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First Results of INTEGRAL
INTEGRAL was launched on October 17 2002
by a Proton Rocket from Baikonour
INTEGRAL had been
proposed in 1989,
accepted in 1993 by
ESA
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First results of INTEGRAL
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T. Courvoisier
First results of INTEGRAL
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INTEGRAL is an ESA
mission with Russian
launcher
and one US ground
station (part time)
Instruments provided through
national funding.
Bus is identical to XMM-Newton
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INTEGRAL is on a
3-days orbit with apogee
at 150 000 km and perigee
at 10 000 km.
Maximises time outside the
electron belts
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High energy instruments are based on coded mask optics:
Coded mask principle
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IBIS tungsten mask in construction
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ISGRI shadowgrammes for single pointings
Crab shadowgramme
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3C 273 shadowgramme
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SPI: spectrometer resolution 500
angular resolution 2.7 degrees
continuum sensitivity: 1.2E-6 ph/cm2skeV
19 cooled Germanium detectors
Pis: J.-P Roques (CESR), V. Schoenfelder (MPE).
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Vedrenne et al. A+A in Press
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IBIS: Imager resolution 12'
sensitivity: 6E-7ph/scm2keV at 100keV (ISGRI)
2 detector planes: ISGRI, 16384 CdTe detectors
PICSIT, 4096 CsI detectors
Pis: P. Ubertini (IAS), F. Lebrun (CEA).
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Ubertini et al. A+A in press
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JEM-X extends the energy coverage down to 5 keV
PI: N.Lund (DSRI), Lund et al. A+A in press
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OMC provides optical (V) coverage of sources in the FOV
PI: M. Mas-Hesse (LAEFF),
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Mas-Hesse et al. A+A in press
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Main instrument characteristics
E-range
E-resolution FOV(deg) ang.Res.
SPI
20keV-8MeV
IBIS
15keV-10MeV
JEM-X 5KeV-30keV
OMC
V
500
9
10
---
16
9
4.8
5
2.5 deg
12'
3'
17''
FOV: Fully coded area diameter or side of square
ang.Res of OMC is the pixel size
Point source location considerably better than the angular resolution
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INTEGRAL sensitivity compared with previous instruments
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First results of INTEGRAL
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INTEGRAL sensitivity compared with previous instruments
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The INTEGRAL Science Data Centre (ISDC)
Courvoisier et al. A+A in press
Link between the data and the community
All data (120 kbits/s) are processed at the ISDC:
-in real time (few seconds after receipt on the ground) to detect gamma ray bursts
and inform the community (IBAS, Merehetti et al. A+A in press)
-in near real time (within few hours) to detect new or very variable sources
-offline to produce a set of standard products
The data are archived and distributed (at present 1.5-2 months after the observation)
to the observers
Analysis tools are provided to the community
http://isdc.unige.ch gives access to the ISDC services
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The INTEGRAL Science Data Centre
Consortium institutes, there is
close collaboration with inst. teams
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ISDC hosted by Geneva Observatory, 35 staff work
in Versoix near geneva
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All data are transferred to ISDC and
are analysed there.
European Space
Operations Center
Darmstadt
ISDC
Observation programme: 30% core programme
AO-1
70% open programme
AO-1 in progress, AO-2 starts January 1, 2004
Exposure map (ISGRI fully coded FOV) revolutions 1-100
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Core programme: Galactic plane scans, every 12 days
Structure of the scans
Distribution of scans in the plane
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Core programme: Galactic center deep exposure (Ao-2)
This is intended to:
-monitor and detect compact sources
-to map electron-positron annihilation map
-to map Aluminium emission
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INTEGRAL Status:
The instruments function very well
The observation programme is progressing as expected.
The observation efficiency is short of few percent of the optimum
The data reach the ISDC in a matter of seconds for near real
time analysis
The data reach the observers in about 6 weeks -2months.
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Cygnus X-1 early images
ISGRI 15-40 keV
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SPI
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Cygnus X-1 Observations in PV phase
(Pottschmidt et al. A+A in press):
RXTE and INTEGRAL data obtained simultaneously
revolutions 11,14,16,18,25 (November 16-December 29)
Cygnus X-1 switched from soft to hard state mid October 2002
RXTE-PCA
IBIS/ISGRI
RXTE-HEXTE
JEM-X
SPI
Counts spectra.
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Model Fit: Disk+Comptonised component+reflection hump
Parameters: KTe = 62keV, τ = 1, reflection: 0.2 similar for all revolutions,
in agreement with previous descriptions.
Instruments agree very well apart from the normalisations.
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IGR J16318-4848
Discovered January 29 2003 in scan of the Galaxy.
Observed in subsequent pointed observation and by XMM-Newton
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IGR J16318-4848: strongly absorbed (NH = 2 1024 cm-2)
strong Fe line at 6.4 keV (EW of 2.1 keV), variable
Preferred interpretation:
1036 ergs/s high mass
X-ray binary at distance
of centre of the Galaxy.
Possible strong contribution
to the X-ray background.
Walter et al. A+A in press
Matt+Guainazzi, 2003
Revnivtsev et al. AL in press
XMM-Newton
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INTEGRAL
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There are 11 published bright sources discovered by
INTEGRAL in the first half of galactic centre observations
of the core programme.
Some are transients, some present but very weak in earlier data
variable, often absorbed.
Many more to
come
courtesy Walter, ISDC
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Low Mass X-ray Binaries during core programme
(Paizis et al. A+A in press)
ISGRI
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20-40
40-60
First results of INTEGRAL
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GX17+2, comptonised black body, evidence for
additional flux at 100 keV?
JEM-X and ISGRI: 1pointing
SPI: combined data.
Seen in black hole candidates
(Gerlinski et al. 1999), but
GX17+2 is a bursting source.
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Le micro-quasar GRS 1915+105
D. Hannikainen et al.
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Core Programme composite map (revolutions 40-67), max exp:790ks
1216 pointings, ISGRI 15-40 keV, Courtesy R. Walter, ISDC
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Central regions:
0
10 degrees
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0
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regions: de notre galaxie:
LeCentral
centre
Sgr A*
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3C 273: bright quasar, monitored by INTEGRAL Courvoisier et al. In press
20-40 keV significance map, insert: flux image GRS 1227+025 (Jourdain et al. 1992)
not seen at less than ½ 3C 273.
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3C 273 INTEGRAL,
XMM-Newton, RXTE
January 03
ratio of normalisations to
XMM PN camera:
RXTE-PCA: 1.34+-.02
RXTE-HEXTE: 1.05+-.06
JEM-X:
0.61+-.05
ISGRI:
1.76+-.2
SPI:
0.95 +-.3
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Using the cross calibration:
continuum single power law
Gamma = 1.74+-0.015,
Norm. at 1keV: 2.24+-0.05 10-2
ph/cm2skeV
Weaker and steeper than previously
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Big Bang
Genèse
des
éléments
Hydrogène + Helium
Tous les autres éléments
fabriqués dans les étoiles,
dont certains sont radioactifs
Étoiles
Fer 60
Aluminium 26
Titane 44
Sodium 22
Cobalt 56, 57
Nickel 56, 57
:
:
:
~ 2 000
~ 1 000 000 ans
:
~ 90 ans
:
~ 4 ans
~ 100, 400 jours
:
~ 8, 2 jours
GAMMA Ray bursts: 6 in the IBIS Field of view.
Localisation to 2-4 arcminutes.
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Burst positions are sent automatically to the community
by the IBAS system (Mereghetti et al. A+A in press)
Best performance to date:
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Conclusion
INTEGRAL is up and well, data are flowing,
the programme evolves as expected.
Special issue of A+A letters in preparation
AO-2 deadline is September 5......
Mission extension beyond end 2004 will
be discussed by ESA-SPC in November
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