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3 EDGE piro

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Published on November 1, 2007

Author: Herminia

Source: authorstream.com

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EDGE Explorer of the Diffuse emission and GRB Explosions Science Review :  EDGE Explorer of the Diffuse emission and GRB Explosions Science Review Luigi Piro IASF/INAF - Rome Contributors from present WGs:  Contributors from present WGs Science Drivers Cluster Evolution and physics: Molendi, Ettori, Borgani, Campana, Brunetti, Kaastra, Girardi, Guzzo Mazzotta, Roncarelli WHIM: Branchini, Ohashi, Corsi, DeRosa, DelSanto, Galeazzi, Kaastra, Moscardini, Nicastro, Ursino, Viel, Shaye, LP GRB: Amati, Kawai, Campana, Corsi, Galli, Gendre, Ghirlanda,Ghisellini, Nicastro, LP Cosmic Vision Related and aux. science EOS-NS/compact: in’t Zand, Natalucci, Bazzano, Cocchi, Mendez, Ubertini Instrument Herder, Pareschi, de Korte, Tawara, Holland, Feroci, Natalucci, Barbera, Campana, Colasanti, Gatti, Labanti, Mineo, Mitsuda, Ohashi Science Drivers:  Science Drivers Evolution of the Universe probed by : Diffuse X-ray Emission from large scale structures: WHIM and clusters are distributed in a filamentary network shaped by the gravitational pull of the dark matter and whose evolution depends also on dark energy EOS GRB Mission profile:  Mission profile Localize in the sky and folllow-up with fast reaction GRB at their brightest levels, thus allowing high resolution (1-3 eV) spectroscopy. Observing and surveying diffuse sources (cluster and WHIM) with a wide field X-ray telescope (1 deg, 10” HEW over the whole FOV), allowing high sensitivity/low background measurements Synergy of spectroscopy and imaging (WHIM, clusters) fast reaction for GRB (WHIM in absorption) with WHIM in emission Cosmic Vision related and Auxiliary Science:  Cosmic Vision related and Auxiliary Science Resulting from mission capabilities (fast reaction, spectroscopy, wide field) Extreme physics of GRB, EOS of NS, compact objects, AGNs, SNR Surveys (from stars to AGN) Deep fields (about 20 sq. degrees) at flux limit of 10-16 cgs. High resolution spectra (2eV) down to 10-15 cgs Dark matter and v’s X-ray counterparts to GW from SMBH binary mergers …. GRB: The brightest and most distant sources:  GRB: The brightest and most distant sources E(iso) up to 1053-1054 erg in few seconds Observing a mid-bright GRB afterglow with a fast (min.) pointing with 1000 cm2 telescope yields 106 X-ray photons, and 103 cts in 1 eV resolution bin Talk by Amati, Kawai GRBs as cosmological beacons :  GRBs as cosmological beacons  Gamma-Ray Bursts as beacons to probing the WHIM properties through high resolution absorption studies measuring the cosmic history of metals in star forming regions and their host galaxies pinpoint the formation of early population of luminous sources ignited in the dark Universe (z>7) Derive the luminosity-redshift relation of GRB as potential probe of Dark Energy How: 150 GRBs with afterglow fluence >10-6 c.g.s. (and Epeak of the prompt emission). Reqs.: med-bright events (WFM with FOV>3sr), fast reaction (1min), 1000cm2, 1-3 eV resolution, 0.1-3 keV GRB: Tomography of the Universe I:  GRB: Tomography of the Universe I Map the metal evolution vs z Simulation of X-ray edges produced by metals (Si, S, Fe) by a medium with column density NH=5 1022 cm-2 with solar-like abundances in the environs of a bright GRB at z=5., as observed (1min to 60 ksec) Fe Si S X-ray redshift ! Talk by Campana Redshift AND Metal abundances:  Redshift AND Metal abundances Redshift from resonant (narrow) absorption lines in GRBs:  Redshift from resonant (narrow) absorption lines in GRBs F=2 10-6 z=1, NH=1E21, NeII and OI, dz/z=10-4 ! NeII@14.6Å OI@23.5Å NeII@14.6Å=>29.2Å Talk by Nicastro Slide11:  talk by Ghirlanda GRBs as standard candles for cosmology The Evolution of large scale structures :  The Evolution of large scale structures Characterize the WHIM through absorption (via GRB) and emission measurements Reqs: 2eV resolution, fast repointing, 1000 cm2 Evolution of physical and chemical properties of clusters from the present to their formation epoch (+ potential probes of dark energy) Deep and medium surveys long observations of a selected sample of bright objects to characterize the physical, dynamical and chemical structure from cluster core to the outskirt (virial radius). Reqs: resolve most of the XRB from discrete sources ( and low instrumental bkg: HEW 10” constant over 1deg, 1000cm2 combined with high res. spectroscopy study the interface (i.e. density, metal enrichment) between the cluster outskirt and the WHIM Slide13:   Probing the WHIM in absorption with GRBs WHIM filaments in Absorption with GRBs:  WHIM filaments in Absorption with GRBs From 150 GRBs with afterglow Fluence>10-6 cgs 150-600 WHIM OVII filaments and 20-40 with 2 or more lines Talk by Branchini WHIM Emission:  WHIM Emission Box # 4: 0.202<z<0.275 Talk by Galeazzi, Ohashi Spectrum :  Spectrum FOV=3’ A filament is in the FOV and O lines are clearly present Slide18:  100 ks 1 Ms 70% (50%) of the mass of WHIM produces OVII line detectable by EDGE in 1 Msec (100 ksec) observation for a bin of 3’ Cluster evolution and physics:  Cluster evolution and physics Long observations of a selected sample of bright objects (10-15) to characterize the physical, dynamical and chemical structure from cluster core to the outskirt (virial radius). The determination of the luminosity and temperature at the virial radius (where most of the mass of the cluster resides) is a major challenge in the field, and it is achieved by EDGE by resolving most of the XRB in discrete sources, and by the low instrumental bkg in low earth orbit Talk by Ettori Cluster surveys :  Cluster surveys The goal is to characterize most of the cluster evolutionary properties up to the formation era With deep (1Ms) pointings all the clusters (with T>1 keV) parameters (L,T,Abund,z) Talk by Molendi EDGE LET spectrum of a typical cluster of 2 keV (L=1044 erg/s) at z=1, F=1.4 10-14 A mid-bright cluster of 1 keV (L=1043 erg/s) at z=1, F=1.4 10-15 Preliminary Strawman Observing programme:  Preliminary Strawman Observing programme Assure that most of science driver science is fulfilled in 3 years Observatory mode (Guest Investigator) for ¼ of the time Note: aux.science for survey data (>120.000 sources down to 10-16 cgs, substantial fraction (f>10-15) with microcalorimeter spectra Net observing time in 3 years (0.8 efficiency thanks to smart pointing, small influence from SAA) = 76 Msec Science Driver 3 yr Programme : 36 Deep pointings (1Msec each): 36 Ms 10 on bright clusters 26 for WHIM, cluster deep surveys and br.clusters nearby fields 50-100 Med-deep pointings (100 ksec each): 5-10 Ms Cluster survey 300 med pointings (50 ksec each, fast reaction): 15 Ms WHIM in absorption, GRB cosmology

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