M. Dadina: XMM-Newton

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XMM-Newton, Chandra Suzaku
M. Dadina XMM-Newton Chandra
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Date December 1970 to March 1973
Vehicle/Mission Uhuru X-ray satellite
Agency/Country NASA Instruments/Detectors
Proportional counters (2 -20 keV) Mirror
Description No mirrors Highlights Uhuru, the
first satellite dedicated to the observation of
cosmic X-ray sources, was equipped with a
sensitive proportional counter attached to a
viewing pipe to locate the sources. It expanded
the number of known sources to more than 400,
showed that X-ray stars are neutron stars or
black holes accreting matter from companions in
binary star systems, and discovered X-rays from
hot gas in galaxy clusters.
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November 1978 to April 1981 Vehicle/Mission
Einstein X-ray Observatory Agency/Country NASA
Instruments/Detectors Proportional
counters/microchannel plate imager/solid state
spectrometer/crystal spectrometer (0.2 -4 keV)
Mirror Description 4 nested mirror pairs with
an area of 350 sq cm and a resolution of 3-5 arc
sec. Highlights The first large X-ray telescope
with mirrors. Einstein made the first X-ray
images of shock waves in supernova remnants, hot
gas in galaxies and clusters of galaxies.
Einstein also located accurately over 7000 X-ray
sources, including stellar coronas, X-ray
binaries, galaxies and quasars. It made possible
a new way to study the mysterious dark matter
that is present in galaxies and clusters of
galaxies and showed that most of the X-ray
background is probably due to discrete sources.
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Date May 1983 to April 1986 Vehicle/Mission
EXOSAT Agency/Country European Space Agency
Instruments/Detectors Proportional counters
(0.1 -10 keV) Mirror Description 2 nested
mirror pairs with 80 sq cm area and 18 arc sec
resolution Highlights Discovery of
quasi-periodic oscillations from neutron stars
and black holes, surveys of variability of wide
variety of galactic and extragalactic sources.
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ROSAT Date June 1990 to February 1999
Vehicle/Mission Roentgensatellite (ROSAT)
Agency/Country Germany Instruments/Detectors
Proportional counters/microchannel plate imager
(0.1 -2.5 keV) Mirror Description 4 nested
mirror pairs with 1140 sq cm area and 3 arc sec
resolution Highlights ROSAT expanded the number
of known X-ray sources to 125,000 and proved to
be especially valuable for investigating the
multi-million degree gas present in the upper
atmospheres of many stars, made the first
detection of radiation from the hot surface of a
neutron star, and comets. It resolved 70 of soft
X-ray background, and made an extensive catalogue
of galaxy clusters
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Date 1993 to July 2000 Vehicle/Mission
Advanced Satellite for Cosmology and Astrophysics
(ASCA) Agency/Country Japan Instruments/Detecto
rs Proportional counters/CCDs (0.4 -12 keV)
Mirror Description 120 nested foil mirrors with
1300 sq cm area and resolution of 180 arc sec
Highlights The ASCA X-ray observatory with low
resolution mirrors, and the first large CCD
detectors, was especially designed to study the
detailed spectra of X-ray sources in supernova
remnants, active galactic nuclei and galaxy
clusters. Found first evidence of the
gravitational redshift due to the strong
gravitational field around a black hole.
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Come funziona un CCD?
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A photoelectric interaction of an X-ray with
silicon atoms in a CCD will generate
electron-hole pairs. On average, the number of
electrons Ne liberated by the interaction is
proportional to the energy of the incident
X-ray Ne E/w, where Ne is the number of
electron liberated, E is the photon energy and w
3.7eV/e- (at T 153 K) is the mean ionization
energy per electron-hole pair and is a function
of the temperature of the silicon. The variance
of the charge liberated is
where F, is the Fano factor and has the value F
0.135. The effect of the statistical nature of
the ionization process, the loss of charge during
collection (?R), the noise in detector, pre-amp,
main amplifier, and signal processing electronics
(?A) , is that the primary peak produced in
response to a beam of monochromatic incident
photons of energy E will be approximately a
Gaussian distribution with mean proportional to E
and a full width at half maximum of
The strong electric field in the CCDs depletion
region separates the electrons and holes before
they recombine. The spectral resolution of the
CCD is mainly determined by the stochastic nature
of the ionization process (Fano Noise), the
charge transfer properties of the CCD and the
electronic noise of the readout amplifier.
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Date December 1995 to present Vehicle/Mission
Rossi X-ray Timing Explorer (RXTE)
Agency/Country NASA Instruments/Detectors
Proportional counters (2 -50 keV) and
scintillation counters (15 -200 keV) Mirror
Description No mirrors Highlights Although
RXTE does not have focusing X-ray mirrors, it has
the unique capability to study rapid time
variability in the emission of cosmic X-ray
sources over a wide band of X-ray energies, and
has made valuable contributions to our
understanding of the behavior of matter in the
vicinity of neutron stars and black holes.
Extremely rapid variability observed by RXTE may
be evidence for the dragging of space by strong
gravity in the vicinity of black holes.
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Date April 1996 to April 2002 Vehicle/Mission
BeppoSAX Agency/Country Italy The Netherlands
Instruments/Detectors Proportional counters
(0.1 -10 keV), scintillation counters (3 -120
keV) and phoswich detectors (15 -300 keV) Mirror
Description No mirrors Highlights BeppoSAX is
the first X-ray mission with a scientific payload
covering more than three decades of energy - from
0.1 to 300 keV, with moderate imaging capability.
BeppoSAX has proved to be especially useful for
wide band spectra of active galactic nuclei, and
for studying gamma-ray bursts by determining
their positions with an unprecedented precision
and monitoring their X-ray afterglow.
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Ricapitolando....
nel 1962 nascelastronomia in banda X. Da allora,
ad ogni missione si sono scoperte cose nuove ed
ogni satellite/telescopio che e stato messo in
orbita aveva strumenti con capacita
nuove.... si e sempre cercato di migliorare
sensibilta
Risoluzione angolare
Copertura spettrale
COSA MANCA?
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High Resolution Mirror Assembly ( HRMA)?
Ottica Wolter Type-I Mirror diameters 1.23,
0.99, 0.87 0.65 m Mirror lenghts 84 cm HRMA
mass 1500 kg Focal lenght 10.07 m PSF FWHM
0.5
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HRMA (2) effective area
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HRMA (3) on-axis PSF
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HRMA (4) off-axis PSF
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Chandra
Focal plane detectors the ACIS CCDs
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Chandra
ACIS (2) quantum efficency, effective area,
vignettin and E res.
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Chandra The focal plane detectors the
pectrometers
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Chandra The spectrometers the effective area
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XMM-Newton... ovvero.. perchè puntare sulla
grande area di raccolta...
Aumenta le capacità di deconvoluzione spettrale
Timing
Maggiore sensibilità alle strutture di missione
estese
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Tutti gli strumenti sempre in azione....
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epn
emos
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PSF
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PSF (2)?
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Effective Area (solo specchi)?
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CCD QE
PN
MOS
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EPIC Response
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RGS
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Suzaku......
ASCA
Suzaku
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come funziona Suzaku.....
IASF-Bo, 5-9 Giugno 2006
M. Dadina XMM-Newton Chandra
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XRS
XRS
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CCDs....
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The End