Constraints on the TeV source population and its contribution to the galactic diffuse TeV emission

Casanova, S.; Dingus, B. L.

doi:10.1016/j.astropartphys.2007.11.008

Cited by 30 publications

(26 citation statements)

References 35 publications

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“…Milagro have reported the detection of a diffuse Galactic component, but a substantial fraction of this may be simply explained by the sum of a collection of unresolved sources below the Milagro detection threshold [39]. In truth, the distinction between very widely extended sources and a diffuse background component is not strict.…”

Section: Results: Galactic Sourcesmentioning

confidence: 99%

Ground-Based Gamma Ray Astronomy

Holder

2014

Braz J Phys

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This paper is the write-up of a rapporteur talk given by the author at the 33rd International Cosmic Ray Conference in Rio de Janeiro, Brazil, in 2013. It attempts to summarize results and developments in ground-based gamma-ray observations and instrumentation from among the ∼ 300 submissions to the gamma-ray sessions of the meeting. Satellite observations and theoretical developments were covered by a companion rapporteur [1]. Any review of this nature is unavoidably subjective, and incomplete. Nevertheless, the article should provide a useful status report for those seeking an overview of this exciting and fast-moving field.

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Section: Results: Galactic Sourcesmentioning

confidence: 99%

Ground-Based Gamma Ray Astronomy

Holder

2014

Braz J Phys

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“…Both experiments report diffuse gamma-ray flux excesses with respect to model predictions in the TeV range in several regions along the Galactic plane. Attempts have been made to explain such excesses by an association with dark matter particles [12][13][14][15] but the explanation that the excesses are due to unresolved sources appears more likely [11,16]. In contrast, recent results from the Fermi Space Telescope show a good agreement between the conventional assumption of the locally measured CR spectrum and measurements of propagated high energy gamma rays [17,18].…”

Section: Galactic Diffuse Emissionmentioning

confidence: 69%

The gamma-ray sky as seen with HAWC

Hüntemeyer

2015

EPJ Web of Conferences

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Abstract. The High-Altitude Water Cherenkov (HAWC) TeV Gamma-Ray Observatory located at a site about two hours drive east of Puebla, Mexico on the Sierra Negra plateau (4100 m a.s.l.) was inaugurated in March 2015. The array of 300 water Cherenkov detectors can observe large portions of the sky simultaneously and, with an energy range of 100 GeV to 100 TeV, is currently one of the most sensitive instruments capable of probing particle acceleration near PeV energies. HAWC has already started science operation in the Summer of 2013 and preliminary sky maps have been produced from 260 days of data taken with a partial array. Multiple > 5 σ (pretrials) hotspots are visible along the galactic plane and some appear to coincide with known TeV sources from the H.E.S.S. catalog, SNRs and molecular cloud associations, and pulsars wind nebulae (PWNe). The sky maps based on partial HAWC array data are discussed as well as the scientific potential of the completed instrument especially in the context of multi-wavelengths studies. The HAWC TeV gamma-ray observatoryThe High-Altitude Water Cherenkov (HAWC) telescope is a continuously operating, wide field of view observatory sensitive to gamma rays and cosmic rays in the energy range of 50 GeV to 100 TeV. The telescope is capable of performing unbiased searches for transients to initiate multi-messenger observations. After five years of operation it will have accumulated an exposure of about 100 km 2 hr on more than half of the sky. As a wide-fieldof-view instrument the HAWC observatory is particularly well suited to measure large scale and extended structures such as the Fermi bubble structures or diffuse emission from the Galactic plane. HAWC combines the advantage of possessing the large duty cycle and field of view of space telescopes with the sensitivity to TeV energies. Thereby it provides a complementarity to imaging air Cherenkov telescope like VERITAS, MAGIC, and H.E.S.S., which are characterized by a smaller field of view but better angular resolution.Construction of the HAWC observatory began in 2012 and was completed in 2015. The observatory is located at 4100 m a.s.l. and 18• 59'41" N 97• 18'30.6" W at Sierra Negra near Pico de Orizaba in Mexico. It consists of 300 water Cherenkov detector (WCD) stations covering an area of 22,000 m 2 . Each WCD is 7.3 m wide and 4.5 m high and contains 200,000 L of purified water and four upward-facing photomultiplier tubes (PMT) attached to the bottom of each WCD: one high-quantum efficiency 10-inch Hamamatsu R7081-MOD PMT at the center and three 8-inch Hamamatsu R5912 PMTs at 1.8 m from the center [1]. Over one year of exposure, the completed HAWC array is expected to be sensitive to pure power law spectra at a level of 5 × 10 −13 cm −2 sec −1 (∼ 50 mCrab) a e-mail: petra@mtu.edu above 2 TeV over 5 sr (40%) of the sky [2]. Simulation studies predict an energy dependent angular resolution of between 0.1 • (at highest energies) and 0.8The reconstruction of the precise direction of a primary gamma ray relies on properly calibrated ...

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“…In the study of diffuse emission, a major difficulty is to disentangle the true diffuse emission from unresolved sources. To estimate contributions from unresolved sources below our detection threshold, we use a method so-called number-intensity relation or log N-log S distribution [7].…”

Section: Contributions From Unresolved Sourcesmentioning

confidence: 99%

Probing Galactic Diffuse TeV Gamma-Ray Emission with the HAWC Observatory

Zhou¹,

Rho²,

Vianello³

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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Galactic diffuse TeV gamma-ray emission is produced by the interaction of high-energy cosmicray particles with matter and radiation in our Galaxy. The measurement of Galactic diffuse TeV gamma-ray emission would provide strong constraints on the acceleration and propagation of Galactic cosmic rays. The High Altitude Water Cherenkov (HAWC) Observatory, located in central Mexico at 4100 m above sea level, is sensitive to gamma rays between a few hundreds GeV and ∼ 100 TeV. Thanks to its large field of view of 2 steradians and excellent background estimation, HAWC has a unique capability to observe large extended sources such as Galactic diffuse emission. We present the analysis strategy to detect the Galactic diffuse emission with HAWC, including techniques to remove contaminations from localized sources.

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Constraints on the TeV source population and its contribution to the galactic diffuse TeV emission

Cited by 30 publications

References 35 publications

Ground-Based Gamma Ray Astronomy

Ground-Based Gamma Ray Astronomy

The gamma-ray sky as seen with HAWC

Probing Galactic Diffuse TeV Gamma-Ray Emission with the HAWC Observatory

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