CANGAROO-III OBSERVATION OF TeV GAMMA RAYS FROM THE UNIDENTIFIED GAMMA-RAY SOURCE HESS J1614–518

Mizukami, Taku; Kubo, H.; Yoshida, Tatsuo; Nakamori, Takeshi; Enomoto, R.; Tanimori, T.; Akimoto, Masanori; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, Shinji; Hara, T.; Hayashi, S.; Ishioka, H.; Kabuki, S.; Kajino, F.; Kawachi, A.; Kifune, T.; Kiuchi, R.; Kunisawa, Takashi; Kushida, J.; Matoba, T.; Matsubara, Y.; Matsuzawa, I.; Mizumoto, Y.; Mori, M.; Muraishi, H.; Naito, T.; Nakayama, K.; Nishijima, K.; Ohishi, M.; Otake, Y.; Ryoki, Shinichi; Saito, Ken; Sakamoto, Yoshitaka; Stamatescu, V.; Suzuki, Takeshi; Swaby, D. L.; Thornton, G.; Tokanai, Fuyuki; Toyota, Y.; Tsuchiya, Ken; Yanagita, S.; Yokoe, Y.; Yoshikoshi, T.; Yukawa, Y.

doi:10.1088/0004-637x/740/2/78

Cited by 3 publications

(9 citation statements)

References 78 publications

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“…and CANGAROO-III [38] telescopes have found several high energy gamma-ray sources in IceCube's FOV. Most of these sources are identified as or correlated with PWNe.…”

Section: Discussionmentioning

confidence: 99%

Search for Galactic PeV gamma rays with the IceCube Neutrino Observatory

Aartsen¹,

Abbasi²,

Abdou³

et al. 2013

Phys. Rev. D

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Gamma-ray induced air showers are notable for their lack of muons, compared to hadronic showers. Hence, air shower arrays with large underground muon detectors can select a sample greatly enriched in photon showers by rejecting showers containing muons. IceCube is sensitive to muons with energies above ∼500 GeV at the surface, which provides an efficient veto system for hadronic air showers with energies above 1 PeV. One year of data from the 40-string IceCube configuration was used to perform a search for point sources and a Galactic diffuse signal. No sources were found, resulting in a 90% C.L. upper limit on the ratio of gamma rays to cosmic rays of 1.2 × 10 −3 for the flux coming from the Galactic Plane region ( −80• ) in the energy range 1.2 -6.0 PeV. In the same energy range, point source fluxes with E −2 spectra have been excluded at a level of (E/TeV) 2 dΦ/dE ∼ 10 −12 − 10 −11 cm −2 s −1 TeV −1 depending on source declination. The complete IceCube detector will have a better sensitivity, due to the larger detector size, improved reconstruction and vetoing techniques. Preliminary data from the nearly-final IceCube detector configuration has been used to estimate the 5 year sensitivity of the full detector. It is found to be more than an order of magnitude better, allowing the search for PeV extensions of known TeV gamma-ray emitters.PACS numbers: 95.55. Vj, 95.55.Ka, 95.85.Pw, 96.50.sd

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“…and CANGAROO-III [38] telescopes have found several high energy gamma-ray sources in IceCube's FOV. Most of these sources are identified as or correlated with PWNe.…”

Section: Discussionmentioning

confidence: 99%

Search for Galactic PeV gamma rays with the IceCube Neutrino Observatory

Aartsen¹,

Abbasi²,

Abdou³

et al. 2013

Phys. Rev. D

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“…This SNR scenario was further investigated by Mizukami et al (2011). By assuming a power-law distribution of a population of accelerated protons and a source distance of 10 kpc, an ambient matter density of 100 cm −3 was required to reproduce the γ-ray spectrum of HESS J1614−518 via a hadronic interaction model.…”

Section: Hess J1614−518mentioning

confidence: 99%

“…A possible association between HESS J1614−518 and the young open stellar cluster Pismis 22 (Piatti et al 2000) was suggested in scenarios where stellar winds from several B-type stars or undetected SNRs from deceased members of the cluster would accelerate cosmic-rays that would interact with ambient gas to produce γ-rays hadronically. Mizukami et al (2011) used the CANGAROO-III telescopes to study the TeV γ-ray emission towards HESS J1614−518, and also investigated the plausibility of several radiation mechanisms. A leptonic scenario based on an undetected SNR was rejected as it was not able to reproduce the observed spectral energy distribution (SED) in γ-rays.…”

Section: Introductionmentioning

confidence: 99%

A Study of the Interstellar Medium Towards the Unidentified Dark TeV γ-Ray Sources HESS J1614–518 and HESS J1616–508

Lau

Rowell

Voisin

et al. 2017

Publ. Astron. Soc. Aust.

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HESS J1614−518 and HESS J1616−508 are two tera-electron volt (TeV) γ-ray sources that are not firmly associated with any known counterparts at other wavelengths. We investigate the distribution of interstellar medium towards the TeV γ-ray sources using results from a 7 mm-wavelength Mopra study, the Mopra Southern Galactic Plane CO Survey, the Millimetre Astronomer's Legacy Team -45 GHz survey and [CI] data from the HEAT telescope. Data in the CO(1−0) transition lines reveal diffuse gas overlapping the two TeV sources at several velocities along the line of sight, while observations in the CS(1−0) transition line reveal several interesting dense gas features. To account for the diffuse atomic gas, archival Hi data was taken from the Southern Galactic Plane Survey. The observations reveal gas components with masses ∼ 10 3 to 10 5 M and with densities ∼ 10 2 to 10 3 cm −3 overlapping the two TeV sources. Several origin scenarios potentially associated with the TeV γ-ray sources are discussed in light of the distribution of the local interstellar medium. We find no strong convincing evidence linking any counterpart with HESS J1614−518 or HESS J1616−508.

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“…This double-peaked structure is also hinted at in the LAT counts map in Figure 19 but is not very significant. The TeV source was also detected by CANGAROO-III (Mizukami et al 2011).…”

Section: Fgl J16152−5138mentioning

confidence: 99%

“…Source A is an extended source consistent with the peak of HESS J1614−518 and source B coincident with Pismis 22 and toward the center but in a relatively dim region of HESS J1614−518 (Matsumoto et al 2008). Three hypotheses have been presented to explain this emission: either source A is an SNR powering the γ -ray emission; source A is a PWN powered by an undiscovered pulsar in either source A or B; and finally that the emission may arise from hadronic acceleration in the stellar winds of Pismis 22 (Mizukami et al 2011).…”

Section: Fgl J16152−5138mentioning

confidence: 99%

SEARCH FOR SPATIALLY EXTENDEDFERMILARGE AREA TELESCOPE SOURCES USING TWO YEARS OF DATA

Landé

Ackermann

Allafort

et al. 2012

ApJ

171

239

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Spatial extension is an important characteristic for correctly associating γ -ray-emitting sources with their counterparts at other wavelengths and for obtaining an unbiased model of their spectra. We present a new method for quantifying the spatial extension of sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope (Fermi). We perform a series of Monte Carlo simulations to validate this tool and calculate the LAT threshold for detecting the spatial extension of sources. We then test all sources in the second Fermi-LAT catalog for extension. We report the detection of seven new spatially extended sources.

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CANGAROO-III OBSERVATION OF TeV GAMMA RAYS FROM THE UNIDENTIFIED GAMMA-RAY SOURCE HESS J1614–518

Cited by 3 publications

References 78 publications

Search for Galactic PeV gamma rays with the IceCube Neutrino Observatory

Search for Galactic PeV gamma rays with the IceCube Neutrino Observatory

A Study of the Interstellar Medium Towards the Unidentified Dark TeV γ-Ray Sources HESS J1614–518 and HESS J1616–508

SEARCH FOR SPATIALLY EXTENDEDFERMILARGE AREA TELESCOPE SOURCES USING TWO YEARS OF DATA

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