ANTARES SEMINAR J'Huovelin 31102002

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ANTARES SEMINAR J.Huovelin 31/10/2002
HESA
The X-ray Solar Monitor for SMART-1 and
Instrument Development for XEUS
Juhani Huovelin Observatory, University of
Helsinki
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ANTARES SEMINAR J.Huovelin 31/10/2002
HESA
SMART-1 Mission

• FIRST EUROPEAN MISSION TO THE MOON
• Launch scheduled for 24 March, 2003
• Launch site Kourou, French Guyana
• Integration of science and technology payload
  completed in October 2002 (_at_ ESTEC)
• Payload and satellite under final testing
• Finnish instruments on SMART-1 XSM (UH/HESA) and
  SPEDE (FMI)

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ANTARES SEMINAR J.Huovelin 31/10/2002
HESA
X-ray Solar Monitor (XSM)
Design and manufacturing Metorex International
Oy Performance requirements, scientific use and
calibrations UNIVERSITY OF HELSINKI Department
of Astronomy and Division of X-ray
Physics/Dept. of Physical Sciences
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ANTARES SEMINAR J.Huovelin 31/10/2002
HESA
X-ray Solar Monitor (XSM)
Detector - HPSi PIN, diameter 2 mm - X-ray
photon counter Performance - Energy range
1-20 keV - Energy resolution 250 eV _at_ 6
keV - Sensitivity 7000 cps _at_ X1
flare 1-2 cps _at_
cycle min - Background lt 0.5 cps -
Spectrum distortion 1 pile-up/20kcps -
Circular FOV, 52o radius Data Counts sampled to
energy spectra - 1 spectrum/16 s (512 energy
channels, 0-20 keV)
Sensor unit - Dimensions 81 x 40 x 26 mm3 -
Mass approx. 200 g - Box material Aluminium -
Contents Detector Cooler
(Peltier) Front end
electronics Shutter mechanism
Calibration source (Fe55Ti)

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Task for XSM
ANTARES SEMINAR J.Huovelin 31/10/2002
HESA

• Monitoring of solar X-ray spectra for about one
  year of effective time during 2 years (gt 50
  efficiency), starting 80 days from launch
• Use of data
• Calibration spectra for Lunar fluorescence
  measurements by D-CIXS X-ray imager
• Independent studies of the solar X-ray corona

I
E
XSM observes the Sun as a star
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XSM science performance
ANTARES SEMINAR J.Huovelin 31/10/2002
HESA

• Energy range of XSM is sensitive to solar flares
• 97 of XSM spectrum counts (1-20 keV) are from
  the flare at the maximum of an X1 event
• XSM can handle big flares
• clean spectra _at_ X3 flare (gt20000cps)
• XSM is sensitive enough to measure X-rays at
  cycle minimum
• 20000 cts/3 hours _at_ solar min.

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Use of XSM data
ANTARES SEMINAR J.Huovelin 31/10/2002
HESA

• Combine XSM data with imaging coronal data of
  other satellites (SOHO, RHESSI, TRACE, ...) and
  ground based solar telescopes (morphology of
  distinctive flares)
• Study the evolution of individual flares with
  high time resolution (X-ray heating mechanism)
• Long term evolution of the solar corona (does
  X-ray heating use more than one mechanism during
  solar cycle?)
• Compare with X-ray observatory data of distant
  objects
• (Use of the Sun as a standard candle also in
  X-rays possible since XSM observes the full
  X-ray sun)

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Results
ANTARES SEMINAR J.Huovelin 31/10/2002
HESA

• Hardware project
• XSM detector Flight Model delivered successfully
  to ESA, and is currently integrated at SMART-1.
• Final testing at ESTEC going on.
• Waiting for launch on 24 March 2003.
• Science planning
• Detector response matrix, based on ground
  calibrations at UH Dept. of Physical Sciences, is
  being constructed
• Raw instrument data will be converted to FITS
  format with software developed at UH Observatory
  ? reduction and analysis can be made with
  standard SW packages (FTOOLS XSPEC)
• Huge amount of Solar coronal X-ray data expected
  (D-CIXS data)
• - a little manpower and some collaboration
  currently available, but more of both would be
  welcome for the science work during 2003-2005 (we
  will also participate in D-CIXS cruise and lunar
  science)

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XEUS
ANTARES SEMINAR J.Huovelin 31/10/2002
HESA

• XEUS (X-ray Evolving Universe Spectroscopy
  Mission)
• Potential follow on to ESAs cornerstone X-ray
  spectroscopy mission (XMM-Newton).
• Schedule for mission start 2010-20
• XEUS will be a long-term X-ray observatory
  providing a telescope aperture equivalent to the
  largest ground-based telescopes.
• Mission lifetime 20-30 years, with regular
  upgrades of detectors (5 year cycle planned)
• XEUS is not yet in ESAs mission schedule

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Plan for XEUS instruments
ANTARES SEMINAR J.Huovelin 31/10/2002
HESA

• 2 Narrow field imaging spectrometers ( NFI,
  cryogenic TES
• and STJ arrays)
• A wide field imager (WFI, a CCD ?)
• Under discussion hard X-ray instrument (TlBr
  array ? )

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XEUS activities in Finland
ANTARES SEMINAR J.Huovelin 31/10/2002
HESA

• Development of technology for XEUS instruments,
  and
• planning of science output from XEUS mission
• - VTT Development of SQUID readout electronics
  for a cryogenic TES sensor array
• University of Jyväskylä Development of cryogenic
  TES sensors, CB-thermometers, and SINIS coolers
• University of Joensuu Development of diffractive
  IR-filters
• Chemistry Dept./UH Development of TlBr material
  for use in hard X-ray detectors in astronomy
• Metorex International Collaborative development
  work with VTT, Jyväskylä, Joensuu and Chemistry
  Dept./UH
• Patria Finavitec Development of Detector Control
  Electronics
• Dept. of Astronomy/UH (HESA) XEUS/ANTARES
  coordination, XEUS science planning with
  international XEUS team

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ANTARES/XEUS project
ANTARES SEMINAR J.Huovelin 31/10/2002
HESA

• Role of ANTARES/HESA
• - Bring together institutes and companies in
  Finland, which have activities and plans for
  XEUS instrument development
• Support further activities toward competitive
  technology for XEUS instruments in Finland
• Acquire influence for Finnish astronomers in XEUS
  science plans
• Our status
• - HESA/ANTARES provides only a fraction of
  funding resources for XEUS instrument development
  in Finland. Main part is from the ESA and
  participating institutes and universities
  themselves.

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Recent progress
ANTARES SEMINAR J.Huovelin 31/10/2002
HESA

• Mainly technological
• Reference XEUS model payload specifications and
  science requirements
• Main areas (some of these explained in posters at
  COSPAR)
• improving spectral resolution of a TES, and
  understanding excess noise sources of a cryogenic
  superconducting calorimeter
• improving performance of SQUID readout (noise and
  speed), and finding the best alternative for a
  SQUID array design (first in the world who fully
  understand which and why. Ask VTT for dets)
• improving quality of TlBr crystal by new growth
  equipment and method (goal is a large enough bulk
  of homogeneous and pure crystal for a hard X-ray
  detector)
• improving optical/thermal quality of diffractive
  IR-filters for XEUS.
• participation in XEUS science meeting at MPE
  Garching (2 posters, April 2002)

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Upcoming challenges
ANTARES SEMINAR J.Huovelin 31/10/2002
HESA

• Only partially achievable during ANTARES
• Spectral resolution of TES needs to be improved
  more, which comes hand in hand with breakthrough
  expected in understanding the mechanism and
  physics of excess noise for cryogenic
  calorimeters (first in the world).
• A TES-based detector array (32x32) needs to be
  designed
• A SQUID array needs to be designed. Stepwise
  process first a 4x2 and finally a 32x32 array.
• Required TlBr crystal quality needs to be
  achieved and a detector designed based on the new
  material
• XEUS specifications needs to be met with our
  IR-filters (first optical/thermal and then
  mechanical requirements)
• Design of Detector Control electronics (will
  begin in 2003)
• our role in the international XEUS science team
  has to be signified