Satellite-based Detectors Research Articles

High temperature spectral emissivity of glass and crystal-bearing basalts

Temperature is a key parameter controlling the rheology of lava flows. However, the unpredictable hazard of eruptions prevents direct measurements of hot volcanic bodies. Thus, the temperature of lava products is mostly retrieved by remote sensing techniques (ground- or satellite-based detectors) build on measuring infrared (IR) radiance. These well-established techniques are however subjected to important errors related to the poor knowledge of one of the most critical parameters, namely spectral emissivity. The aim of our study is to fill this gap by exploring the emissivity–temperature relationship of three different basalts. We performed in situ emissivity measurements at high temperatures (up to 1800 K) over a wide spectral range (350–8000 cm−1; 1.25–28.6 μm), using a non-contact IR apparatus. To unravel the complex radiative behavior of the samples with temperature, structural, chemical and textural analyses using Raman spectroscopy, XRD, DSC, SEM, EMPA and TEM were systematically performed. Our results show that spectral emissivity varies with temperature, wavenumber, and the sample degree of polymerization combined with total FeO content. Spectral emissivity is greatly affected by the crystallization of Fe-Mg-rich crystals at the micro-scale. Consequently, this study proves that spectral emissivity cannot be assumed constant for a single magmatic composition. Finally, our laboratory-measured values of spectral emissivity allowed refining the remote sensing temperature of the 2014–2015 Holuhraun eruption (Bárðarbunga, volcano) by 50 K in average. These new insights will ultimately reduce uncertainties in temperature estimates based on IR technology, information that are crucial to improve hazard assessment in volcanic crisis.

Gamma-ray burst detection prospects for next generation ground-based VHE facilities

ABSTRACT Gamma-ray Bursts (GRB) were discovered by satellite-based detectors as powerful sources of transient γ-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 ($E \gt 10$ GeV), by the Large Area Telescope (LAT). More recently, follow-up observations by Cherenkov telescopes detected very high energy emission ($E \gt 100$ 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 characterize 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 γ-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 ($E_{low} \lt 200$ GeV), with good point source sensitivity ($F_{lim} \approx 10^{-11} \,\mathrm{erg\, cm^{-2}\, s^{-1}}$ in $1$ 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 $10$ s, accessing a time domain that will not be available to Imaging Atmospheric Cherenkov Telescopes instruments.

Monte Carlo simulation of a satellite-based detector of cosmic ray ions with elemental separation from hydrogen to nickel

Observing cosmic rays and solar energetic particles provides important information about the solar wind and solar storms. We are working toward building a Thai detector of energetic ions from space that is inspired by the Mass Spectrometer Telescope (MAST), a satellite-based detector installed on SAMPEX of cosmic ray ions with the energy range of 0.01 to 0.5 GeV/nucleon with the objective to determine the nuclear charge and kinetic energy for nuclei with atomic number of Z = 1 (hydrogen) to 28 (nickel). The energy range of the detector covers the energy range of anomalous cosmic rays, Galactic cosmic rays and solar energetic particles. Therefore, observations by such a detector can provide insight into the origin and transport of these ions in cosmic rays and solar energetic particles. During solar events, measurements of the elemental composition of solar energetic particles can be compared with the composition of the solar corona. We have created a computational model of the MAST detector to simulate ion detection using the FLUKA program to measure the energy deposition of heavy ions in multiple detector components to determine their initial kinetic energy in the simulation. From the simulation results, we can identify the ions’ energies and species using established methods and calculate the geometry factor of the detector, comparing the results with previous reports.

Possibility of using satellite-based detector for recording the Cherenkov light from ultrahigh-energy extensive atmospheric shower penetrating into ocean water

We have estimated the reflected component of Cherenkov radiation, which arises in developing of an extensive air shower with primary energy of 10^20 eV over the ocean surface. It has been shown that, under conditions of the TUS experiment, a flash of the reflected Cherenkov photons at the end of the fluorescence track can be identified in showers with zenith angles up to 20 degrees.

Gamma-ray detection from neutralino annihilation in non-universal SUGRA scenarios

We analyze the indirect detection of neutralino dark matter in supergravity scenarios with non-universal soft scalar and gaugino masses. In particular, the gamma-ray flux arising from the galactic center due to neutralino annihilation is computed. In important regions of the parameter space it can be increased significantly (about two orders of magnitude) with respect to the universal scenario. This result is compared with the sensitivity of current and planned experiments, such as the satellite-based detectors EGRET and GLAST and the ground-based atmospheric telescope HESS. For example, for tan β < 35 the sensitivity region of GLAST and HESS can only be reached in non-universal scenarios.

Detection Techniques of Microsecond Gamma‐Ray Bursts Using Ground‐based Telescopes

Gamma-ray observations above 200 MeV are conventionally made by satellite-based detectors. The EGRET detector on the Compton Gamma Ray Observatory has provided good sensitivity for the detection of bursts lasting for more than 200 ms. Theoretical predictions of high-energy gamma-ray bursts produced by quantum mechanical decay of primordial black holes (Hawking) suggest the emission of bursts on shorter timescales. The final stage of a primordial black hole results in a burst of gamma rays, peaking around 250 MeV and lasting for 1/10 of a microsecond or longer depending on particle physics. In this work we show that there is an observational window using ground-based imaging Cerenkov detectors to measure gamma-ray burst emission at energies E > 200 MeV. This technique, with a sensitivity for bursts lasting nanoseconds to several microseconds, is based on the detection of multiphoton-initiated air showers.

New Ground-Based Arrays to Probe Cosmic Powerhouses

GAMMA RAY ASTRONOMYTOKYO-- The highest energy gamma rays elude satellite-based detectors because of their poor angular resolution. So, in a flurry of construction in deserts and on mountain peaks, astronomers are building arrays of reflectors and light detectors designed to pick up the faint glow produced when gamma ray photons slam into the upper atmosphere. Built at a tiny fraction of the cost of satellites, these telescopes should help unlock the mysteries behind high-energy sources of photons such as gamma ray bursts, supernovae, and the black hole-powered infernos called blazars, which are the most powerful and puzzling phenomena in the universe.

A search for very high energy bursts

Of great importance in distinguishing between models for gamma-ray bursts (GRBs) is the experimental determination of the highest energy gamma rays associated with bursts. The EGRET detection of a 15 GeV gamma ray indicates that the spectra of at least some bursts extend well beyond the several MeV limit of the BATSE detectors (Hurleyet al., 1994). The low expected flux means that the collecting area of the present generation of satellite-based detectors is too small to detect gamma rays much above this energy efficiently, and such searches are currently undertaken with ground based detectors. In this paper searches made for very high energy GRBs with a southern hemisphere air shower particle array are described.

FIGARO IV: Large-area balloon-borne telescope to study rapid time variabilities in the gamma-ray sources at energies above 50 MeV

We present a new γ-ray telescope based on the Limited Streamer Tube technology, used as tracking chambers to detect photons above 100 MeV. This technique allows to obtain very large sensitive areas (16 m2 in our experiment), together with a good angular resolution for payloads embarcable in high-altitude balloon flights. The capability to collect a large signal in a short exposure time makes the telescope particularly suitable and competitive with respect to satellite-based detectors for studying both periodic and random time variabilities on galactic and extragalactic γ-ray sources.