Future mission for GRB and Xray cosmology: ESTREMOWFXRT

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Future mission for GRB and X-ray cosmology
ESTREMO/WFXRT
Luigi PiroIASF-INAF, Rome
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The Early Universe and its evolution to present
ages

• ESTREMO/WFXRT will use two different cosmological
  probes  Gamma-Ray Burts and large scale
  structures (Clusters of Galaxies and the cosmic
  network) to address this challenging goal by
  observing
• The X-ray cosmic web, filaments (WHIM Warm Hot
  Intragalactic Medium) of gas accreting onto Dark
  Matter structures.
• Outskirts of clusters (where most of the yet
  unobserved cluster mass is residing)
• Cluster surveys to constrain  Dark Energy.
•  Gamma-Ray Bursts as beacons to
• pinpoint the formation of first population of
  luminous sources ignited in the dark Universe
  (zgt7)
• measuring the cosmic history of metals in star
  forming regions
• probing the WHIM properties through high
  resolution absorption studies.
• Derive the luminosity-redshift relation of GRB as
  clues to the nature of the Dark Energy

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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 a X-ray telescope
  with a wide field of view and with high
  sensitivity extended sources, like cluster and
  WHIM 

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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 2000 cm2 telescope yields
106 X-ray photons, and 103 cts in 1 eV
resolution bin
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Dark GRB and the dark Universe

• About 20 of GRB are Dark (no optical afterglow)
• Very high extinction in dusty environment
• High z events (Lya forest absorption at zgt6)

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GRB050908 z6.3

• Kawai et al 2005

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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)
• Consistent with NH in Giant Molecular clouds

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GRB Tomography of the Universe I

• Map the metal evolution vs z

Simulation of X-ray edges produced by metals (Si,
S, Ar, Fe) by a medium with column density NH5
1022 cm-2 with 1/10 and solar-like abundances in
the environs of a bright GRB at z5., as observed
ESTREMO/WFXRT (1min to 60 ksec)
X-ray redshift !
Ar
S
Fe
Si
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The Early Universe and its evolution to present
ages

• ESTREMO/WFXRT will use two different cosmological
  probes  Gamma-Ray Burts and large scale
  structures (Clusters of Galaxies and the cosmic
  network) to address this challenging goal by
  observing
• The X-ray cosmic web, filaments (WHIM Warm Hot
  Intragalactic Medium) of gas accreting onto Dark
  Matter structures.
• Outskirts of clusters (where most of the yet
  unobserved cluster mass is residing) (Talk by S.
  Molendi)
• Cluster surveys to constrain  Dark Energy. (Talk
  by S. Molendi)
•  Gamma-Ray Bursts as beacons to
• pinpoint the formation of first population of
  luminous sources ignited in the dark Universe
  (zgt7)
• measuring the cosmic history of metals in star
  forming regions
• probing the WHIM properties through high
  resolution absorption studies.
• Derive the luminosity-redshift relation of GRB as
  clues to the nature of the Dark Energy

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The Early Universe and its evolution to present
ages

• ESTREMO/WFXRT will use two different cosmological
  probes  Gamma-Ray Burts and large scale
  structures (Clusters of Galaxies and the cosmic
  network) to address this challenging goal by
  observing
• The X-ray cosmic web, filaments (WHIM Warm Hot
  Intragalactic Medium) of gas accreting onto Dark
  Matter structures in emission
• Outskirts of clusters (where most of the yet
  unobserved cluster mass is residing)
• Cluster surveys to constrain  Dark Energy.
•  Gamma-Ray Bursts as beacons to
• pinpoint the formation of first population of
  luminous sources ignited in the dark Universe
  (zgt7)
• measuring the cosmic history of metals in star
  forming regions
• probing the WHIM properties through high
  resolution absorption studies.
• Derive the luminosity-redshift relation of GRB as
  clues to the nature of the Dark Energy

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Dark matter WHIM X-ray forest
Structure simulation from Cen Ostriker (1999)
?
Simulations of WHIM absorption features from OVII
as expected from filaments (at different z, with
EW0.2-0.5 eV from Hellsten et al 98) in the
l.o.s. toward a GRB with Fluence4 10-6 as
observed with ESTREMO/WFXRT (in 60 ksec). About
10 of GRB (10 events per year per 3sr).
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Detecting WHIM filaments in Absorption
N.of GRBs and WHIM filaments in 3 yrs
6 GRB, 60 filaments
60 GRB, 360 filaments
300 GRB, 600 filaments
500-1000 WHIM filaments detected in absorption
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Synthetic Absorption Spectra Hydro-model
(Borgani, Viel, et al)
Metallicity
Temperature
Density
OVII Density
OVIII Density
Redshift Slice z0.45,0.514
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WHIM Emission
Box 4 0.202ltzlt0.275
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Spectrum
FOV3 A filament is in the FOV and O lines are
clearly present
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100 ks
1 Ms
70 (50) of the mass of WHIM produces OVII line
detectable by ESTREMO/WFXRT in 1 Msec (100 ksec)
observation for a bin of 3
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The Early Universe and its evolution to present
ages

• ESTREMO/WFXRT will use two different cosmological
  probes  Gamma-Ray Burts and large scale
  structures (Clusters of Galaxies and the cosmic
  network) to address this challenging goal by
  observing
• The X-ray cosmic web, filaments (WHIM Warm Hot
  Intragalactic Medium) of gas accreting onto Dark
  Matter structures.
• Outskirts of clusters (where most of the yet
  unobserved cluster mass is residing)
• Cluster surveys to constrain  Dark Energy.
•  Gamma-Ray Bursts as beacons to
• pinpoint the formation of first population of
  luminous sources ignited in the dark Universe
  (zgt7)
• measuring the cosmic history of metals in star
  forming regions
• probing the WHIM properties through high
  resolution absorption studies.
• Derive the luminosity-redshift relation of GRB as
  clues to the nature of the Dark Energy

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GRB as standard candles dark energy investigation
GRBs

• Ghirlanda et al 2004, Amati et al 2002

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Dark energy from cluster survey

Haiman et al. (2005)
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Mission profile

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• Wide field monitor in the X/hard-X range to
  localize transients (gt1/4 of the sky)
• Fast (min) autonomous follow-up observations with
  X-ray telescope (2000 cm2) with
• High resolution X-ray spectroscopy (0.1-8 keV
  range, 2eV resolution below 2 keV with TES
  microcalorimeters)
• Wide field (1) for imaging with 10 resolution
  (CCD) for extended faint structures (risolve and
  subtract 70 of XRB) and cluster survey
• Low background 600 km equatorial orbit

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Wide Field XRT
X-ray optics with polynomial profile

• Mirrors are usually built in the Wolter I
  (paraboloid-hyperboloid) configuration which
  provides, in principle, perfect on-axis images.
• This design exhibits no spherical aberration
  on-axis but suffers from field curvature, coma
  and astigmatism, which make the angular
  resolution to degrade rapidly with increasing
  off-axis angles.
• More general mirror designs than Wolter's exist
  in which the primary and secondary mirror
  surfaces are expanded as a power series.
• These polynomial solutions are well suited for
  optimization purposes, which may be used to
  increase the angular resolution at large off-axis
  positions, degrading the on-axis performances
  (Burrows, Burgh and Giacconi 1992)
• The wide-field polynomial optics concept was
  extensively studied e.g as a part of the WFXT
  mission concept (OAB, CfA, Univ. of Leicester)

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WFXRT
Tests _at_ Panter-MPE Marshall XRF
WFXT (epoxy replication on SiC carrier) Ø 60
cm Focal Lenght 300 cm HEW 10 arcsec
Citterio et al. 1999, SPIE 3766 198
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Wide Field Imager

• Wide-field monitor Localization and study of
  GRB X-Ray transients
• 2-100 keV 2-3 arcmin resolution solid angle gt 3
  sr such that gt50-100 GRB per year and a similar
  number of transient sources)
• Detector Technologies CdZnTe, Si (Sagile-like),
  Si-drift
• Small omnidirectional spectrometer for GRB
  spectrum (Epeak)

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Spacecraft, launcher and Orbit

• Time to to slew to 60 degrees 60 sec (goal), 180
  sec (requirement)
• 3-axis stabilized, smart pointing
• Post facto attititude reconstruction lt10
• Zone of sun avoidance TBD
• Orbit LEO preferred for lower bkg and payload
  mass,
• P/L mass 750 kg
• P/L power 1000 W
• on-board memory upto 250 Gb
• downlink in S and X bands upto 512 kbps and
  210Mbps respectively during the passage
• VEGA launcher (upto 2200 kg)

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Assessment on P/L accomodation, launcher and fast
repointing

• Alcatel Alenia Space support
• Mass budget, size within VEGA capability
• Momentum of Inertia low enough for delivering
  fast repointing with standard Reaction Wheels

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X-ray vision

• ESTREMO/WFXRT characterized by unique and
  mostly complementary science wrt XEUS (wide
  fieldbright transients during their explosive
  phases vs faint sources)
• Some of the key hardware is similar cryogenic
  TES
• ESA Cosmic Vision call
• Small/mid size, 2016 launch time frame
  ESTREMO/WFXRT (NEW)
• Cornerstone, Large Observatory, post 2020 XEUS