Science results. N. Produit INTEGRAL science results 2 INTEGRAL is on a 3-days orbit with apogee at 150 000 km and perigee at 10 000 km. Maximizes time.

Science results

N. Produit INTEGRAL science results 2

INTEGRAL is on a3-days orbit with apogeeat 150 000 km and perigeeat 10 000 km.

Maximizes time outside the electron belts

N. Produit INTEGRAL science results 3

The instruments

The spectrometer SPI (Ge)- 20 keV -> 8 MeV (1keV)- field of view: 16 degrees- angular resolution: 2 degrees

The optical camera OMC- field of view: 5 degrees- resolution: 17.6 arcsec- up to 19.7 mag

The X-ray imager JEM-X- 3 -> 35 keV- angular resolution: 1 arcmin- FCFOV 4.8(dia) degrees

The imager IBIS (CdTe, CsI)- 15 keV -> 10 MeV (10keV)- resolution: 12 arcmin- FCFOV 9X9 degrees

Technique ofcoded maskfor IBIS, SPIand JEM-X

Exposure Map up to February 2006maximum 107 sec

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Science with INTEGRAL

Emission processes:

● Matter anti-matter annihilation

● Matter matter collision ● Black body radiation (surface of neutron stars)

● Bremsstrahlung (clusters of galaxies also a deep gravitational well)

● Synchrotron radiation (relativistic electrons in B-field)

● Compton processes (electron-photon diffusion) with either thermal electrons or relativistic electrons

● Relativstic jets that boost either process

● Nuclear line emission

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The variable γ ray sky

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“MAGNETAR, B ~ 1015 G Neutron star, Field re-arrangement INTEGRAL SPI/ACS von Kienlin et al.

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micro-quasar GRS 1915+105 D. Hannikainen et al.

New type of variability

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20-60keV variability mapNeronov et al.

Variability ofgalactic centerless than 8%

Extended emission

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Galactic center Revnivtsev et al. 2004, A&A 425, L49)

16-60keV

ISGRI data

Fe contoursASCAoverplot

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● INTEGRAL: PL ~ 1.8, no cut-off << 100 keV:

→ Initial SgrA* spectrum similar to low luminosity AGN’s

6.4 keV line is stable over ~ 10 y

Compton continuum

Fluorescence

cut-off (Comptonrecoil of h.e. γ’s)

Scattered radiation

NH: 8x1022 cm-2, Fe-abundance: 1.9 (x solar) MSgrB2: 2x106 M (r/10 pc)2

Close stellar XRB transients inside cloud (~30 ly across) ruled out. Illuminating source: Sgr A*, ± 1700 A.D. Past luminosity (2-200 keV) ~ 1039 erg/s (104 of today’s value)

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IGR J00291+5934 Shaw, Eckert et al. 2005INTEGRAL ISGRI 20-60keV

Fastest accreting msec pulsar, discovered December 2 2004

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Radio Pulsars

Millisecond Radio Pulsars

Spin u

p by

mass

accre

tion

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GX5-1, Neutron star binary system A. Paizis et al.

Accretion disk and a Compton component, hard tails arenot a signature of the presence of black holes.

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Bright unidentified sources

Many unidentified sources should be HMXBOver-density in the (inner) Norma arm region

High HMXB density

Low HMXB density

Walter et al 2005

Lutovinov et al 2005

New : -0.9HMXB : -0.6HMXB+new: -0.6HMXB (XTE): -0.6±0.1

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Electron-positron annihilation, SPI map

There are 1043 annihilation per second. Spectrum suggests annihilation in warm medium (7000K) Churasov et al. MNRAS 357, 1377, 2005

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Big Bang

Hydrogène + Helium

Fe 60 : ~ 2 000 000 yearsAl 26 : ~ 1 000 000 yearsTi 44 : ~ 90 yearsNa 22 : ~ 4 yearsCo 56, 57 : ~ 100, 400 daysNi 56, 57 : ~ 8, 2 days

Nucleosynthesis

Some of the stellarnucleo synthesis productsare observable

Stars

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Diehl et al.Nature 2006

26Al emissionassociatedwithdisk population

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Quasar 3C 273

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Courvoisier et al.,2003, A&A 411,L343

GRS 1227+025 notobserved

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GAMMA Ray bursts: 1 per month in the IBIS Field of view.

Localisation to 2-4 arcminutes.

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Burst positions are sent automatically to the communityby the IBAS system (Mereghetti et al.,2003, A&A 411, L291Burst light curve and trigger history:

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Earth observation

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As conclusion

INTEGRAL is already in an extended mission phaseA further extension until 2008 has been accepted by ESA

AO4 is open you can submit observation requests!

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