EDGE Explorer of Diffuse Emission and GRB explosions: The Science Case

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EDGEExplorer of Diffuse EmissionandGRB
explosionsThe Science Case
L. Piro, J.W. den Herder, T. Ohashi, on behalf
of the EDGE collaboration
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EDGE Working Groups

• Science GRB L. Amati , J.L. Atteia, S.
  Barthelmy, M. Boer, M. Briggs, D. Burrows, S.
  Campana, A. Corsi, A. Galli, B. Gendre, N.
  Gehrels, G. Ghirlanda, G. Ghisellini, N. Kawai,
  C. Kouveliotou, F. Nicastro, P. O Brien, J.
  Osborne, G. Sato, D.Willingale, R. Wijers
• Science WHIM E. Branchini, Schaye, M. Galeazzi,
  F. Paerels, E. Ursino, Y. Suto, K. Yoshikawa, Y.
  Takei, H. Kawahara, S. Sazaki, M. Viel, W.
  Hermsen.
• Science Cluster S. Molendi, S. Ettori, Borgani,
  Kaastra, Campana, P. Tozzi, P. Mazzotta, M.
  Girardi, T. Ponman, L. Guzzo, P. Rosati
• Cosmic Vision-related / Aux. Science J. In t
  Zand, S. Paltani, M. Mendez, J. Schmitt, S.
  Sciortino, G. Branduardi-Raymont, M. Page,
  Shaposhnilokov, A. Comastri, F. Haardt, R.
  Salvaterra, O. Boyarski. T. Tsuru, J. Vink, G.
  Matt, D. Barret
• Instruments and Mission WFS Tawara, de Korte,
  H. Hoevers, N. Yamasaki, I. Sakurai, Gatti, J.
  Hepburn, Mineo, M. Barbera, E. Perinati, L.
  Colasanti, C. Macculi, l. Ferrari, Mitsuda, WFI
  Pareschi, A. Holland, Paolo P., S.Campana,
  WFM(GRBM) M. Feroci, D. Barret, C
  Budtz-Jorgensen, L. Natalucci, Ubertini,
  Quadrini, C.Labanti, Kouveliotou, Briggs,
  Spacecraft Alcatel Alenia Spazio (P. Attina et
  al)
• And other people.

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Primary ESA CV themes for X-ray missions

• 3.What are the fundamental physical laws of the
  Universe?
• 3.3 Matter under extreme conditions
• 4. How did the Universe originate and what is it
  made of?
• 4.1 The early Universe
• 4.2 The Universe taking shape
• 4.3 The evolving violent Universe

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ScienceDrivers

• Evolution of the Universe probed by
• 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 as cosmological beacons

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Mission profile

• Observing with fast reaction transient sources,
  like GRB, at their brightest levels, thus
  allowing high resolution spectroscopy.
• Observing and surveying through two X-ray
  telescopes with a wide field of view and low
  background (high angular and high spectral
  resolution) extended sources, like cluster and
  WHIM 

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EDGE Mission and Payload
Wide Field Imager 1000cm2_at_1keV 0.3-8 keV
CCD Field1 ang.res15 constant
Vega Launcher 2 tons in LEO ilt5 Autonomous
fast (1 min) pointing

Wide Field Spectrometer 1000cm2_at_0.5keV 0.1-3
keV TES DE3eV Field0.7 ang.res2
Wide Field Monitors ¼ of the sky, 3
localization 8-200 keV
Gamma-Ray Burst Monitor 25 keV 2 MeV
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Exploring a new region of the Cosmic web
Hot (clusters)
Diffuse WHIM (filaments)
Dense WHIM (groups)
Cold Diffuse
Star forming
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The Evolution of large scale structures

• Characterize the WHIM
• through absorption (via GRB) and emission
  measurements
• Evolution of physical and chemical properties of
  clusters from formation epoch
• 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).
• Study the connection between the cluster
  outskirts and the WHIM

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Tomography of the Universe with GRBs the X-ray
forest from the Cosmic Web
?
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WHIM filaments in Absorption with GRBs
From 150 GRBs with afterglow Fluencegt10-6 cgs
150-600 WHIM OVII filaments and 20-40 with 2 or
more lines in 3 years
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Image of Cosmic Web in Oxygen lines (DE2 eV)
Significance gt 5s
Effective area 1000 cm2
OVII line
105 sec
106 sec
OVIII line
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Cluster evolution and physics

• Long observations of a selected sample of bright
  objects (10-15) to characterize the physical,
  dynamical and chemical structure especially in
  the outskirts.
• The determination of the surface brightness and
  temperature in clusters outskirt radius (where a
  sizeable mass of the cluster resides) is a major
  challenge. EDGE achieves it by resolving most of
  the XRB in discrete sources, and by the low
  instrumental bkg in low earth orbit.

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Tracing clusters at virial radius

• Surface brightness image for a cosmological
  simulation of a cluster at a redshift of 0.05
• XMM-like EDGE

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Tracing clusters at virial radius

• Spectrum from EDGE spectrometer at OVIII

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Tracing clusters at virial radius

• Spectrum from EDGE spectrometer at OVIII
• Removing 65 CXB Imager point sources

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Cluster survey with the Imager
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Cluster surveys with Spectrometer
Spectrum of a typical cluster of 2 keV (L1044
erg/s) at z1, F1.4 10-14
A mid-bright cluster of 1 keV (L1043 erg/s) at
z1, F1.4 10-15
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EDGE GRBs as cosmological beacons

•  Gamma-Ray Bursts as beacons to
• probe the missing baryons through high
  resolution absorption studies.
• measure the cosmic history of metals in GRB
  regions and their host galaxies
• pinpoint the formation of early population of
  luminous sources ignited in the dark Universe
  (zgt7)
• Derive the luminosity-redshift relation of GRB
  and, if proven, use to constrain the Dark Energy

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GRBs Lighthouses in the Universe

• About 10 GRBs at zgt5
• About 90 have a X-ray afterglow, 20-40 are dark
• High z events are dark (Lya forest absorption at
  zgt6)
• The only way to get the redshift X-ray and IR
• 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
• Golden sample of gt150 GRBs in 3 years (high res.
  X-ray redshift, metals), good measurement of
  prompt luminosity and Epeak

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X-ray absorption in the GRB local environment

• X-ray absorption column densities in the
  afterglow NH1021-22 cm-2 (Stratta et al 2000,
  Campana et al 2006)

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GRB Tomography of the Universe

• Map the metal evolution vs z

Simulation of X-ray edges produced by metals (Si,
S, Fe) by a medium with column density NH5 1022
cm-2 with solar-like and 1/10 abundances in the
environs of a bright GRB at z5., 10 as observed
(1min to 60 ksec) by EDGE
X-ray redshift !
Fe
S
0.2
0.1
9
10
11
z
Si
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Narrow abs lines from ISM in our own host galaxy

• Bright galactic binary (1820-303) observed with
  Chandra grating (Yao and Wand 2006)

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ISM (and redshift) from absorption lines in GRBs
host galaxies
F2 10-6 z1, NH1E21, NeII and OI, dz/z10-4 !
NeII_at_14.6Ågt29.2Å
OI_at_23.5Å
NeII_at_14.6Å
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Potential use of GRBs to estimate Cosmological
parameters
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Survey
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Cosmic Vision related and Auxiliary Science

• Extreme physics of GRB, EOS of NS, compact
  objects.
• Feedback in action SNR, ISM, AGNs
• Surveys (stars, AGN)
• Dark matter and vs
• X-ray counterparts to GW from cosmological Binary
  BH mergers
• Solar system

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Observing Programme

• Efficiency (LEO, smart pointing)gt80
• Science drivers achieved in 3 years (54 Ms)
• WHIM emission and cluster deep (F?10-16 cgs)
  contiguous field (2.8x2.8) 16 Ms
• Cluster medium (F?10-15 cgs) sensitivity survey
  (100 x 50ksec) in a contiguous field 5 Ms
• Cluster sample (9 objects) 17 x 1 Ms
• WHIM emission studies of LOS from absorption
  4x1Ms
• GRB (WHIM absorption, history metals, isotropic
  non contiguous medium sensitivity survey)
  240x50ksec 12 Ms
• ¼ of the time open to Guest Investigator in the
  first 3 years (19 Ms)
• Science Drivers observations open to the
  community

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Summary

• Exciting science (GRB, WHIM, cluster) addressing
  CV 4 and 3
• Science drivers achieved in 3 years (CP data
  available to the community), plus ¼ of the first
  3 years time for Guest Investigators Programme
• Medium class mission to ESA Cosmic Vision
• Unique and Complementary to other missions (large
  grasp, fast reaction, high spectral resolution)