ISGRI: The INTEGRAL soft gamma-ray imager

By F. Lebrun, J. Leray, P. Lavocat, J. Cretolle, M. Arques, C. Blondel, C. Bonnin, A. Bouère, C. Cara, T. Chaleil and 14 more. 2003

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For the first time in the history of high energyastronomy, a large CdTe gamma-ray camera is operating in space. ISGRI is the low-energy camera of the IBIS telescope on board the INTEGRAL satellite. This paper details its design and itsin-flight behavior and performances. Having a sensitive area of 2621 cm$^2$ with a spatial resolution of 4.6 mm, a low threshold around 12 keV and an energy resolution of $\sim$ 8\% at 60 keV, ISGRI shows absolutely no signs of degradation after 9 months in orbit. All aspects of its in-flight behavior and scientific performance are fully nominal, and in particular the observedbackground level confirms the expected sensitivity of 1 milliCrab for a 10$^6$s observation.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering

View Paper: https://www.semanticscholar.org/paper/cc3de49f43523ae1d8e4b2dbdda9529078ba5202

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Citations in the corpus

THE FERMI GBM GAMMA-RAY BURST SPECTRAL CATALOG: THE FIRST TWO YEARS (2012, result): “The available reliable energy channels in the NaI detectors lie between ∼8 keV and ∼1 MeV.”
A Decade of Gamma-Ray Bursts Observed by Fermi-LAT: The Second GRB Catalog (2019, background): “…et al. 2005) onboard the Neil Gehrels Swift Observatory (Gehrels et al. 2004), and the International Gamma-Ray Astrophysics Laboratory Soft Gamma-Ray Imager (INTEGRAL/ISGRI; Lebrun et al. 2003) onboard the INTEGRAL Satellite (Winkler et al. 2003), or reported by the Interplanetary Network (IPN2).”
Polarization of the Crab Pulsar and Nebula as Observed by the INTEGRAL/IBIS Telescope (2008, background): “Events recorded in ISGRI and PiCsIT within the same time window of 3.8 µs are tagged as ’Compton’ events, but do not all result from Compton scattering.”
THE FOURTH IBIS/ISGRI SOFT GAMMA-RAY SURVEY CATALOG (2009, methodology): “The data are collected with the low-energy array, ISGRI (INTEGRAL Soft Gamma-Ray Imager; Lebrun et al. (2003)), consisting of a pixellated 128x128 CdTe solid-state detector that views the sky through a coded aperture mask.”
Unveiling Supergiant Fast X-Ray Transient Sources with INTEGRAL (2006, methodology): “The IBIS/ISGRI instrument (Ubertini et al. 2003, Lebrun et al. 2003) on board the INTEGRAL satellite (Winkler et al. 2003) is particularly suited to the detection of new or already known supergiant fast X-ray transient sources since it provides a very powerful combination of a large FOV, good…”
Probing clumpy stellar winds with a neutron star (2007, methodology): “…aim at studying the clumping of stellar wind in HMXB using the hard X-ray variability observed by the IBIS/ISGRI instrument (Ubertini et al. 2003; Lebrun et al. 2003) on board the INTErnational GammaRay Astrophysics Laboratory (INTEGRAL, Winkler et al. 2003) which could be used to probe clump…”
Discovery of Luminous Pulsed Hard X-Ray Emission from Anomalous X-Ray Pulsars 1RXS J1708–4009, 4U 0142+61, and 1E 2259+586 by INTEGRAL and RXTE (2006, methodology): “Next, only events with rise times between 7 and 90 (see Lebrun et al. 2003 for definition), detected in nonnoisy ISGRI detector pixels, which have an illumination factor of more than 25% (i.e., at least 25% of a detector pixel must have been illuminated by the target), are passed for further…”
INTEGRAL observations of the cosmic X-ray background in the 5–100 keV range via occultation by the Earth (2006, methodology): “A pure statistical error (joint fit to JEM-X, IBIS/ISGRI and SPI data) in the normalization of the CXB component is ∼1%.”
The Third IBIS/ISGRI Soft Gamma-Ray Survey Catalog (2006, methodology): “The data are collected with the low-energy array, ISGRI (INTEGRAL Soft Gamma-Ray Imager; Lebrun et al. (2003)), consisting of a pixellated 128x128 CdTe solidstate detector that views the sky through a coded aperture mask.”
INTEGRAL Discovery of a Burst with Associated Radio Emission from the Magnetar SGR 1935+2154 (2020, background): “ISGRI collects photon-by-photon events, tagged with a resolution of 61 μs, in the nominal 15–1000 keV energy range (Lebrun et al. 2003).”
INTEGRAL observations of recurrent fast X-ray transient sources (2005, background): “…and available at http://www.edpsciences.org/aa or http://dx.doi.org/10.1051/0004-6361:20053103 The IBIS/ISGRI detector (Ubertini et al. 2003; Lebrun et al. 2003) on board the INTEGRAL satellite (Winkler et al. 2003) is particularly suited to detect new or already known fast X-ray transient…”
INTEGRAL Detection of the First Prompt Gamma-Ray Signal Coincident with the Gravitational-wave Event GW170817 (2017, methodology): “We note that with this orientation, the sensitivity of IBIS (ISGRI, Lebrun et al. 2003; PICsIT, Labanti et al. 2003; Veto, Quadrini et al. 2003 detectors) to a signal from the direction of AT 2017gfo was much lower if compared to SPI-ACS for any plausible type of event spectrum.”
The PalermoSwift-BAT hard X-ray catalogue: II. Results after 39 months of sky survey (2009, background): “Today, the IBIS-ISGRI camera (Ubertini et al. 2003; Lebrun et al. 2003) on the INTEGRAL observatory (Winkler et al. 2003) with its field of view of 8◦×8◦ (fully coded) is carrying out a hard X-ray survey focussing mostly on the Galactic plane in the 20–150 keV energy band with sensitivity higher…”
An Embedded X-Ray Source Shines through the Aspherical AT 2018cow: Revealing the Inner Workings of the Most Luminous Fast-evolving Optical Transients (2018, methodology): “…the incident photon energies with the latest available calibration files, we extracted the hard X-ray spectrum from the ISGRI detector (Lebrun et al. 2003) on the IBIS instrument (Ubertini et al. 2003) of INTEGRAL (Winkler et al. 2003) for each of the ∼2 ks long individual pointing of…”
The INTEGRAL/IBIS scientific data analysis (2003, methodology): “…and 2 pixellated gamma-ray detector planes, both approx- imately of the same size of the mask basic pattern: ISGRI, the low energy band (15 keV - 1 MeV) camera (Lebrun et al. 2003) and PICsIT, sensitive to photons between 175 keV and 10 MeV, disposed about 10 cm below ISGRI (Di Cocco et al. 2003).”