Relevant bibliographies by topics / Galactic emissions

Academic literature on the topic 'Galactic emissions'

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Published: 4 May 2024

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Journal articles on the topic "Galactic emissions"

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Grimaldi, Claudio. "Demography of galactic technosignatures." Monthly Notices of the Royal Astronomical Society 500, no. 2 (November 7, 2020): 2278–88. http://dx.doi.org/10.1093/mnras/staa3450.

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ABSTRACT Probabilistic arguments about the existence of technological life beyond Earth traditionally refer to the Drake equation to draw possible estimates of the number of technologically advanced civilizations releasing, either intentionally or not, electromagnetic emissions in the Milky Way. Here, we introduce other indicators than Drake’s number ND to develop a demography of artificial emissions populating the Galaxy. We focus on three main categories of statistically independent signals (isotropic, narrow beams, and rotating beacons) to calculate the average number NG of emission processes present in the Galaxy and the average number of them crossing Earth, $\bar{k}$, which is a quantity amenable to statistical estimation from direct observations. We show that $\bar{k}$ coincides with ND only for isotropic emissions, while $\bar{k}$ can be orders of magnitude smaller than ND in the case of highly directional signals. We further show that while ND gives the number of emissions being released at the present time, NG considers also the signals from no longer active emitters but whose emissions still occupy the Galaxy. We find that as long as the average longevity of the emissions is shorter than about 105 yr, NG is fully determined by the rate of emissions alone, in contrast to ND and $\bar{k}$ which depend also on the emission longevity. Finally, using analytic formulas of NG, ND, and $\bar{k}$ determined for each type of emission processes here considered, we provide a comprehensive overview of the values these quantities can possibly achieve as functions of the emission birthrates, longevities, and directionality.
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Okuda, H., T. Nakagawa, H. Shibai, Y. Doi, K. Mochizuki, Y. Yamashita-Yui, M. Yui, T. Nishimura, and F. J. Low. "Diffuse [CII] Emission in the Galaxy." Symposium - International Astronomical Union 169 (1996): 497–98. http://dx.doi.org/10.1017/s0074180900230143.

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An extensive survey of [C II] line emission at 158 microns using the balloon borne telescope (BICE) has provided a complete map of the emission intensity distribution in the first and the fourth quadrants of the galactic plane (280° < l < 80°, −5° < b < 5°: Okuda et al. 1993). The emission is very extended throughout the galactic plane in which three intensity maxima are seen towards the tangential directions of the Scutum and the Norma arms as well as in the Galactic center region. However the Galactic center maximum is much less prominent compared with the two other distributions, unlike the case of far infrared continuum and CO emissions.
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Sofue, Yoshiaki. "4.1. Radio continuum and molecular gas in the Galactic center: large-scale structures." Symposium - International Astronomical Union 184 (1998): 161–68. http://dx.doi.org/10.1017/s0074180900084473.

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The radio emission from the Galactic Center is a mixture of thermal (free-free) and non-thermal (synchrotron) emissions (Fig. 1a). However, the spectral index in the central 3° region is flat almost everywhere (Sofue 1985), even in regions where strong linear polarization is detected. Therefore, a flat spectrum observed near the galactic center can no longer be taken as an indicator of thermal emission.
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Abbasi, R., M. Ackermann, J. Adams, N. Aggarwal, J. A. Aguilar, M. Ahlers, J. M. Alameddine, et al. "Searches for Neutrinos from Large High Altitude Air Shower Observatory Ultra-high-energy γ-Ray Sources Using the IceCube Neutrino Observatory." Astrophysical Journal Letters 945, no. 1 (March 1, 2023): L8. http://dx.doi.org/10.3847/2041-8213/acb933.

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Abstract Galactic PeV cosmic-ray accelerators (PeVatrons) are Galactic sources theorized to accelerate cosmic rays up to PeV in energy. The accelerated cosmic rays are expected to interact hadronically with nearby ambient gas or the interstellar medium, resulting in γ-rays and neutrinos. Recently, the Large High Altitude Air Shower Observatory (LHAASO) identified 12 γ-ray sources with emissions above 100 TeV, making them candidates for PeVatrons. While at these high energies the Klein–Nishina effect exponentially suppresses leptonic emission from Galactic sources, evidence for neutrino emission would unequivocally confirm hadronic acceleration. Here, we present the results of a search for neutrinos from these γ-ray sources and stacking searches testing for excess neutrino emission from all 12 sources as well as their subcatalogs of supernova remnants and pulsar wind nebulae with 11 yr of track events from the IceCube Neutrino Observatory. No significant emissions were found. Based on the resulting limits, we place constraints on the fraction of γ-ray flux originating from the hadronic processes in the Crab Nebula and LHAASO J2226+6057.
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Miroshnichenko, Anatoly S. "MWC 314 – A new galactic B[e] supergiant." Symposium - International Astronomical Union 162 (1994): 396–97. http://dx.doi.org/10.1017/s0074180900215489.

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We present a new study of MWC 314 = BD +14°3887 – a poorly investigated object with strong emission lines and IR excesses. Merrill (1927) payed attention to it because of the presence of hydrogen and Fe II emissions in its spectrum. Swensson (1942) also detected interstellar lines H and K CaII and 4430 Å band, Balmer emissions from Hα to H8, NaI 5890 and 5896 Å emissions and estimated its spectral type as gG2-3 or dG4-5 from the SED in continuum, and B2 from the excitation degree. Photospheric lines and spectral features of late-type stars were not observed. Allen (1973) noted that the object's SED corresponds to that of a late-type star but it might be a symbiotic system or a reddened normal star. The IRAS fluxes were obtained only at 12 and 25 μm. The object is unknown as a radio source. From this we can conclude that this system consists of, at least, a hot star surrounded by a gaseous envelope.
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Macías-Pérez, J. F., R. D. Davies, R. Watson, C. M. Gutierrez, and R. Rebolo. "A Characterization of the Diffuse Galactic Emissions at Large Angular Scales Using the Tenerife Data." Advances in Astronomy 2013 (2013): 1–15. http://dx.doi.org/10.1155/2013/780407.

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The anomalous microwave emission (AME) has been proved to be an important component of the galactic diffuse emission in the range from 20 to 60 GHz. To discriminate between different models of AME, low frequency microwave data from 10 to 20 GHz are needed. We present here a reanalysis of published and unpublished Tenerife data from 10 to 33 GHz at large angular scales (from 5 to 15 degrees). We cross-correlate the Tenerife data to templates of the main galactic diffuse emissions: synchrotron, free-free, and thermal dust. We find evidence of dust-correlated emission in the Tenerife data that could be explained as spinning dust grain emission.
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Giard, Martin, and Guilaine Lagache. "Galactic emissions: seeing through the Galaxy." Comptes Rendus Physique 4, no. 8 (October 2003): 901–8. http://dx.doi.org/10.1016/j.crhy.2003.09.009.

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Desai, Abhishek, Justin Vandenbroucke, Samalka Anandagoda, Jessie Thwaites, and M. J. Romfoe. "Constraints on the Origins of the Galactic Neutrino Flux Detected by IceCube." Astrophysical Journal 966, no. 1 (April 23, 2024): 23. http://dx.doi.org/10.3847/1538-4357/ad2a5e.

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Abstract Galactic and extragalactic objects in the Universe are sources of high-energy neutrinos that may contribute to the astrophysical neutrino signal seen by IceCube. Recently, a study done using cascade-like events seen by IceCube reported neutrino emission from the Galactic plane with >4σ significance. In this work, we put a lower limit on the number of Galactic sources required to explain this emission. To achieve this, we use a simulation package created to simulate point sources in the Galaxy along with the neutrino and gamma-ray flux emissions originating from them. Along with using past IceCube discovery potential curves, we also account for Eddington bias effects due to Poisson fluctuations in the number of detected neutrino events. We present a toy Monte Carlo simulation to show that there must be at least eight sources, each with luminosity less than 1.6 × 1035 erg s−1, responsible for the Galactic neutrino emission. Our results constrain the number of individual point-like emission regions, which apply both to discrete astrophysical sources and to individual points of diffuse emission.
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Yamauchi, S. "Hot Plasma in the Galaxy." Symposium - International Astronomical Union 188 (1998): 47–50. http://dx.doi.org/10.1017/s0074180900114408.

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In the X-ray band, we can see weak and extended X-rays along the Galactic plane and near the Galactic Bulge region, although these regions are dominated by many point sources (e.g., Warwick et al. 1985). The Tenma satellite discovered conspicuous emission lines from selected regions near the Galactic plane (Koyama et al. 1986). These lines are identified with K-shell line from He-like Fe, hence the extended emission is attributable to optically thin hot plasmas with temperatures of several keV. The origin of the thin hot plasmas, however, have been debatable, because no class of X-ray objects shows such high temperature plasma emissions. To investigate the origin of the extended X-rays, we are currently observing the Galactic plane regions with the ASCA satellite. In this paper, we report on the ASCA results: the hard X-ray imaging and spectroscopy of the hot plasma in the Galaxy.
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Fauvet, L., J. F. Macías-Pérez, S. R. Hildebrandt, and F. X. Désert. "A Characterization of the Diffuse Galactic Emissions in the Anticenter of the Galaxy." Advances in Astronomy 2013 (2013): 1–8. http://dx.doi.org/10.1155/2013/746020.

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Using the Archeops and WMAP data, we perform a study of the anticenter Galactic diffuse emissions—thermal dust, synchrotron, free-free, and anomalous emissions—at degree scales. The high-frequency data are used to infer the thermal dust electromagnetic spectrum and spatial distribution allowing us to precisely subtract this component at lower frequencies. After subtraction of the thermal dust component, a mixture of standard synchrotron and free-free emissions does not account for the residuals at these low frequencies. Including the all-sky 408 MHz Haslam data we find evidence for anomalous emission with a spectral index of −2.5 in units. However, we are not able to provide coclusion regarding the nature of this anomalous emission in this region. For this purpose, data between 408 MHz and 20 GHz covering the same sky region are needed.
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Dissertations / Theses on the topic "Galactic emissions"

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Szabo, Anthony Paul. "High energy emissions for astrophysical objects." Title page, contents and abstract only, 1992. http://web4.library.adelaide.edu.au/theses/09PH/09phs996.pdf.

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Fauvet, Lauranne. "Cosmologie observationnelle avec le satellite Planck : modélisation des émissions galactiques polarisées." Phd thesis, Grenoble, 2010. http://www.theses.fr/2010GRENY032.

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Cette thése est dédiée à la mesure des anisotropies du Fond Diffus Cosmologique (CMB) ainsi qu'à la caractérisation des émissions d'avant-plan galactiques. Les travaux que nous avons réalisés s'inscrivent dans le cadre de la préparation à l'analyse des données du satellite PLANCK. Cette thèse débute par une description du modèle de Big Bang chaud et de la physique du CMB. Ensuite un état des lieux des expériences dédiées à la mesure du CMB est dressé, donnant lieu à la présentation des expériences Archeops, WMAP et PLANCK. Une deuxième partie est dédiée à la présentation des émissions galactiques diffuses puis à l'étude de ces émissions dans le plan galactique, permettant d'établir des cartes partielles des variations spatiales de la température des grains de poussière et des indices spectraux des émissions synchrotron et de poussière. Une troisième partie est dédiée à l'étude des deux principales émissions galactiques polarisées diffuses : les émissions synchrotron et de la poussière. Nous avons étudié des modèles effectifs de ces émissions basés sur l'utilisation de cartes-patron. Ensuite nous avons construit des modèles basés sur la physique de ces émissions et les avons comparés aux données Archeops et WMAP afin de contraindre les paramètres de ces modèles. Ceci nous permet de proposer pour la première fois un modèle cohérent de ces deux émissions. Ensuite nous fournissons une méthode pour améliorer ces contraintes à l'aide des données PLANCK. Dans une dernière partie nous étudions les spectres de puissance angulaires de ces émissions galactiques et estimons la contamination du signal CMB par ces émissions d'avant-plan. Enfin nous proposons une méthode pour minimiser la contamination du signal CMB de PLANCK par l'émission de la poussière
This thesis is dedicated to the Cosmic Microwave Background (CMB) anisotropies measurement and to the characterization of the foreground Galactic emissions. This work is in the framework of the Planck satellite data analysis preparation. First, this thesis gives a description of the Big Bang model and of the CMB physics. Then, we present the Archeops, WMAP and PLANCK experiments and their data analysis. Part two is devoted to the description of the diffuse Galactic synchrotron, free-free and thermal dust emissions and to the study of those emissions in the Galactic plane. Using comparison between our simulations and the WMAP, Archeops and IRIS data we are able to provide partial maps of the spatial variations of the dust grain temperature and of the spectral index of the synchrotron and thermal dust emissions. Third part is dedicated to the study of the two main polarized Galactic emissions: synchrotron and thermal dust emissions. We evaluate effective models based on template maps. We also build physical model based on physics for these emissions that is to say shape of the Galactic magnetic field and matter density in our Galaxy. Using maps and Galactic profiles, we compare our simulations of these emissions to the Archeops and WMAP data. Thanks to that we are able to provide for the first time a coherent model of the synchrotron and thermal dust emissions. Then we propose a method to improve the constraints on our model using the PLANCK data. Finally the last part focuses on the angular power spectra of the polarized Galactic emissions. We estimate the contamination due to these foreground emissions on the CMB signal. In addition we propose a method to minimize the contamination of the CMB PLANCK data by the thermal dust emission using masks
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Jones, Laurence Richard. "X-ray emission from galactic supernova remnants." Thesis, University of Leicester, 1986. http://hdl.handle.net/2381/35703.

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X-ray emission from galactic supernova remnants X-ray images and spectra are used to determine the structure and physical conditions of shock heated interstellar gas and stellar ejecta within three galactic supernova remnants (SNRs). Parameters describing the initial supernova explosions (total energy, ejected mass) and ambient interstellar medium (density, homogeneity) are then derived. The interior density of the "middle-aged" SNR W44 is found to be fairly uniform, and inconsistent with the standard Sedov model, but similar to that predicted by models in which thermal conduction and/or heating and evaporation of engulfed, cold, interstellar clouds are important. This expanding bubble of hot, high pressure gas is likely to be an example of the formation of the hot component of interstellar medium, as detected in the vicinity of the Sun. In addition, it is likely that the SNR has collided with a nearby dense molecular cloud. The SNR W49B is found to be probably the remnant of a Type II supernova which occurred in a relatively dense medium 2000-5000 years ago. The abundance of hot iron in the ejecta is consistent with the cosmic value. The youngest SNR studied, SN1006, is found to be the remnant of a Type I supernova which occurred in a region of low, but fairly uniform (to within a factor of 2), interstellar density. Emission from reverse shocked ejecta may be most prominent in a limited area of the SNR, explaining a discrepancy between previous X-ray spectra of the remnant. A common result in all three SNRs is the detection of hot gas at their centres; the likely effects of a reverse shock and thermal conduction within SNRs are emphasized.
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Cerruti, Matteo. "High-energy emission from active galactic nuclei." Paris 7, 2012. http://www.theses.fr/2012PA077225.

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Ce manuscrit résume les travaux effectués pendant les trois années de thèse doctorale au sein du LUTh (Laboratoire Univers et Théories) et de la collaboration H. E. S. S. Le projet de recherche a été l'étude de l'émission aux hautes énergies (rayons X et rayons y) des Noyaux Actifs de Galaxies (NAG), et a comporté deux parties distinctes: d'un côté l'étude de l'émission en rayons X des galaxies de Seyfert 1 (en s'intéressant particulièrement au problème de l'excès de rayons X-mous, ou soft-excess), et d'un autre côté l'étude de l'émission en rayons y des blazars, en utilisant en particulier les données du réseau de télescopes de type Cherenkov (pour l'observation de photons aux energies de l'ordre du TeV) H. E. S. S. Après une courte Introduction sur les NAG et l'astronomie au TeV, nous décrivons tout d'abord l'émission aux rayons X des galaxies de Seyfert (Chapitre 1). Ce Chapitre est une introduction à l'étude détaillée de l'émission en rayons X de deux galaxies de Seyfert 1, Mrk 509 et Mrk 841, presentée dans le Chapitre 2. Une caractéristique importante de l'émission X de ce type de NAG est le soft-excess, qui ap- paraît comme un excès de flux au-dessous de environ 1 keV par rapport à l'extrapolation à basse énergie de la loi de puissance ajustée entre 3-10 keV. Dans ce Chapitre, nous nous concentrons en particulier sur l'interprétation de cette émission, en ajustan les données Suzaku avec trois modèles différents: une double Comptonisation, une réflexion sur la partie la plus interne du disque d'accrétion, et une absorption par un vent relativiste. Alors que pour Mrk 841 les trois scénarios donnent des résultats statistiquement équivalents, pour Mrk 509 le scénario avec reflexion est exclu. La deuxième partie commence par une introduction générale sur les blazars (Chapitre 3), avant de présenter le réseau de télescope H. E. S. S. , ainsi qu'une revue des NAG observés au TeV (Chapter 4). Nous présentons ensuite l'étude spécifique du blazar émetteur au TeV 1RXS 3101015. 9 - 311909 (Chapitre 5): l'analyse des observations effectuées par H. E. S. S. Et par d'autres observatoires dans l'optique, en rayons-X et rayons-y (ATOM, Swift et Fermi) nous permet de construire la distribution spectrale d'énergie de la source. L'émission de 1RXS 3101015. 9 - 311909 est modélisée dans le cadre d'un modèle lep- tonique, de type synchrotron self-Compton (SSC). Les Chapitres suivants sont plus théoriques, et traitent de la modélisation de l'émission des blazars. Les modèles developpés dans la littérature scientifique peuvent être divisés en deux familles: leptoniques et hadroniques, selon que les particules responsables de l'émission soient des paires electrons/positrons ou des protons, respectivement. Concernant les modèles leptoniques, nous avons developpé un nouvel algorithme numérique pour la détermination des paramètres du modèle d'émission de type SSC (Chapter 6). Cette méthode, appliquée comme exemple au cas spécifique de 1RXS 3101015. 9 - 311909, montre que, pour un blazar de type HBL (high-frequency-peaked BL Lac object), émetteur au GeV et au TeV, l'espace des paramètres du modèle SSC peut être bien determiné, et améliore les contraintes obtenues avec des formules analytiques. Nous pouvons aussi utiliser, sous certaines hypothèses, cet algorithme pour contraindre la distance d'un HBL dont on ne tonnait pas le redshift (application au cas de PKS 0447- 439). Dans le Chapitre 7 nous nous concentrons sur les processus d'émission de type hadronique, en de- crivant le développement d'un nouveau code stationnaire lepto-hadronique (qui prend en compte à la fois les processus leptonique et hadronique), et nous présentons une première application à Mrk 421 et à PKS 2155-304. Le code nous permet de modéliser l'émission des blazars dans un scenario soit lep- tonique soit hadronique, en changeant les paramètres de la région émettrice et des particules présentes. Des scenarios mixtes lepto-hadroniques (dans lesquels l'émission aux hautes énergies est associée aux deux composantes) peuvent être également étudiés dans ce contexte. Nous terminons, dans le Chapitre 8, avec la modélisation de 3C 454. 3, un blazar de type FSRQ (flat- spectrum-radio-quasar), dont le spectre au GeV est décrit par un processus de type inverse Compton sur les photons produits dans la Broad-Line-Region. Les observations conjointes du téléscope Fermi (au GeV) et des télescopes Cherenkov au sol (au TeV, comme H. E. S. S. , MAGIC, VERITAS), ont permit d'observer la composante en rayons-y des blazars avec une très bonne résolution en énergie. Le nouveau téléscope H. E. S. S. II (dont la prémière lumière a été obtenue pendant l'été 2012) va pouvoir améliorer notre connaissance des blazars, en permettant de baisser le seuil d'observation en énergie et donc d'étudier la partie du spectre compris entre Fermi et les télescopes de type Cherenkov. La communauté de l'astronomie au TeV développe actuellement le réseau de nouvelle génération, CTA (Cherenkov Telescope Array). Le projet est dans sa phase préparatoire, et !es premiers prototypes sont en construction (comme par exemple le télescope SST-GATE, sur le site de l'Observatoire de Meudon). Dans ce contexte, en appendix A est présentée une perspective de détection par CTA de blazars au grand redshift
. In this thesis manuscript we tried to summarize the research work done during the last three years in the high-energy group of the LUTh laboratory, as well as in the H. E. S. S. Collaboration. The project deals with the study of high-energy emission from active galactic nuclei (AGN), where, with high energy, we refer here to X and y-rays. The thesis covers in fact two différent aspects of the physics of AGN, firstly the study of the X-ray emission from Seyfert galaxies (radio-quiet AGN), and then of the y-ray emission from blazars (radio-loud AGN). We start then by providing a short introduction to the scientific context of AGN physics (by present- ing the unified AGN model), as well as of TeV astronomy. In the first part we first describe the problem of the soft-X-ray excess in Seyfert galaxies (Chapter 1), before entering in the details of the study of Suzaku observations of two particular objects (Mrk 509 and Mrk 841, Chapter 2), presenting the data analysis and their modelling. The second part starts with an introduction on the blazar physics (Chapter 3), before showing the results achieved by the H. E. S. S. Telescope array on AGN (Chapter 4). A detailed study has been done on a particular blazar detected at TeV energies (1RXS J101015. 9 - 311909), and is presented in Chapter 5. The following chapters are more theoretical, and discuss the modelling of the observed blazar emis- sion. In particular, in Chapter 6 we discuss the constrains on the synchrotron-self-Compton model, presenting a new numerical algorithm to determine the best-fit solution, while in Chapter 7 we present a new stationary lepto-hadronic code, which can be used to model the blazar emission in leptonic, hadronic and mixed scenarios. In Chapter 8 we present the problem of the spectral break observed in the GeV spectrum of 3C 454. 3, and we model it consistently in an external-inverse-Compton scenario. Finally we present a perspective for the detection of high-redshift sources with the future telescope CTA (Appendix A)
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Espey, Brian Russell. "Emission line studies of high redshift AGN." Thesis, University of Cambridge, 1989. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.317876.

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Hands, Alex. "Diffuse and discrete sources of galactic X-ray emission." Thesis, University of Leicester, 2004. http://hdl.handle.net/2381/30675.

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Our Galaxy is a luminous X-ray source by virtue of its discrete X-ray source populations and various large-scale diffuse processes which produce the ultra-hot interstellar medium. This thesis presents an analysis of the properties of a variety of Galactic X-ray emitting components, based on data from the EPIC CCD cameras onboard ESA's XMM-NEWTON satellite observatory. In total 51 individual observations are analysed for which the combined exposure time is nearly 900 ks. X-ray spectra measured over a wide range in Galactic longitude and latitude are used to disentangle the different components of the diffuse soft X-ray background (SXRB). The SXRB is comprised primarily of a two-temperature Galactic halo, an unabsorbed local hot bubble (LHB) and, in certain directions, an extended plasma 'superbubble', all with temperatures in the range of 1-3 million K. Observations towards the Galactic Plane provide evidence that the LHB may be larger in extent than has previously been assumed, with some of the emission lying behind an absorption wall with a column density of NH ~ 3 x 1020 cm-2. The diffuse hard X-ray phenomenon known as the Galactic ridge is investigated at various locations both on and near to the Galactic Plane. The spectrum of the ridge at high energies is well described by a thermal plasma model with a temperature of 108.0 K. The exact nature of this emission is uncertain but several possibilities are discussed in this thesis. The surface brightness of the ridge is measured as ~ 10-10 erg s -1 cm-2 deg-2 (2-10 keV), of which ~ 15% is due to point sources and a further ~2% has been resolved and identified as extended supernova remnants and HII regions. In the region of XMM-NEWTON's X-ray Galactic Plane Survey (XGPS), a total of 424 discrete X-ray sources have been detected. Cumulative log N - log S distributions, including data from other satellites, illustrate how the dominating source population changes from Galactic X-ray binaries at high fluxes to extragalactic objects at fainter fluxes. However, an additional lower luminosity population, possibly associated with cataclysmic variables and RS CVns, appears to contribute significantly at intermediate X-ray fluxes.
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Alves, Marta Isabel Rocha. "Diffuse radio recombination line emission on the galactic plane." Thesis, University of Manchester, 2011. https://www.research.manchester.ac.uk/portal/en/theses/diffuse-radio-recombination-line-emission-on-the-galactic-plane(54655adf-a0da-4f27-86fb-0d8ae43e1e80).html.

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A full-sky free-free template is increasingly important for the high-sensitivity Cosmic Microwave Background (CMB) experiments, such as Planck. On the Galactic plane, where free-free estimations from Halpha measurements become unreliable, Radio Recombination Lines (RRLs) can be used to determine the thermal brightness temperature unambiguously with no dust contamination. RRLs are a powerful tool for the diagnostic of the interstellar medium, tracing the ionised component, its electron temperature, velocity and radial distributions.This thesis describes the investigation of the ionised emission from HII regions and diffuse gas along the Galactic plane using RRLs, with the aim of providing a map of the free-free emission to complement the high latitude Halpha observations. Measuring the free-free emission on the Galactic plane is of great importance to understand and characterise other Galactic emission components: synchrotron, anomalous dust and thermal dust emission. The fully-sampled HI Parkes All-Sky Survey and associated deep Zone of Avoidance Survey are re-analysed to recover extended RRL emission. They include three RRLs (H166alpha, H167alpha and H168alpha) at frequencies near 1.4 GHz. A data cube covering l=20 degree to 44 degree and |b| < 4 degree is constructed of RRL spectra with velocity and spatial resolution of 20 km/s and 14.8 arcmin, respectively. Well-known HII regions are identified as well as the diffuse RRL emission on the Galactic plane.In order to convert the integrated RRL emission into a free-free brightness temperature a value of the electron temperature (Te) of the ionised gas is needed. Using the continuum and line data from the present survey, the variation of Te with Galactocentric radius was derived for the longitude range l=20 degree to 44 degree, with a mean Te on the Galactic plane of 6000 K. The derived Te variation was used to obtain the first direct measure of the free-free brightness in this region of the Galactic plane. Subtraction of this thermal emission from the total continuum at 1.4 GHz leaves the first direct measurement of the synchrotron emission. A narrow component of width 2 degree is identified in the synchrotron latitude distribution.Determining the free-free and synchrotron emission in this region of the Galactic plane identifies the anomalous microwave component, when combined with WMAP and IRIS data. The results are in agreement with models of small spinning dust grains.
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Mak, Wai-ying, and 麥偉瑩. "Very high energy gamma-ray emission from active galactic nuclei." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1999. http://hub.hku.hk/bib/B31221464.

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Mak, Wai-ying. "Very high energy gamma-ray emission from active galactic nuclei /." Hong Kong : University of Hong Kong, 1999. http://sunzi.lib.hku.hk/hkuto/record.jsp?B20567492.

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Page, Mathew James. "X-ray evolution and variability of active galactic nuclei." Thesis, University College London (University of London), 1997. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.267655.

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Books on the topic "Galactic emissions"

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Ilić, Dragana. Aktivna galaktička jezgra: Primer galaksije Mrk 817. Beograd: Zadužbina Andrejević, 2006.

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United States. National Aeronautics and Space Administration., ed. Final technical report: Studies of the evolution of the X-ray emission of clusters of galaxies. [Washington, D.C: National Aeronautics and Space Administration, 1990.

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United States. National Aeronautics and Space Administration., ed. Final technical report: Studies of the evolution of the X-ray emission of clusters of galaxies. [Washington, D.C: National Aeronautics and Space Administration, 1990.

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IAU Colloquium (159th 1996 Shanghai, China). Emission lines in active galaxies: New methods and techniques : IAU Colloquim 159 : meeting held in Shanghai, People's Republic of China, 17-20 June 1996. San Francisco, Calif: Astronomical Society of the Pacific, 1997.

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Verner, Ekaterina. Fe II emission from HII regions and active galactic nuclei. Toronto: Graduate Department of Astronomy, University of Toronto, 2000.

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Hartmann, Dap. The Leiden/Dwingeloo survey of galactic neutral hydrogen. Leiden: Sterrewacht Leiden, 1994.

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Hartmann, Dap. The Leiden/Dwingeloo survey of galactic neutral hydrogen. Leiden: Sterrewacht Leiden, 1995.

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Canary Islands Winter School on Astrophysics (18th 2006 Instituto de Astrofísica de Canarias). The emission-line universe: XVIII Canary Islands Winter School of Astrophysics. New York: Cambridge University Press, 2008.

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Sandford, Scott A. The galactic distribution of aliphatic hydrocarbons in the diffuse interstellar medium. [Washington, D.C: National Aeronautics and Space Administration, 1995.

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Sandford, Scott A. The galactic distribution of aliphatic hydrocarbons in the diffuse interstellar medium. [Washington, D.C: National Aeronautics and Space Administration, 1995.

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Book chapters on the topic "Galactic emissions"

1

Tavani, Marco. "Binary Pulsar Shock Emissions as Galactic Gamma-Ray Sources." In The Gamma Ray Sky with Compton GRO and SIGMA, 181–95. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0067-0_15.

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Netzer, Hagai. "AGN Emission Lines." In Active Galactic Nuclei, 57–160. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-662-39816-6_2.

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Moore, N. P., J. S. Panesar, and A. H. Nelson. "Galactic Dynamo Models." In Multi-Wavelength Continuum Emission of AGN, 486. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-010-9537-2_187.

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Green, Richard, Patrick Osmer, and Alain Porter. "Quasar Emission — Line Strengths." In Active Galactic Nuclei, 124–25. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0963-2_36.

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Salter, Chris J., and Robert L. Brown. "Galactic Nonthermal Continuum Emission." In Astronomy and Astrophysics Library, 1–36. New York, NY: Springer New York, 1988. http://dx.doi.org/10.1007/978-1-4612-3936-9_1.

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Strong, A. W. "Diffuse Galactic Continuum Emission." In The Gamma Ray Sky with Compton GRO and SIGMA, 147–58. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0067-0_12.

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Impey, C. D., C. G. Wynn-Williams, and E. E. Becklin. "Infrared Emission from Radio Galaxies." In Active Galactic Nuclei, 404–5. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0963-2_125.

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Maoz, Dan. "Emission-Line Variability in AGN." In Active Galactic Nuclei, 100–102. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0963-2_25.

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Junkkarinen, Vesa. "QSO Emission Line Redshift Differences." In Active Galactic Nuclei, 122–23. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0963-2_35.

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Kallman, T. R., J. H. Krolik, and B. J. Wilkes. "Quasar Emission Line Profile Modelling." In Active Galactic Nuclei, 131–32. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0963-2_39.

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Conference papers on the topic "Galactic emissions"

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Digel, Seth W. "Galactic Diffuse Emissions." In THE FIRST GLAST SYMPOSIUM. AIP, 2007. http://dx.doi.org/10.1063/1.2757281.

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Renzi, Alessandro. "Primordial non-Gaussianity and diffuse Galactic emissions." In Big Bang, Big Data, Big Computers. Trieste, Italy: Sissa Medialab, 2013. http://dx.doi.org/10.22323/1.165.0031.

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Papavasileiou, Theodora V., Odysseas T. Kosmas, and Ioannis Sinatkas. "Modeling simulated emissions from galactic binary stars." In 11TH INTERNATIONAL CONFERENCE ON MATHEMATICAL MODELING IN PHYSICAL SCIENCES. AIP Publishing, 2023. http://dx.doi.org/10.1063/5.0162914.

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Higdon, J. C. "Theoretical estimates of diffuse galactic γ-ray emissions." In AIP Conference Proceedings Volume 170. AIP, 1988. http://dx.doi.org/10.1063/1.37249.

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Moskalenko, Igor, G. Johannesson, E. Orlando, Troy Porter, and A. W. Strong. "GALPROP Code for Galactic Cosmic Ray Propagation and Associated Photon Emissions." In 35th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.0279.

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von Ballmoos, P. "A distribution for the galactic 26Al and e+e− line emissions." In Gamma-ray line astrophysics. AIP, 1991. http://dx.doi.org/10.1063/1.40928.

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Moskalenko, Igor, Guðlaugur Jóhannesson, and Troy Porter. "GALPROP Code for Galactic Cosmic Ray Propagation and Associated Photon Emissions." In 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.0152.

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Moskalenko, Igor, Gudlaugur Johannesson, and Troy Porter. "GALPROP Code for Galactic Cosmic Ray Propagation and Associated Photon Emissions." In 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.0111.

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Moskalenko, Igor. "GALPROP Code for Galactic Cosmic Ray Propagation and Associated Photon Emissions." In The 34th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.236.0492.

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Fauvet, Lauranne, and Juan-Francisco Macias-Pérez. "Preparation to the Planck Analysis: 3D Modelisation of the Polarized Galactic Emissions." In International Workshop on Cosmic Structure and Evolution. Trieste, Italy: Sissa Medialab, 2010. http://dx.doi.org/10.22323/1.097.0016.

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Reports on the topic "Galactic emissions"

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Moskalenko, Igor V., Andrew W. Strong, Seth W. Digel, and Troy A. Porter. Developing the Galactic Diffuse Emission Model for the GLAST Large Area Telescope. Office of Scientific and Technical Information (OSTI), April 2007. http://dx.doi.org/10.2172/903007.

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Porter, Troy A., Igor V. Moskalenko, and Andrew W. Strong. Inverse Compton Emission from Galactic Supernova Remnants: Effect of the Interstellar Radiation Field. Office of Scientific and Technical Information (OSTI), August 2006. http://dx.doi.org/10.2172/888781.

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Baltz, E. Diffuse Inverse Compton and Synchrotron Emission from Dark Matter Annihilations in Galactic Satellites. Office of Scientific and Technical Information (OSTI), April 2004. http://dx.doi.org/10.2172/826862.

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Woods, Natasha. Probing the Geometry and Physics of the Emission Region in Active Galactic Nuclei using hard X-ray & Gamma-ray Observations. Office of Scientific and Technical Information (OSTI), August 2010. http://dx.doi.org/10.2172/992928.

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