scholarly journals A physical model for the origin of the diffuse cosmic infrared background and the opacity of the Universe to very high energy γ-rays

2010 ◽  
Vol 410 (4) ◽  
pp. 2180-2192 ◽  
Author(s):  
Joshua D. Younger ◽  
Philip F. Hopkins
Keyword(s):  
Physical Model ◽  
High Energy ◽  
Infrared Background ◽  
Very High Energy ◽  
Γ Rays ◽  
Cosmic Infrared Background ◽  
The Universe ◽  
Very High

scholarly journals Search for High Energy emission from GRBs with MAGIC

2016 ◽  
Vol 12 (S324) ◽  
pp. 70-73
Author(s):  
Alessio Berti ◽  
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
Cherenkov Telescopes ◽  
Gamma Ray Imaging ◽  
Very High Energy ◽  
Γ Rays ◽  
High Energy Emission ◽  
The Universe ◽  
Very High

AbstractGamma-Ray Bursts (GRBs) are the most violent explosions in the Universe, releasing a huge amount of energy in few seconds. While our understanding of the prompt and the afterglow phases has increased with Swift and Fermi, we have very few information about their High Energy (HE, E ≲ 100) emission components. This requires a ground-based experiment able to perform fast follow-up with enough sensitivity above ~ 50 GeV. The MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes have been designed to perform fast follow-up on GRBs thanks to fast slewing movement and low energy threshold (~ 50 GeV). Since the beginning of the operations, MAGIC followed-up 89 GRBs in good observational conditions. In this contribution the MAGIC GRBs follow-up campaign and the results which could be obtained by detecting HE and Very High Energy (VHE, E ≳ 100 GeV) γ-rays from GRBs will be reviewed.

scholarly journals Low frequency radio counterparts of HESS J1731−347 a.k.a SNR G353.6−0.7

2017 ◽  
Vol 12 (S331) ◽  
pp. 201-205
Author(s):  
A. J. Nayana ◽  
Poonam Chandra
Keyword(s):  
Radio Emission ◽  
Radio Telescope ◽  
Supernova Remnants ◽  
Low Frequency ◽  
High Energy ◽  
Spectral Indices ◽  
Thermal Radio Emission ◽  
Very High Energy ◽  
Γ Rays ◽  
Very High

AbstractHESS J1731−347 a.k.a. SNR G353.6−0.7 is one of the five known very high energy (VHE, Energy > 0.1 TeV) shell-type supernova remnants. We carried out Giant Metrewave Radio Telescope (GMRT) observations of this TeV SNR in 1390, 610 and 325 MHz bands. We detected the 325 and 610 MHz radio counterparts of the SNR G353.6−0.7 (Nayana et al. 2017). We also determined the spectral indices of individual filaments and our values are consistent with the non-thermal radio emission. We compared the radio morphology with that of VHE emission. The peak in radio emission corresponds to the faintest feature in the VHE emission. We explain this anti-correlated emission in a possible leptonic origin of the VHE γ-rays.

scholarly journals High Energy γ-Rays from the Direction of the Crab Pulsar

1981 ◽  
Vol 94 ◽  
pp. 327-328
Author(s):  
T. Dzikowski ◽  
B. Grochalska ◽  
J. Gawin ◽  
J. Wdowczyk
Keyword(s):  
High Energy ◽  
Crab Pulsar ◽  
Muon Detector ◽  
Extensive Air Shower ◽  
Air Shower ◽  
Very High Energy ◽  
Γ Rays ◽  
Shower Array ◽  
Very High ◽  
Air Shower Array

A search has been made for very high energy photons from the direction of the Crab Pulsar using the Lodz extensive air shower array. This device is particularly suitable for such a study because it consists of a large muon detector which can be used to search for the characteristic muon poor showers.

A Blind Search for Transient Bursts of Very High Energy γ Rays With Milagro

2008 ◽  
Author(s):  
Vlasios Vasileiou ◽  
M. Galassi ◽  
David Palmer ◽  
Ed Fenimore ◽  
Keyword(s):  
High Energy ◽  
Very High Energy ◽  
Γ Rays ◽  
Blind Search ◽  
Very High

scholarly journals Massive stars at (very) high energies: γ-ray binaries

2010 ◽  
Vol 6 (S272) ◽  
pp. 581-586
Author(s):  
Guillaume Dubus ◽  
Benoît Cerutti
Keyword(s):  
High Energy Physics ◽  
Thermal Emission ◽  
Compact Object ◽  
High Energy ◽  
Be Stars ◽  
Radiative Power ◽  
Very High Energy ◽  
Γ Rays ◽  
Γ Ray ◽  
Very High

Abstractγ-ray binaries are systems that emit most of their radiative power above 1 MeV. They are associated with O or Be stars in orbit with a compact object, possibly a young pulsar. Much like colliding wind binaries, the pulsar generates a relativistic wind that interacts with the stellar wind. The result is non-thermal emission from radio to very high energy γ-rays. The wind, radiation and magnetic field of the massive star play a major role in the dynamics and radiative output of the system. They are particularly important to understand the high energy physics at work. Inversely, γ-ray binaries offer novel probes of stellar winds and insights into the fate of O/B binaries.

scholarly journals Very high energy gamma-rays from flat spectrum radio quasars

2014 ◽  
Vol 10 (S313) ◽  
pp. 27-32
Author(s):  
Elina Lindfors
Keyword(s):  
Gamma Rays ◽  
Gamma Ray ◽  
High Energy ◽  
High Energy Gamma ◽  
Spectrum Radio ◽  
Very High Energy ◽  
Energy Gamma ◽  
Emission Models ◽  
Γ Rays ◽  
Very High

AbstractThe detection of Flat Spectrum Radio Quasars (FSRQs) in the Very High Energy (VHE, E>100 GeV) range is challenging, mainly because of their steep soft spectra and distance. Nevertheless four FSRQs are now known to be VHE emitters. The detection of the VHE γ-rays has challenged the emission models of these sources. The sources are also found to exhibit very different behavior. I will give an overview of what is known about the VHE emission of these sources and about the multiwavelength signatures that are connected to the VHE gamma-ray emission.

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