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Title:
EDGE: Explorer of diffuse emission and gamma-ray burst explosions
Authors:
Piro, L.; den Herder, J. W.; Ohashi, T.; Amati, L.; Atteia, J. L.; Barthelmy, S.; Barbera, M.; Barret, D.; Basso, S.; Boer, M.; Borgani, S.; Boyarskiy, O.; Branchini, E.; Branduardi-Raymont, G.; Briggs, M.; Brunetti, G.; Budtz-Jorgensen, C.; Burrows, D.; Campana, S.; Caroli, E.; Chincarini, G.; Christensen, F.; Cocchi, M.; Comastri, A.; Corsi, A.; Cotroneo, V.; Conconi, P.; Colasanti, L.; Cusumano, G.; de Rosa, A.; Del Santo, M.; Ettori, S.; Ezoe, Y.; Ferrari, L.; Feroci, M.; Finger, M.; Fishman, G.; Fujimoto, R.; Galeazzi, M.; Galli, A.; Gatti, F.; Gehrels, N.; Gendre, B.; Ghirlanda, G.; Ghisellini, G.; Giommi, P.; Girardi, M.; Guzzo, L.; Haardt, F.; Hepburn, I.; Hermsen, W.; Hoevers, H.; Holland, A.; in't Zand, J.; Ishisaki, Y.; Kawahara, H.; Kawai, N.; Kaastra, J.; Kippen, M.; de Korte, P. A. J.; Kouveliotou, C.; Kusenko, A.; Labanti, C.; Lieu, R.; Macculi, C.; Makishima, K.; Matt, G.; Mazzotta, P.; McCammon, D.; Méndez, M.; Mineo, T.; Mitchell, S.; Mitsuda, K.; Molendi, S.; Moscardini, L.; Mushotzky, R.; Natalucci, L.; Nicastro, F.; O'Brien, P.; Osborne, J.; Paerels, F.; Page, M.; Paltani, S.; Pareschi, G.; Perinati, E.; Perola, C.; Ponman, T.; Rasmussen, A.; Roncarelli, M.; Rosati, P.; Ruchayskiy, O.; Quadrini, E.; Sakurai, I.; Salvaterra, R.; Sasaki, S.; Sato, G.; Schaye, J.; Schmitt, J.; Sciortino, S.; Shaposhnikov, M.; Shinozaki, K.; Spiga, D.; Suto, Y.; Tagliaferri, G.; Takahashi, T.; Takei, Y.; Tawara, Y.; Tozzi, P.; Tsunemi, H.; Tsuru, T.; Ubertini, P.; Ursino, E.; Viel, M.; Vink, J.; White, N.; Willingale, R.; Wijers, R.; Yoshikawa, K.; Yamasaki, N.
Affiliation:
AA(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), AB(SRON, the Netherlands Institute for Space Research), AC(Tokyo Metropolitan University), AD(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), AE(LAT, Observatoire Midi-Pyrénées), AF(NASA GSFC), AG(Dipartimento Scienze Fisiche e Astronomiche, Università di Palermo), AH(CESR Centre d'Étude Spatiale des Rayonnements), AI(INAF, Osservatorio Astronomico Brera), AJ(Observatoire de Haute Provence), AK(INAF, Osservatorio Astronomico), AL(CERN), AM(Università Roma III), AN(Mullard Space Science Lab/UCL), AO(University of Alabama in Huntsville), AP(INAF-IRA Bologna), AQ(DNSC/Technical University of Denmark), AR(Penn State University), AS(INAF, Osservatorio Astronomico Brera), AT(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), AU(INAF, Osservatorio Astronomico Brera), AV(DNSC/Technical University of Denmark), AW(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), AX(INAF, Osservatorio Astronomico Bologna), AY(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), AZ(INAF, Osservatorio Astronomico Brera), BA(INAF, Osservatorio Astronomico Brera), BB(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), BC(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), BD(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), BE(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), BF(INAF, Osservatorio Astronomico Bologna), BG(Institute of Space and Aeronautical Science, JAXA), BH(Istituto Nazionale di Fisica Nucleare), BI(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), BJ(University Space Research Association), BK(Marshall Space Flight Center), BL(Institute of Space and Aeronautical Science, JAXA), BM(University of Miami), BN(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), BO(Istituto Nazionale di Fisica Nucleare), BP(NASA GSFC), BQ(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), BR(INAF, Osservatorio Astronomico Brera), BS(INAF, Osservatorio Astronomico Brera), BT(ASI Data Center), BU(INAF, Osservatorio Astronomico), BV(INAF, Osservatorio Astronomico Brera), BW(Università di Insubria (Como)), BX(Mullard Space Science Lab/UCL), BY(SRON, the Netherlands Institute for Space Research), BZ(SRON, the Netherlands Institute for Space Research), CA(University of Brunel), CB(SRON, the Netherlands Institute for Space Research), CC(Nagoya University), CD(University of Tokyo), CE(Tokyo Institute of Technology), CF(SRON, the Netherlands Institute for Space Research), CG(Los Alamos National Laboratory), CH(SRON, the Netherlands Institute for Space Research), CI(Marshall Space Flight Center), CJ(UCLA), CK(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), CL(University of Alabama in Huntsville), CM(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), CN(Tokyo University of Science), CO(Università Roma III), CP(Università di Roma Tor Vergata), CQ(University of Wisconsin), CR(SRON, the Netherlands Institute for Space Research), CS(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), CT(Marshall Space Flight Center), CU(Institute of Space and Aeronautical Science, JAXA), CV(INAF, Istituto Astrofisica Spaziale e Fisica Cosmica), CW(Università di Bologna), CX(NASA GSFC), CY(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), CZ(INAF, Osservatorio Astronomico Roma), DA(Leicester University), DB(Leicester University), DC(Columbia University), DD(Mullard Space Science Lab/UCL), DE(Integral Science Data Center), DF(INAF, Osservatorio Astronomico Brera), DG(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), DH(Università Roma III), DI(University of Birmingham), DJ(KIPAC/Standord), DK(INAF, Osservatorio Astronomico Bologna), DL(ESO), DM(Institut des Hautes Etudes Scientifiques), DN(INAF, Istituto Astrofisica Spaziale e Fisica Cosmica), DO(Nagoya University), DP(Università di Insubria (Como)), DQ(Tokyo Metropolitan University), DR(NASA GSFC), DS(University of Leiden), DT(University of Hamburg), DU(INAF, Osservatorio Astronomico Palermo), DV(Ecole Polytechnique Fédérale de Lausanne), DW(Tokyo Metropolitan University), DX(INAF, Osservatorio Astronomico Brera), DY(University of Tokyo), DZ(INAF, Osservatorio Astronomico Brera), EA(Institute of Space and Aeronautical Science, JAXA), EB(SRON, the Netherlands Institute for Space Research), EC(Nagoya University), ED(INAF, Osservatorio Astronomico), EE(Osaka University), EF(Kyoto University), EG(INAF, Istituto Astrofisica Spaziale Fisica Cosmica), EH(University of Miami), EI(INAF, Osservatorio Astronomico), EJ(University of Utrecht), EK(NASA GSFC), EL(Leicester University), EM(University of Amsterdam), EN(University of Tokyo), EO(Institute of Space and Aeronautical Science, JAXA)
Publication:
Experimental Astronomy, Volume 23, Issue 1, pp.67-89 (ExA Homepage)
Publication Date:
03/2009
Origin:
SPRINGER
Keywords:
X-rays, Cosmology, Clusters, Gamma-ray bursts, Warm&ndash, hot intergalactic medium, Missions
DOI:
10.1007/s10686-008-9092-y
Bibliographic Code:
2009ExA....23...67P

Abstract

How structures of various scales formed and evolved from the early Universe up to present time is a fundamental question of astrophysical cosmology. EDGE (Piro et al., 2007) will trace the cosmic history of the baryons from the early generations of massive stars by Gamma-Ray Burst (GRB) explosions, through the period of galaxy cluster formation, down to the very low redshift Universe, when between a third and one half of the baryons are expected to reside in cosmic filaments undergoing gravitational collapse by dark matter (the so-called warm hot intragalactic medium). In addition EDGE, with its unprecedented capabilities, will provide key results in many important fields. These scientific goals are feasible with a medium class mission using existing technology combined with innovative instrumental and observational capabilities by: (a) observing with fast reaction Gamma-Ray Bursts with a high spectral resolution. This enables the study of their star-forming and host galaxy environments and the use of GRBs as back lights of large scale cosmological structures; (b) observing and surveying extended sources (galaxy clusters, WHIM) with high sensitivity using two wide field of view X-ray telescopes (one with a high angular resolution and the other with a high spectral resolution). The mission concept includes four main instruments: a Wide-field Spectrometer (0.1-2.2 eV) with excellent energy resolution (3 eV at 0.6 keV), a Wide-Field Imager (0.3-6 keV) with high angular resolution (HPD = 15'') constant over the full 1.4 degree field of view, and a Wide Field Monitor (8-200 keV) with a FOV of ¼ of the sky, which will trigger the fast repointing to the GRB. Extension of its energy response up to 1 MeV will be achieved with a GRB detector with no imaging capability. This mission is proposed to ESA as part of the Cosmic Vision call. We will outline the science drivers and describe in more detail the payload of this mission.
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