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Paré, E. "Gamma-Ray Astronomy: Extension Beyond the GeV Domain by Ground-Based Observations." In TeV Gamma-Ray Astrophysics, 127–36. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_11.

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Fegan, D. J. "The Art and Power of Čerenkov Imaging." In TeV Gamma-Ray Astrophysics, 137–51. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_12.

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Chadwick, P. M., J. E. Dickinson, M. R. Dickinson, N. A. Dipper, J. Holder, T. J. L. McComb, K. J. Orford, et al. "Stereoscopic Measurements of the Čerenkov Radiation Produced by TeV Gamma Rays." In TeV Gamma-Ray Astrophysics, 153–67. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_13.

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Lorenz, E. "Wide Angle Air Cerenkov Detectors." In TeV Gamma-Ray Astrophysics, 169–83. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_14.

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Bernlöhr, Konrad. "Low Threshold Particle Arrays." In TeV Gamma-Ray Astrophysics, 185–97. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_15.

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Yodh, Gaurang B. "Water Cherenkov Detectors:Milagro." In TeV Gamma-Ray Astrophysics, 199–212. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_16.

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Resvanis, L. K. "High Energy Neutrino Telescopes." In TeV Gamma-Ray Astrophysics, 213–34. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0171-1_17.

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Conference papers on the topic "TeV gamma ray astrophysics"

1

Vacanti, G. "Gamma-ray astronomy at 1 TeV." In Particle astrophysics. AIP, 1990. http://dx.doi.org/10.1063/1.39151.

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Lamb, R. C. "GeV gamma-ray sources." In GeV-TeV gamma ray astrophysics workshop. AIP, 2000. http://dx.doi.org/10.1063/1.1291381.

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Chadwick, P. M. "TeV emission from supernovae." In GeV-TeV gamma ray astrophysics workshop. AIP, 2000. http://dx.doi.org/10.1063/1.1291370.

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Yodh, Gaurang B. "Gamma hadron separation in Milagro." In GeV-TeV gamma ray astrophysics workshop. AIP, 2000. http://dx.doi.org/10.1063/1.1291410.

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Chadwick, P. M. "TeV observations of X-ray binaries." In GeV-TeV gamma ray astrophysics workshop. AIP, 2000. http://dx.doi.org/10.1063/1.1291378.

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Mereghetti, S. "The AGILE gamma-ray astronomy mission." In GeV-TeV gamma ray astrophysics workshop. AIP, 2000. http://dx.doi.org/10.1063/1.1291412.

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Rowell, G. P. "The SNR W28 at TeV energies." In GeV-TeV gamma ray astrophysics workshop. AIP, 2000. http://dx.doi.org/10.1063/1.1291366.

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Chadwick, P. M. "TeV emission from PKS 2155−304." In GeV-TeV gamma ray astrophysics workshop. AIP, 2000. http://dx.doi.org/10.1063/1.1291348.

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Horan and the VERITAS Collaboration, D. "Observations of the BL Lac object, 1H1426+428 at TeV gamma-ray energies." In GAMMA 2001: Gamma-Ray Astrophysics 2001. AIP, 2001. http://dx.doi.org/10.1063/1.1419423.

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Moriarty, P. "Kernel analysis in TeV gamma-ray selection." In GeV-TeV gamma ray astrophysics workshop. AIP, 2000. http://dx.doi.org/10.1063/1.1291390.

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Reports on the topic "TeV gamma ray astrophysics"

1

Lamb, R. C., and D. A. Lewis. Very high energy gamma ray astrophysics. Office of Scientific and Technical Information (OSTI), February 1990. http://dx.doi.org/10.2172/5076918.

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Lamb, R. C., and D. A. Lewis. Very high energy gamma ray astrophysics. Office of Scientific and Technical Information (OSTI), February 1992. http://dx.doi.org/10.2172/5693223.

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Woosley, Stan. Computational Astrophysics Consortium 3 - Supernovae, Gamma-Ray Bursts and Nucleosynthesis. Office of Scientific and Technical Information (OSTI), August 2014. http://dx.doi.org/10.2172/1150840.

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Tajima, T., and Y. Takahashi. Laboratory laser acceleration and high energy astrophysics: {gamma}-ray bursts and cosmic rays. Office of Scientific and Technical Information (OSTI), August 1998. http://dx.doi.org/10.2172/674811.

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Lamb, R., and D. Lewis. Very high energy gamma ray astrophysics. Technical progress report, May 1, 1992--April 30, 1993. Office of Scientific and Technical Information (OSTI), February 1993. http://dx.doi.org/10.2172/6750211.

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Lamb, R. C., and D. A. Lewis. Very high energy gamma ray astrophysics. Technical progress report, May 1, 1991--April 30, 1992. Office of Scientific and Technical Information (OSTI), February 1992. http://dx.doi.org/10.2172/10122596.

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Byrum, K., D. Horan, T. Tait, R. Wanger, G. Zaharijas, J. Buckley, E. A. Baltz, et al. Section on prospects for dark matter detection of the white paper on the status and future of ground-based TeV gamma-ray astronomy. Office of Scientific and Technical Information (OSTI), May 2009. http://dx.doi.org/10.2172/952938.

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