The Likelihood Analysis of EGRET Data

Mattox, J. R.; Bertsch, D. L.; Chiang, J.; Dingus, B. L.; Digel, S. W.; Esposito, J. A.; Fierro, J. M.; Hartman, R. C.; Hunter, S. D.; Kanbach, G.; Kniffen, D. A.; Lin, Y. C.; Macomb, D. J.; Mayer‐Hasselwander, H. A.; Michelson, P. F.; Montigny, C. von; Mukherjee, R.; Nolan, P. L.; Ramanamurthy, P. V.; Schneid, E. J.; Sreekumar, P.; Thompson, D. J.; Willis, T. D.

doi:10.1086/177068

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“…The full light curve was built using 1 week time binning. The sources from 3FGL LAT catalog (Acero et al 2015) with the high test statistics (TS, Mattox et al 1996) were used to generate the source model. The source was modelled using a log-parabola…”

Section: Gamma-ray Fermi /Lat Datamentioning

confidence: 99%

Multiwavelength observations of the γ-ray flaring quasar S4 1030+61 in 2009–2014

Kravchenko

Kovalev

Hovatta

2016

Mon. Not. R. Astron. Soc.

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We present a study of the parsec-scale multi-frequency properties of the quasar S4 1030+61 during a prolonged radio and γ-ray activity. Observations were performed within Fermi γ-ray telescope, OVRO 40-m telescope and MOJAVE VLBA monitoring programs, covering five years from 2009. The data are supplemented by four-epoch VLBA observations at 5, 8, 15, 24, and 43 GHz, which were triggered by the bright γ-ray flare, registered in the quasar in 2010. The S4 1030+61 jet exhibits an apparent superluminal velocity of (6.4±0.4)c and does not show ejections of new components in the observed period, while decomposition of the radio light curve reveals nine prominent flares. The measured variability parameters of the source show values typical for Fermi-detected quasars. Combined analysis of radio and γ-ray emission implies a spatial separation between emitting regions at these bands of about 12 pc and locates the γ-ray emission within a parsec from the central engine. We detected changes in the value and direction of the linear polarization and the Faraday rotation measure. The value of the intrinsic brightness temperature of the core is above the equipartition state, while its value as a function of distance from the core is well approximated by the power-law. Altogether these results show that the radio flaring activity of the quasar is accompanied by injection of relativistic particles and energy losses at the jet base, while S4 1030+61 has a stable, straight jet well described by standard conical jet theories.

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Section: Gamma-ray Fermi /Lat Datamentioning

confidence: 99%

Multiwavelength observations of the γ-ray flaring quasar S4 1030+61 in 2009–2014

Kravchenko

Kovalev

Hovatta

2016

Mon. Not. R. Astron. Soc.

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“…The gamma-ray emission from the 2 blazars was investigated between 70 MeV and 300 GeV (100 MeV to 300 GeV for the Vela pulsar) energies using the gtlike routine to maximise the binned likelihood function (Mattox et al, 1996). The data were extracted from a square region 30 • ×30 • centred 2 3FGL time interval 3 http://fermi.gsfc.nasa.gov/ssc/data/analysis/software/ 4 http://www.slac.stanford.edu/exp/glast/groups/canda/lat Performance.htm on the position given by the 3FGL catalogue using events with evtclass = 128 and evtype = 3 5 .…”

Section: Analysis Of the Fermi -Lat Datamentioning

confidence: 99%

Cut-off characterisation of energy spectra of bright fermi sources: Current instrument limits and future possibilities

Romoli

Taylor

Aharonian

2017

Astroparticle Physics

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In this paper some of the brightest GeV sources observed by the Fermi -LAT were analysed, focusing on their spectral cut-off region. The sources chosen for this investigation were the brightest blazar flares of 3C 454.3 and 3C 279 and the Vela pulsar with a reanalysis with the latest Fermi -LAT software. For the study of the spectral cut-off we first explored the Vela pulsar spectrum, whose statistics in the time interval of the 3FGL catalog allowed strong constraints to be obtained on the parameters. We subsequently performed a new analysis of the flaring blazar SEDs. For these sources we obtained constraints on the cut-off parameters under the assumption that their underlying spectral distribution is described by a power-law with a stretched exponential cut-off. We then highlighted the significant potential improvements on such constraints by observations with next generation ground based Cherenkov telescopes, represented in our study by the Cherenkov Telescope Array (CTA). Adopting currently available simulations for this future observatory, we demonstrate the considerable improvement in cut-off constraints achievable by observations with this new instrument when compared with that achievable by satellite observations.

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“…To perform a quantitative evaluation, we employ the method of likelihood fitting (e.g., Mattox et al 1996;Cowan 1998;Feigelson & Babu 2012). We focus here on the ability of CTA to determine the dominant emission component from the prospectively observed morphology.…”

Section: Gamma-ray Imagementioning

confidence: 99%

Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946

Acero¹,

Aloisio²,

Amans³

et al. 2017

ApJ

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The Likelihood Analysis of EGRET Data

Cited by 1,304 publications

References 0 publications

Multiwavelength observations of the γ-ray flaring quasar S4 1030+61 in 2009–2014

Multiwavelength observations of the γ-ray flaring quasar S4 1030+61 in 2009–2014

Cut-off characterisation of energy spectra of bright fermi sources: Current instrument limits and future possibilities

Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946

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