A Variability and Localization Study of the Galactic Center Gamma‐Ray Source 3EG J1746−2851

Pohl, M.

doi:10.1086/430085

Cited by 14 publications

(12 citation statements)

References 34 publications

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“…The authors suggest that the GeV source observed by EGRET has another origin. This is consistent with the recent determination of the position of the EGRET source 3EG J1746Ϫ2851 by Hooper & Dingus (2002) and Pohl (2005). Other scenarios for the gray production in the vicinity of Sgr A* have also been found to be consistent with the TeV observations but not with the GeV observations (Aharonian & Neronov 2005).…”

Section: Discussionsupporting

confidence: 90%

“…Pohl (1997) proposed that the GeV emission can be related to the GC radio arc. Crocker et al (2005;see also Fatuzzo & Melia 2003) argue for the GeV and TeV emission coming from different sites of the shell of the very powerful supernova remnant Sgr A East.…”

Section: Discussionmentioning

confidence: 99%

“…However, an independent analysis of the EGRET data (Hooper & Dingus 2002) indicates a point source whose position is different from the GC at a confidence level beyond 99.9%. This was recently sustained by Pohl (2005).…”

Section: Introductionmentioning

confidence: 94%

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Observation of Gamma Rays from the Galactic Center with the MAGIC Telescope

Albert

Aliu

Anderhub

et al. 2006

ApJ

153

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Recently, the Galactic center has been reported to be a source of very high energy (VHE) γ-rays by the CANGAROO, VERITAS, and HESS experiments. The energy spectra as measured by these experiments show substantial differences. In this Letter we present MAGIC observations of the Galactic center, resulting in the detection of a differential γ-ray flux consistent with a steady, hard-slope power law, described as dNγ/(dAdtdE)=(2.9+/-0.6)×10-12(E/TeV)-2.2+/-0.2 cm-2 s-1 TeV-1. The γ-ray source is centered at (R.A., decl.) = (17h45m20s, -29°2'). This result confirms the previous measurements by the HESS experiment and indicates a steady source of TeV γ-rays. We briefly describe the observational technique used and the procedure implemented for the data analysis, and we discuss the results in the perspective of different models proposed for the acceleration of the VHE γ-rays

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Section: Discussionsupporting

confidence: 90%

Section: Discussionmentioning

confidence: 99%

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Observation of Gamma Rays from the Galactic Center with the MAGIC Telescope

Albert

Aliu

Anderhub

et al. 2006

ApJ

153

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“…Indeed, it was explicitly noted by Mayer-Hasselwander et al (1998) that no localized excess associated with the Sgr B complex was detected by EGRET excluding the possibility of a significantly enhanced CR density in these cloudsin the appropriate energy range, of course. The closest source EGRET did detect in these pointings, 3EG J1746-2851, was at first thought to have a localization marginally compatible with Sgr A* or Sgr A East, but was later shown to be perceptibly off-set to Galactic east (Hooper & Dingus 2005;Pohl 2005). This imples that this ∼ GeV source can not be identified with the point source seen by HESS at/near Sgr A* (HESS J1745-2290: Crocker et al (2005)).…”

Section: Gev γ-Ray Observations Of Sgr Bmentioning

confidence: 90%

The Cosmic Ray Distribution in Sagittarius B

Crocker

Jones

Protheroe

et al. 2007

ApJ

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The HESS instrument has observed a diffuse flux of ~ TeV gamma rays from a large solid angle around the Galactic center (GC). This emission is correlated with the distribution of gas in the region suggesting that the gamma rays originate in collisions between cosmic ray hadrons (CRHs) and ambient matter. Of particular interest, HESS has detected gamma rays from the Sagittarius (Sgr) B Molecular Cloud Complex. Prompted by the suggestion of a hadronic origin for the gamma rays, we have examined archival 330 and 74 MHz Very Large Array radio data and 843 MHz Sydney University Molonglo Sky Survey data covering Sgr B, looking for synchrotron emission from secondary electrons and positrons (expected to be created in the same interactions that supply the observed gamma rays). Intriguingly, we have uncovered non-thermal emission, but at a level exceeding expectation. Adding to the overall picture, recent observations by the Atacama Pathfinder Experiment telescope show that the cosmic ray ionization rate is ten times greater in the Sgr B2 region of Sgr B than the local value. Lastly, Sgr B2 is also a very bright X-ray source. We examine scenarios for the spectra of CRHs and/or primary electrons that would reconcile all these different data. We determine that (i) a hard (~ E^-2.2), high-energy (> TeV) population CRHs is unavoidably required by the HESS gamma ray data and (ii) the remaining broad-band, non-thermal phenomenology is explained either by a rather steep (~ E^-2.9) spectrum of primary electrons or a (~ E^-2.7) population of CRHs. No single, power-law population of either leptons or hadrons can explain the totality of broadband, non-thermal Sgr B phenomenology.Comment: 45 pages, 5 figures; Minor revisions - version accepted for publication in Ap

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“…Nearby the young cluster; the Arches cluster, at the Galactic center, is another gamma-ray source, 3EG J1746-2851, which may radiate via inverse Compton scattering of the radiation field of the cluster (Yusef-Zadeh et al 2003). However, since the Galactic center is well populated with a wide variety of putative such objects, and is somewhat dynamic and confused, it may be premature to conclude definitively that this is the precise mechanism operating in this case (Pohl 2005;Tatischeff et al 2012).…”

Section: Introductionmentioning

confidence: 99%

The Environment around the Young Massive Star Cluster RSGC 1 and HESS J1837-069

Fujita,

Nakanishi,

Muller

et al. 2013

Preprint

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We report on Mopra observations toward the young massive star cluster RSGC 1, adjoined by, and possibly associated with the gamma-ray source HESS J1837-069. We measure the CO (J = 1-0) distribution around the cluster and gamma-ray source, and find that the cluster is slightly higher than the velocity ranges associated with the Crux-Scutum arm. We reveal the cluster is associated with much less molecular gas compared with other young massive clusters in the Galaxy, Westerlund 1 (Wd 1) and 2 (Wd 2), which also radiate gamma-rays. We find no other structures that would otherwise indicate the action of supernova remnants, and due to the lack of material which may form gamma-rays by hadronic interaction, we conclude that the gamma-rays detected from HESS J1837-069 are not created through proton-proton interactions, and may more plausibly originate from the pulsar that was recently found near RSGC 1.

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A Variability and Localization Study of the Galactic Center Gamma‐Ray Source 3EG J1746−2851

Cited by 14 publications

References 34 publications

Observation of Gamma Rays from the Galactic Center with the MAGIC Telescope

Observation of Gamma Rays from the Galactic Center with the MAGIC Telescope

The Cosmic Ray Distribution in Sagittarius B

The Environment around the Young Massive Star Cluster RSGC 1 and HESS J1837-069

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