THE FERMI GAMMA-RAY BURST MONITOR

By C. Meegan, G. Lichti, P. N. Bhat, E. Bissaldi, M. S. Briggs, V. Connaughton, R. Diehl, G. Fishman, J. Greiner, A. Hoover and 11 more. 2009

1,020 citations recorded by the source corpus.

The Gamma-Ray Burst Monitor (GBM) will significantly augment the science return from the Fermi Observatory in the study of gamma-ray bursts (GRBs). The primary objective of GBM is to extend the energy range over which bursts are observed downward from the energy range of the Large Area Telescope (LAT) on Fermi into the hard X-ray range where extensive previous data sets exist. A secondary objective is to compute burst locations onboard to allow re-orienting the spacecraft so that the LAT can observe delayed emission from bright bursts. GBM uses an array of 12 sodium iodide scintillators and two bismuth germanate scintillators to detect gamma rays from ∼8 keV to ∼40 MeV over the full unocculted sky. The onboard trigger threshold is ∼0.7 photons cm−2 s−1 (50–300 keV, 1 s peak). GBM generates onboard triggers for ∼250 GRBs per year.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Radiation

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In Astronomy and Astrophysics

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4. B. Metzger
5. E. Liang
6. A. Pe’er
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In Nuclear and High Energy Physics

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In Radiation

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4. Shrinivas R. Kulkarni
5. Binbin Zhang
6. Joshua S. Bloom
7. R. Cameron
8. M. Koss

Citations in the corpus

• An Ordinary Short Gamma-Ray Burst with Extraordinary Implications: Fermi-GBM Detection of GRB 170817A (2017, background): “The other two detectors are composed of bismuth germanate (BGO) crystals, cover an energy range of 200 keV–40 MeV, and are placed on opposite sides of the spacecraft.”
• Detection of a Spectral Break in the Extra Hard Component of GRB 090926A (2011, background): “…Space Telescope hosts two instruments, the Large Area Tele- scope (LAT, 20 MeV to more than 300 GeV; Atwood et al. 2009) and the Gamma-ray Burst Monitor (GBM, 8 keV–40 MeV; Meegan et al. 2009), which together are capable of measuring the spectral parameters of GRBs across seven decades in energy.”
• Terrestrial gamma‐ray flashes in the Fermi era: Improved observations and analysis methods (2013, background): “[7] GBM extends the energy range of Fermi, observing from 8 keV to 40 MeV with two types of scintillation detectors [Meegan et al., 2009].”
• THE SECOND FERMI GBM GAMMA-RAY BURST CATALOG: THE FIRST FOUR YEARS (2014, methodology): “The GBM instrument is described in more detail in Meegan et al. (2009).”
• THE SECOND FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS (2013, methodology): “Fermi was launched on 2008 June 11, carrying two gamma-ray instruments: the LAT and the Gamma-ray Burst Monitor (Meegan et al. 2009); the latter was not used to prepare this catalog.”
• Spectral properties of 438 GRBs detected by Fermi/GBM (2010, methodology): “The other instrument on boardFermi is the GBM (Meegan et al. 2009) which is similar to BATSE and, despite its slightly worse sensitivity, allows to study the GRB spectrum over an unprecedented wide energy range, from 8 keV to 40 MeV.”
• The 105-Month Swift-BAT All-sky Hard X-Ray Survey (2018, result): “Our results for the Crab nebula are consistent with those reported Wilson-Hodge et al. (2011) with a ∼ 7% decline in the 15− 50 keV band from the observation of the Fermi Gamma-ray Burst Monitor (Meegan et al. 2009).”
• THE AFTERGLOW OF GRB 130427A FROM 1 TO 1016 GHz (2013, methodology): “Consequently, the BAT trigger time does not provide a useful reference time for the burst; we instead employ the Fermi Gamma-Ray Burst Monitor (GBM; Meegan et al. 2009) trigger time of 07:47:06.42 (von Kienlin 2013) as t0 in all of our subsequent analyses, an adjustment of 50.58 s for times…”
• Gamma-ray bursts in the comoving frame (2011, methodology): “Most of theEobspeak were determined by the Konus–Wind satellite (Aptekar et al.1995), or, since mid 2008, by the Gamma Burst Monitor (GBM; Meegan et al. 2009 with energy bandpass 8 keV–35 MeV) on board theFermi satellite.”
• GRB110721A: AN EXTREME PEAK ENERGY AND SIGNATURES OF THE PHOTOSPHERE (2012, background): “On 21 July 2011 the Gamma-Ray Burst Monitor (GBM; Meegan et al. 2009) and the Large Area Telescope (LAT; Atwood et al. 2009) onboard Fermi detected high energy emission from GRB110721A (GCNs 12187, 12188).”
• A COMPREHENSIVE ANALYSIS OF FERMI GAMMA-RAY BURST DATA. I. SPECTRAL COMPONENTS AND THE POSSIBLE PHYSICAL ORIGINS OF LAT/GBM GRBs (2010, background): “The two instru- ments on board Fermi, the Gamma-ray Burst Monitor (GBM; Meegan et al. 2009) and the Large Area Telescope (LAT; Atwood et al. 2009), provide an unprecedented spectral coverage for 7 orders of magnitude in energy (from ∼8 keV to ∼300 GeV).”
• IDENTIFICATION AND PROPERTIES OF THE PHOTOSPHERIC EMISSION IN GRB090902B (2009, background): “…theFermi Gamma-ray Space Telescope which regularly observes GRBs with its two instruments, the Large Area Telescope (LAT, nominal energy range 20 MeV–>300GeV; Atwood et al. 2009) and the Gamma-ray Burst Monitor (GBM, 8 keV–40MeV; Meegan et al. 2009), thus covering an unprecedented spectral range.”
• AFTERGLOW OBSERVATIONS OF FERMI LARGE AREA TELESCOPE GAMMA-RAY BURSTS AND THE EMERGING CLASS OF HYPER-ENERGETIC EVENTS (2010, methodology): “…energy release (the Ep–Eγ,iso, or “Amati” relation; Amati 2006), MeV/GeV events detected by either the Gamma-Ray Burst Monitor (GBM, 8 keV – 40MeV; Meegan et al. 2009) or the Large Area Telescope (LAT, 20MeV – 300GeV; Atwood et al. 2009) onboard Fermi preferentially select a sample of GRBs…”
• FERMI GBM OBSERVATIONS OF LIGO GRAVITATIONAL-WAVE EVENT GW150914 (2016, background): “GBM consists of 12 Thallium-doped Sodium Iodide (NaI) detectors with a diameter of 12.7 cm and a thickness of 1.27 cm and two Bismuth Germanate (BGO) detectors with a diameter and thickness of 12.7 cm (Meegan et al. 2009).”
• High-Energy Atmospheric Physics: Terrestrial Gamma-Ray Flashes and Related Phenomena (2012, background): “Fermi observes TGFs in its Gamma-ray Burst Monitor (GBM) instrument (Meegan et al. 2009).”