Gamma-Ray Burst detection prospects for next generation ground-based VHE facilities. (arXiv:2109.06676v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mura_G/0/1/0/all/0/1">G. La Mura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Almeida_U/0/1/0/all/0/1">U. Barres de Almeida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conceicao_R/0/1/0/all/0/1">R. Conceição</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angelis_A/0/1/0/all/0/1">A. De Angelis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Longo_F/0/1/0/all/0/1">F. Longo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pimenta_M/0/1/0/all/0/1">M. Pimenta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prandini_E/0/1/0/all/0/1">E. Prandini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruiz_Velasco_E/0/1/0/all/0/1">E. Ruiz-Velasco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tome_B/0/1/0/all/0/1">B. Tomé</a>
Gamma-ray Bursts (GRB) were discovered by satellite-based detectors as
powerful sources of transient $gamma$-ray emission. The Fermi satellite
detected an increasing number of these events with its dedicated Gamma-ray
Burst Monitor (GBM), some of which were associated with high energy photons $(E
> 10, mathrm{GeV})$, by the Large Area Telescope (LAT). More recently,
follow-up observations by Cherenkov telescopes detected very high energy
emission $(E > 100, mathrm{GeV})$ from GRBs, opening up a new observational
window with implications on the interpretation of their central engines and on
the propagation of very energetic photons across the Universe. Here, we use the
data published in the 2nd Fermi-LAT Gamma Ray Burst Catalogue to characterise
the duration, luminosity, redshift and light curve of the high energy GRB
emission. We extrapolate these properties to the very high energy domain,
comparing the results with available observations and with the potential of
future instruments. We use observed and simulated GRB populations to estimate
the chances of detection with wide-field ground-based $gamma$-ray instruments.
Our analysis aims to evaluate the opportunities of the Southern
Wide-field-of-view Gamma-ray Observatory (SWGO), to be installed in the
Southern Hemisphere, to complement CTA. We show that a low-energy observing
threshold $(E_{low} < 200, mathrm{GeV})$, with good point source sensitivity
$(F_{lim} approx 10^{-11}, mathrm{erg, cm^{-2}, s^{-1}}$ in $1,
mathrm{yr})$, are optimal requirements to work as a GRB trigger facility and
to probe the burst spectral properties down to time scales as short as $10,
mathrm{s}$, accessing a time domain that will not be available to IACT
instruments.
Gamma-ray Bursts (GRB) were discovered by satellite-based detectors as
powerful sources of transient $gamma$-ray emission. The Fermi satellite
detected an increasing number of these events with its dedicated Gamma-ray
Burst Monitor (GBM), some of which were associated with high energy photons $(E
> 10, mathrm{GeV})$, by the Large Area Telescope (LAT). More recently,
follow-up observations by Cherenkov telescopes detected very high energy
emission $(E > 100, mathrm{GeV})$ from GRBs, opening up a new observational
window with implications on the interpretation of their central engines and on
the propagation of very energetic photons across the Universe. Here, we use the
data published in the 2nd Fermi-LAT Gamma Ray Burst Catalogue to characterise
the duration, luminosity, redshift and light curve of the high energy GRB
emission. We extrapolate these properties to the very high energy domain,
comparing the results with available observations and with the potential of
future instruments. We use observed and simulated GRB populations to estimate
the chances of detection with wide-field ground-based $gamma$-ray instruments.
Our analysis aims to evaluate the opportunities of the Southern
Wide-field-of-view Gamma-ray Observatory (SWGO), to be installed in the
Southern Hemisphere, to complement CTA. We show that a low-energy observing
threshold $(E_{low} < 200, mathrm{GeV})$, with good point source sensitivity
$(F_{lim} approx 10^{-11}, mathrm{erg, cm^{-2}, s^{-1}}$ in $1,
mathrm{yr})$, are optimal requirements to work as a GRB trigger facility and
to probe the burst spectral properties down to time scales as short as $10,
mathrm{s}$, accessing a time domain that will not be available to IACT
instruments.
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