The first energetic gamma-ray experiment telescope (EGRET) source catalog

Fichtel, C. E.; Bertsch, D. L.; Chiang, J.; Dingus, B. L.; Esposito, J. A.; Fierro, J. M.; Hartman, R. C.; Hunter, S. D.; Kanbach, G.; Kniffen, D. A.; Kwok, P. W.; Lin, Y. C.; Mattox, J. R.; Mayer‐Hasselwander, H. A.; McDonald, L. M.; Michelson, P. F.; Montigny, C. von; Nolan, P. L.; Pinkau, K.; Radecke, H. D.; Rothermel, H.; Sreekumar, P.; Sommer, M.; Schneid, E. J.; Thompson, D. J.; Willis, T. D.

doi:10.1086/192082

Cited by 248 publications

(147 citation statements)

References 0 publications

Supporting

Mentioning

144

Contrasting

Order By: Relevance

“…The figure shows in green archival radio and IR data (from NED) and the EGRET upper limit (Fichtel et al 1994). The gray line represents the GLAST sensitivity curve.…”

Section: Fig 2 Spectral Energy Distributions and Models (Solid Linementioning

confidence: 99%

See 1 more Smart Citation

The changing look of PKS 2149-306

Bianchin¹,

Foschini²,

Ghisellini

et al. 2009

A&A

View full text Add to dashboard Cite

Aims. We study the blazar nature of the high-redshift Flat-Spectrum Radio Quasar PKS 2149-306 (z = 2.345) by investigating its long-term behavior. Methods. We analyzed all publicly available optical-to-X-ray observations performed by XMM-Newton, Swift, and INTEGRAL. Results. PKS 2149-306 is one of four blazars at z > 2 that have been observed in the hard-X-ray regime with both the BAT and ISGRI instruments. Observations acquired almost 1 year apart in the 60−300 keV energy band in the object rest frame, exhibit no noticeable change in spectral slope associated with a flux variation of more than a factor of two. Swift data appear to show a roll-off below ∼1 keV, which becomes increasingly evident during a ∼3-day time-frame, that can be explained as the natural spectral break caused by the Inverse Compton onset. The broad-band spectra allow us to identify two different states. The SED modeling suggests that they can be interpreted by only a change in the bulk Lorentz factor of the jet.

show abstract

“…The figure shows in green archival radio and IR data (from NED) and the EGRET upper limit (Fichtel et al 1994). The gray line represents the GLAST sensitivity curve.…”

Section: Fig 2 Spectral Energy Distributions and Models (Solid Linementioning

confidence: 99%

“…X-ray points are corrected only for the Galactic absorption. The multiwavelength spectra are completed with radio and IR data taken from NED, and the EGRET upper limit (Fichtel et al 1994). We attempt to describe the two states in terms of changes in the physical parameters of the source.…”

Section: Sed Modelingmentioning

confidence: 99%

The changing look of PKS 2149-306

Bianchin¹,

Foschini²,

Ghisellini

et al. 2009

A&A

View full text Add to dashboard Cite

show abstract

“…EGRET observed 3C 345 between 1991 and 1994 during a time of enhanced radio activity. An upper limit of 2.5 × 10 −7 ph cm −2 s −1 for the viewing period September 12th−19th, 1991, was reported (Fichtel et al 1994). However, Casandjian & Grenier (2008) report the detection of a γ-ray source that could be consistent with 3C 345 in the period April 23rd−May 7th, 1996 with a γ-ray flux of (3.5 ± 0.8) × 10 −7 ph cm −2 s −1 , but it was noted that the association with 3C 345 remains unclear because of a possible confusion with Mrk 501.…”

Section: Discussion and Summarymentioning

confidence: 97%

Identification ofγ-ray emission from 3C 345 and NRAO 512

Schinzel

Sokolovsky

D’Ammando

et al. 2011

A&A

View full text Add to dashboard Cite

For more than 15 years, since the days of the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO; 1991−2000, it has remained an open question why the prominent blazar 3C 345 was not reliably detected at γ-ray energies ≥20 MeV. Recently a bright γ-ray source (0FGL J1641.4+3939/1FGL J1642.5+3947), potentially associated with 3C 345, was detected by the Large Area Telescope (LAT) on Fermi. Multiwavelength observations from radio bands to X-rays (mainly GASP-WEBT and Swift) of possible counterparts (3C 345, NRAO 512, B3 1640+396) were combined with 20 months of Fermi-LAT monitoring data (August 2008−April 2010) to associate and identify the dominating γ-ray emitting counterpart of 1FGL J1642.5+3947. The source 3C 345 is identified as the main contributor for this γ-ray emitting region. However, after November 2009 (15 months), a significant excess of photons from the nearby quasar NRAO 512 started to contribute and thereafter was detected with increasing γ-ray activity, possibly adding flux to 1FGL J1642.5+3947. For the same time period and during the summer of 2010, an increase of radio, optical and X-ray activity of NRAO 512 was observed. No γ-ray emission from B3 1640+396 was detected.

show abstract

“…EGRET detected 14 CJF sources and provided an upper limit for 50 more (Fichtel et al 1994;Hartman et al 1999). Unlike for the radio and the X-rays, the γ-ray study of this sample is A16, page 2 of 13 not complete because EGRET only made targeted observations of some of the CJF sources.…”

Section: γ-Ray Emissionmentioning

confidence: 99%

γ-rays in flat-spectrum AGN: revisiting the fast jet hypothesis with the CJF sample

Karouzos

Britzen

Witzel

et al. 2011

A&A

View full text Add to dashboard Cite

Context. The recent release of the First Fermi-LAT Source Catalog solidified the predominant association of extragalactic γ-ray emitters to active galaxies, in particular blazars. A tight connection between AGN jet kinematics and γ-ray properties has been argued for, attributing the energetic emission from active galaxies to their highly relativistic outflows. Aims. We investigate the Caltech-Jodrell Bank flat-spectrum (CJF) sample to study the connection between AGN jet kinematics and their γ-ray properties. The high number of sources included in the sample, in addition to the excellent kinematic data available, allows us to investigate the origin of γ-ray emission in AGN. Methods. We identify the CJF sources detected in γ-rays (by Fermi-LAT and EGRET). We use γ-ray luminosities and the available VLBI kinematic data to look for correlations between γ-ray and kinematic properties, as well as for differences between AGN classes (quasars, BL Lacs, radio galaxies). We also check the kinematics of the TeV sources in the CJF. Results. 21.8% of the CJF has been detected in the γ-ray regime. We find the detectability of BL Lacs significantly higher compared to quasars. Sources detected in the γ-rays show a wider apparent jet velocity distribution compared to the non-detected ones, but the maxima of both distributions are at similar values. No strong link between γ-ray detectability and fast apparent jet speeds is found. A tentative correlation is found between γ-ray luminosity and maximum apparent jet speeds, stronger for BL Lac and γ-variable sources. We find non-radial jet motions to be important to γ-ray emission. We suggest two-zone, spine-sheath models as a possible explanation for our results. Two out of four CJF TeV sources show superluminal jet speeds, in contrast to previous studies.

show abstract

The first energetic gamma-ray experiment telescope (EGRET) source catalog

Cited by 248 publications

References 0 publications

The changing look of PKS 2149-306

The changing look of PKS 2149-306

Identification ofγ-ray emission from 3C 345 and NRAO 512

γ-rays in flat-spectrum AGN: revisiting the fast jet hypothesis with the CJF sample

Contact Info

Product

Resources

About