2013A&A...558A..37C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST02:41:38

2013A&A...558A..37C - Astronomy and Astrophysics, volume 558A, 37-37 (2013/10-1)

Calibration of AGILE-GRID with in-flight data and Monte Carlo simulations.

CHEN A.W., ARGAN A., BULGARELLI A., CATTANEO P.W., CONTESSI T., GIULIANI A., PITTORI C., PUCELLA G., TAVANI M., TROIS A., VERRECCHIA F., BARBIELLINI G., CARAVEO P., COLAFRANCESCO S., COSTA E., DE PARIS G., DEL MONTE E., DI COCCO G., DONNARUMMA I., EVANGELISTA Y., FERRARI A., FEROCI M., FIORETTI V., FIORINI M., FUSCHINO F., GALLI M., GIANOTTI F., GIOMMI P., GIUSTI M., LABANTI C., LAPSHOV I., LAZZAROTTO F., LIPARI P., LONGO F., LUCARELLI F., MARISALDI M., MEREGHETTI S., MORELLI E., MORETTI E., MORSELLI A., PACCIANI L., PELLIZZONI A., PEROTTI F., PIANO G., PICOZZA P., PILIA M., PREST M., RAPISARDA M., RAPPOLDI A., RUBINI A., SABATINI S., SANTOLAMAZZA P., SOFFITTA P., STRIANI E., TRIFOGLIO M., VALENTINI G., VALLAZZA E., VERCELLONE S., VITTORINI V. and ZANELLO D.

Abstract (from CDS):

AGILE is a γ-ray astrophysics mission which has been in orbit since 23 April 2007 and continues to operate reliably. The γ-ray detector, AGILE-GRID, has observed Galactic and extragalactic sources, many of which were collected in the first AGILE Catalog. We present the calibration of the AGILE-GRID using in-flight data and Monte Carlo simulations, producing instrument response functions (IRFs) for the effective area (Aeff), energy dispersion probability (EDP), and point spread function (PSF), each as a function of incident direction in instrument coordinates and energy. We performed Monte Carlo simulations at different γ-ray energies and incident angles, including background rejection filters and Kalman filter-based γ-ray reconstruction. Long integrations of in-flight observations of the Vela, Crab and Geminga sources in broad and narrow energy bands were used to validate and improve the accuracy of the instrument response functions. The weighted average PSFs as a function of spectra correspond well to the data for all sources and energy bands. Changes in the interpolation of the PSF from Monte Carlo data and in the procedure for construction of the energy-weighted effective areas have improved the correspondence between predicted and observed fluxes and spectra of celestial calibration sources, reducing false positives and obviating the need for post-hoc energy-dependent scaling factors. The new IRFs have been publicly available from the AGILE Science Data Center since November 25, 2011, while the changes in the analysis software will be distributed in an upcoming release.

Abstract Copyright:

Journal keyword(s): instrumentation: detectors - methods: data analysis - techniques: image processing - telescopes - gamma rays: general

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4803 1
2 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5594 4
3 IC 443 SNR 06 18 02.7 +22 39 36           ~ 1100 1
4 NAME Geminga Psr 06 33 54.153 +17 46 12.91           ~ 1092 0
5 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1110 2
6 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545           ~ 2056 1

    Equat.    Gal    SGal    Ecl

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2020.07.04-02:41:38

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