NED New ESTREMO DIOS

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NED(New ESTREMO DIOS)

• J.W. den Herder

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Cosmic Vision

• What are the conditions for life and planetary
  formation?
• How does the Solar System work?
• What are the fundamental laws of the Universe?
• Explore limits of contemporary physics
• The gravitational wave Universe
• Matter under extreme conditions
• How did the Universe originate and what is it
  made of?
• The early Universe
• The Universe taking shape
• The evolving violent Universe

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• Call for mission proposals expected, to be
  submitted by the end of January
• Selection of 3 small/medium class missions, down
  selection of to single mission 2011, launch 2017
• Selection of 3 large missions for further study,
  down selection to single mission in 2015 (XEUS,
  DARWIN, Jupiter probe, ?) with launch in 2020 or
  later
• Structure of proposals not yet known, emphasis on
  science
• XEUS, a gamma-ray imager (GRI) and NED (TBC) will
  be proposed
• missions such as eRosita and Lobster will be
  implemented outside this call (as will Symbol-X,
  tbc)

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NEW Status

• XEUS/NEW priority for SRON
• Possible significant study funding (1-3 M) but
  nothing for sure
• Possible additional funding for technology (1-2
  M) combined with industrial use of key
  technology
• Funding of major part of detector looks realistic
  
• Funding of a major part of a mission is clearly
  more difficult (astronomy has already more than a
  fair share of the funding in the Netherlands)

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Sterile neutrinos

• Potential dark matter particle (but certainly not
  the only one)
• Three active neutrinos are known ne, nm, nt.
  Oscillations, expressed by mixing angle q,
  explains difference in neutrino state as produced
  in the sun and as detected on earth
• Introduction of right-handed neutrinos with no
  Standard Model interactions (hence sterile) are
  good Dark Matter particles (interaction only
  through gravity)
• Quantum mechanics allows for oscillations between
  active and sterile neutrinos. Through weak
  interaction the neutrino can decay while emitting
  a photon

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ns ? n e,m,t g E g,s ms / 2 Decay rate Gs ?
sin2 2q (ms/keV)5
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• Attractive in various ways
• additional neutrino also needed to explain mass
  differences between active neutrinos (10-5, 10-3
  and 1 eV2)
• Pulsar velocities anisotropic neutrino emission
  from a supernova
• Eliminates problems with CDM and explains small
  cores in dwarf spherodial galaxies
• Explains early star formation and reionization

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• Contours production predictions
• with different lepton numbers
• Current constraints from
• X-ray background
• Coma/Virgo cluster (XMM)
• LMC (diagonal)
• Ly a (SDSS Lya forest,
• high-z Lya, SMMT)
• Overproduced (gray)
• Dwarf galaxy (Fornax)
• Ly a limit gt 10 keV
• Dwarf spheroidal galaxies 1- 5 keV

• not the correct theory
• (Ws lt 0.26)

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Controversial and speculative but interesting

• Where to search (all done but now with increased
  sensitivity)
• XRB
• Clusters
• Dwarf galaxies
• How to search
• Search for line emission correlated with assumed
  dark matter distribution
• Figure of merit AWE/DE E-range
• See Shaposnikov, Viel, Kuchenko for solid
  information. They (Shaposnikov) showed clear
  interest to contribute

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Instrument requirements

• Improve current instruments by one order of
  magnitude (figure of merit AWE/DE)
• XMM-Newton _at_ 0.5 keV 600
• NED _at_0.5 keV 80.000
• Aeff 500 cm2
• E-range 0.5 2.5 but preferably higher
• W 1 degree
• DE 3 eV
• Dq arcmin
• sources 10 (?) survey data

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Science requirements

• See table

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Strawmans observation program (4 year, 60
efficiency)
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Mission profiles
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Payload resources
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Mission trade-off
Requirement model ? Goal model ?
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Mirror XEUS precursor feasibility

• Milli pore optics angular resolution 1 arcmin
  (? 10 introducing Wolter I design)
• Light weight nn kg/m2
• GRASP considerable compared to Rasmussen design
• Optimize focal length some (10 cm2) area at 6
  keV
• Least mature but could be of interest for ESA as
  XEUS precursor (to be mentioned in the proposal ?)

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Instrument trade-off

• TES detector Area ? E-resolution ? angular
  resolution
• CCD detector pixel size ? Field of View
• Burst detector energy range ? weight
• weight ? sky coverage
• Mirror weight ? angular resolution
• focal length ? Energy range