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Bahmanabadi, M.; Anvari, A.; Ghomi, M. Khakian; Purmohammad, D.; Samimi, J.; Rachti, M. Lamehi

doi:10.1023/a:1022038816555

Cited by 11 publications

(13 citation statements)

References 6 publications

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“…In E1 the total number of EAS events was 53 907 and the duration of the experiment was 501 460 s. So the mean event rate of the first experiment was 0.1075 events per second. The distribution of the time between successive events is in good agreement with an exponential function, indicating that the event sampling is completely random (Bahmanabadi et al 2003). In E2 the total number of events was 173 765 and the duration of the second experiment was 2 902 857 s, so its mean event rate was 0.05986 events per seconds.…”

Section: Discussionmentioning

confidence: 52%

“…The error due to the first two factors was ∆t 2 ns (Bahmanabadi et al 2002). The error in the logged time of each EAS event was ∆T = 0.07 s which is due to the recording rate and the synchronizing of the computer.…”

Section: Error Estimation Of Investigated Sources In Galactic Coordinmentioning

confidence: 99%

“…A slight North-South anisotropy is observed which is attributed to the geomagnetic field. We fitted this distribution with a harmonic function as follows: (Bahmanabadi et al 2002) …”

Section: Calculation Of Local Coordinates Of Each Eas Eventmentioning

confidence: 99%

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Observation of EGRET gamma-ray sources by an Extensive Air Shower experiment

Ghomi

Bahmanabadi

Samimi

2005

A&A

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Abstract. Ultra-high-energy (E > 100 TeV) Extensive Air Showers (EASs) have been monitored for a period of five years (1997)(1998)(1999)(2000)(2001)(2002)(2003), using a small array of scintillator detectors in Tehran, Iran. The data have been analyzed taking into account the dependence of source counts on zenith angle. During a calendar year different sources come into the field of view of the detector at varying zenith angles. Because of varying thickness of the overlaying atmosphere, the shower count rate is extremely dependent on zenith angle, which has been carefully analyzed over time (Bahmanabadi et al. 2002, Exp. Astron., 13, 39). High energy gamma-ray sources from the EGRET third catalogue where observed and the data were analyzed using an excess method. Upper limits were obtained for a number of EGRET sources, including 6 AGNs or probably AGNs and 4 unidentified sources.

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Section: Discussionmentioning

confidence: 52%

Section: Error Estimation Of Investigated Sources In Galactic Coordinmentioning

confidence: 99%

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Observation of EGRET gamma-ray sources by an Extensive Air Shower experiment

Ghomi

Bahmanabadi

Samimi

2005

A&A

Self Cite

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“…Moreover, if the trigger efficiency of an array is sensitive to the shower lateral extension, the GeoMF can change the acquisition rate as a function of the zenith and azimuth angles. An azimuthal modulation was observed at the Yakutsk array for EAS with energies above 50 PeV [3] and at the ALBORZ Observatory for energies above 100 TeV [4]. The GeoMF effect has been observed in radio experiments [5] and studied to improve the EAS simulation [6], to correct the pointing ofCerenkov telescopes [7], and to discriminate the primary mass [8].…”

Section: Introductionmentioning

confidence: 98%

Evidence of a geomagnetic effect on extensive air showers detected with the ARGO-YBJ experiment

Mari¹,

Bartoli²,

Bernardini³

et al. 2014

Phys. Rev. D

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The geomagnetic field causes not only the east-west effect on primary cosmic rays but also affects the trajectories of the secondary charged particles in the shower, causing their lateral distribution to be stretched. Thus, both the density of the secondaries near the shower axis and the trigger efficiency of detector arrays decrease. The effect depends on the direction of the showers, thus, introducing a modulation in the measured azimuthal distribution. The azimuthal distribution of the events collected by the ARGO-YBJ detector is deeply investigated for different zenith angles in light of this effect.

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“…The study of the GeoMF effect on the shower development are expected to be performed at higher energies, in fact an azimuthal modulation was already observed not only at the Yakutsk array for EAS with energies above 50 PeV [16] and at the ALBORZ Observatory for energies above 100 TeV [17], but also in radio experiments [18].…”

Section: Introductionmentioning

confidence: 99%

The analog Resistive Plate Chamber detector of the ARGO-YBJ experiment

Bartoli

Bernardini

et al. 2015

Astroparticle Physics

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The ARGO-YBJ experiment has been in stable data taking from November 2007 till February 2013 at the YangBaJing Cosmic Ray Observatory (4300 m a.s.l.). The detector consists of a single layer of Resistive Plate Chambers (RPCs) (6700 m 2 ) operated in streamer mode. The signal pick-up is obtained by means of strips facing one side of the gas volume. The digital readout of 1 arXiv:1504.01510v1 [astro-ph.IM] 7 Apr 2015 the signals, while allows a high space-time resolution in the shower front reconstruction, limits the measurable energy to a few hundred TeV. In order to fully investigate the 1-10 PeV region, an analog readout has been implemented by instrumenting each RPC with two large size electrodes facing the other side of the gas volume. Since December 2009 the RPC charge readout has been in operation on the entire central carpet (∼ 5800 m 2 ). In this configuration the detector is able to measure the particle density at the core position where it ranges from tens to many thousands of particles per m 2 . Thus ARGO-YBJ provides a highly detailed image of the charge component at the core of air showers. In this paper we describe the analog readout of RPCs in ARGO-YBJ and discuss both the performance of the system and the physical impact on the EAS measurements.

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Cited by 11 publications

References 6 publications

Observation of EGRET gamma-ray sources by an Extensive Air Shower experiment

Observation of EGRET gamma-ray sources by an Extensive Air Shower experiment

Evidence of a geomagnetic effect on extensive air showers detected with the ARGO-YBJ experiment

The analog Resistive Plate Chamber detector of the ARGO-YBJ experiment

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