The spectral energy distribution of fermi bright blazars

We have conducted a detailed investigation of the broadband spectral properties of the γ-ray selected blazars of the Fermi LAT Bright AGN Sample (LBAS). By combining our accurately estimated Fermi γ-ray spectra with Swift, radio, infra-red, optical, and other hard X-ray/γ-ray data, collected within 3 months of the LBAS data taking period, we were able to assemble high-quality and quasi-simultaneous spectral energy distributions (SED) for 48 LBAS blazars. The SED of these γ-ray sources is similar to that of blazars discovered at other wavelengths, clearly showing, in the usual log ν-log ν Fν representation, the typical broadband spectral signatures normally attributed to a combination of low-energy synchrotron radiation followed by inverse Compton emission of one or more components. We have used these SED to characterize the peak intensity of both the low- and the high-energy components. The results have been used to derive empirical relationships that estimate the position of the two peaks from the broadband colors (i.e., the radio to optical, αro, and optical to X-ray, αox, spectral slopes) and from the γ-ray spectral index. Our data show that the synchrotron peak frequency (νSpeak) is positioned between 1012.5 and 1014.5 Hz in broad-lined flat spectrum radio quasars (FSRQs) and between 10 13 and 1017 Hz in featureless BL Lacertae objects. We find that the γ-ray spectral slope is strongly correlated with the synchrotron peak energy and with the X-ray spectral index, as expected at first order in synchrotron-inverse Compton scenarios. However, simple homogeneous, one-zone, synchrotron self-Compton (SSC) models cannot explain most of our SED, especially in the case of FSRQs and low energy peaked (LBL) BL Lacs. More complex models involving external Compton radiation or multiple SSC components are required to reproduce the overall SED and the observed spectral variability. While more than 50% of known radio bright high energy peaked (HBL) BL Lacs are detected in the LBAS sample, only less than 13% of known bright FSRQs and LBL BL Lacs are included. This suggests that the latter sources, as a class, may be much fainter γ-ray emitters than LBAS blazars, and could in fact radiate close to the expectations of simple SSC models. We categorized all our sources according to a new physical classification scheme based on the generally accepted paradigm for Active Galactic Nuclei and on the results of this SED study. Since the LAT detector is more sensitive to flat spectrum γ-ray sources, the correlation between νSpeak and γ-ray spectral index strongly favors the detection of high energy peaked blazars, thus explaining the Fermi overabundance of this type of sources compared to radio and EGRET samples. This selection effect is similar to that experienced in the soft X-ray band where HBL BL Lacs are the dominant type of blazars. © 2010 The American Astronomical Society

Insights into the high-energy γ-ray emission of Markarian 501 from extensive multifrequency observations in the Fermi era

We report on the γ-ray activity of the blazar Mrk 501 during the first 480 days of Fermi operation. We find that the average Large Area Telescope (LAT) γ-ray spectrum of Mrk 501 can be well described by a single power-law function with a photon index of 1.78 ± 0.03. While we observe relatively mild flux variations with the Fermi-LAT (within less than a factor of two), we detect remarkable spectral variability where the hardest observed spectral index within the LAT energy range is 1.52 ± 0.14, and the softest one is 2.51 ± 0.20. These unexpected spectral changes do not correlate with the measured flux variations above 0.3 GeV. In this paper, we also present the first results from the 4.5 month long multifrequency campaign (2009 March 15-August 1) on Mrk 501, which included the Very Long Baseline Array (VLBA), Swift, RXTE, MAGIC, and VERITAS, the F-GAMMA, GASP-WEBT, and other collaborations and instruments which provided excellent temporal and energy coverage of the source throughout the entire campaign. The extensive radio to TeV data set from this campaign provides us with the most detailed spectral energy distribution yet collected for this source during its relatively low activity. The average spectral energy distribution of Mrk 501 is well described by the standard one-zone synchrotron self-Compton (SSC) model. In the framework of this model, we find that the dominant emission region is characterized by a size ≲0.1 pc (comparable within a factor of few to the size of the partially resolved VLBA core at 15-43 GHz), and that the total jet power (≃1044 erg s-1) constitutes only a small fraction (∼10-3) of the Eddington luminosity. The energy distribution of the freshly accelerated radiating electrons required to fit the time-averaged data has a broken power-law form in the energy range 0.3 GeV-10 TeV, with spectral indices 2.2 and 2.7 below and above the break energy of 20 GeV. We argue that such a form is consistent with a scenario in which the bulk of the energy dissipation within the dominant emission zone of Mrk 501 is due to relativistic, proton-mediated shocks. We find that the ultrarelativistic electrons and mildly relativistic protons within the blazar zone, if comparable in number, are in approximate energy equipartition, with their energy dominating the jet magnetic field energy by about two orders of magnitude. © 2011. The American Astronomical Society

Method of determination of fluidizers firing of a volley fire the reactive systems

Пропонується спосіб визначення установок для стрільби реактивними системами залпового вогню на основі рішення системи диференційних рівнянь руху оперених літальних апаратів в збуджуючому середовищі.В статье предлагается способ определения установок для стрельбы реактивными системами залпового огня на основе решения системы дифференциальных уравнений движения оперенных летательных аппаратов в возмущенной среде.In the article the method of determination of fluidizers is offered firing of a volley fire the reactive systems on the basis of decision of the system of differential equalizations of motion of finned aircrafts in a perturbative environment

Account of displacement of center of grouping of breaks of shells in investigation of warming-up of barrels of instruments during implementation of fire tasks

В статті проведений аналіз впливу зміщення центра групування снарядів, яке виникає у наслідок розігріву ствола під час ведення інтенсивного вогню. Розглянуто існуючі способи визначення та обліку впливу розігріву ствола в ході підготовки та ведення вогню. Запропоновано спосіб урахування розігріву ствола під час коректування стрільби на ураження спостережених цілей за допомогою перспективної балістичної станції, що встановлюється на кожній гарматі та алгоритм обліку розігріву ствола в результаті інтенсивної стрільби.В статье проведен анализ влияния смещения центра группирования снарядов, которое возникает в следствии разогрева ствола во время ведения интенсивного огня. Рассмотрены существующие способы определения и учета влияния разогрева ствола в ходе подготовки и ведения огня. Предложен способ учета разогрева ствола во время корректировки стрельбы на поражение наблюдаемых целей с помощью перспективной баллистической станции, которая устанавливается на каждом орудии и алгоритм учета разогрева ствола в результате интенсивной стрельбы.The analysis of influence of displacement of center of grouping of shells, which arises up in investigation of warming-up of barrel during the conduct of intensive fire, is conducted in the article. The existent methods of determination and account of influence of warming-up of barrel are considered during preparation and conduct of fire. The method of account of warming-up of barrel is offered during adjustment of firing on the defeat of the looked after aims by the perspective ballistic station which is set on every instrument and algorithm of account of warming-up of barrel as a result of the intensive firing