1L. Piro : Xenia and the WHIM - HEAD 2010
The XENIA mission and the missing barions
Luigi Piro, C. Kouveliotou, J.W. den Herder, T. Ohashi, D. Hartmann, D.
Burrowsand the WHIM team:
E. Branchini, Y Takei, E. Ursino, M. Galeazzi, F. Nicastro, L. Amati, A.
Corsi, J. Kaastra, F. Paerels, M.Viel, L. Moscardini, M. Roncarelli
2L. Piro : Xenia and the WHIM - HEAD 2010
z
10
1
0Stars Galaxies Clusters Filaments
Structure size
Structure Formation
GRB as cosmological beacons: fast reaction, high res. absorption spectroscopy
High resolution spectroscopy and spatial resolution, wide field in emission
Most of the baryon of the Universe are locked in large scale, low density structures visible only in X-rays
HOW ?
3L. Piro : Xenia and the WHIM - HEAD 2010
XENIA: Mission and Payload
TED: Transient Event Detector¼ of the sky, 3’ localization8-200 keV
CRIS: Cryogenic Imaging Spectrometer [email protected] keV TES DE<2.5eVField=1.0° ang.res=3’
HARI: High Angular Resolution Imager1000cm2@1keV 0.3-8 keV CCDField=1.4° ang.res=10” constant
• Low bkg: LEO
equatorial• Autonomous
fast pointing in 60 s
• 2 tons • TRL4• Decadal
Survey • medium
size
4L. Piro : Xenia and the WHIM - HEAD 2010
Exploring a new region of the Cosmic web
Hot (clusters)
WHIM
Cold DiffuseStar forming
Cluster @Virial r.
Branchini et al 2009
5L. Piro : Xenia and the WHIM - HEAD 2010
Tomography of the Universe: the X-ray forest from the Cosmic
Web with GRBs
From 150 GRBs with afterglow Fluence>2 10-6 cgs
~200s OVII-OVIII filaments in 5 years
6L. Piro : Xenia and the WHIM - HEAD 2010
3D mapping of the Cosmic Web
Detected, OVII+OVIII in emission, 5 s, 1 Ms
Model, Dz=0.02 @z=0.22
5x5°
Down to overdensities of 30
7L. Piro : Xenia and the WHIM - HEAD 2010
WHIM Angular Correlation • Xenia HARI • Remove 50%
bright pixels (dominated by hot dense gas phase) + 2000 AGN + foreground
• Galeazzi talk, Ursino & Branchini, Nicastro et al
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Summary• Xenia unique capabilities wrt WHIM : fast
reaction to GRB, high spectral resolution with wide field of view– probe at least 200 filaments in absorption by
exploiting bright GRB afterglows – Afterglow decay allows follow up observation of the
same filament region in emission, providing a unique abs+emission measurement
– Deep wide field (5x5) spectroscopy in emission: tomography of the WHIM up to z=0.5 (about 104 OVII+OVIII line measurements)
• Wide Field High Angular resolution:– ACF of the WHIM
• Proposal to ASTRO2010 as medium size mission
• More info: http://sms.msfc.nasa.gov/xenia/
9L. Piro : Xenia and the WHIM - HEAD 2010
Back up slides
10L. Piro : Xenia and the WHIM - HEAD 2010
Absorption
11L. Piro : Xenia and the WHIM - HEAD 2010
12L. Piro : Xenia and the WHIM - HEAD 2010
WHIM in emission• Spectrum from a 2.6’x2.6’ bin in 1 Ms by
Xenia CRIS
13L. Piro : Xenia and the WHIM - HEAD 2010
Whim in emission probed by Xenia
• Black line is the gas model distribution, Blu is the gas acessed by Xenia in 100 ksec, red in 1Ms, allowing access to lower density WHIM regions
14L. Piro : Xenia and the WHIM - HEAD 2010
Number of emission line detections
15L. Piro : Xenia and the WHIM - HEAD 2010
0.1 ph cm-2 s-1 sr-1 gives 50 line photons in a 2.5x2.5’ pixel of Xenia/CRIS in 1Ms
16L. Piro : Xenia and the WHIM - HEAD 2010
Tracing clusters at virial radius
17L. Piro : Xenia and the WHIM - HEAD 2010
Spectroscopy: fast reaction and wide field
• Line spectroscopy merit factor for variable sources = S/N for EW=1eV for a typical GRB afterglow
18L. Piro : Xenia and the WHIM - HEAD 2010
Observing programme
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20L. Piro : Xenia and the WHIM - HEAD 2010
Xenia will trace the cosmic history of baryons
Gamma-Ray Bursts• Evolution of massive star
formation using GRBs to trace their explosions back to z > 8)
• Measure the metals in the host galaxies of GRBs and the explosive enrichment in their close environment out to z>8Clusters of Galaxies
• Trace the evolution and physics of clusters out to their formation epoch (z>1)
• Measure the thermodynamical and chemical properties of a fair sample out to the virial radius Cosmic Web• Detect the largest reservoir
of baryons from z~1 to the present time by measuring densities ~30 times smaller
21L. Piro : Xenia and the WHIM - HEAD 2010
CRIS
• Mirror: 2/4 reflection• TES microcalorimeter
22L. Piro : Xenia and the WHIM - HEAD 2010
HARI
• Mirror: Polynomial profile with constant PSF
• CCD
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TED
• 2 Coded Mask / CZT detectors
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Angular Correlation
Remove 50% brightest pixels
Normalized to Total Flux
