T. Courvoisier

T. Courvoisier First results of INTEGRAL 1

First Results of INTEGRAL

INTEGRAL was launched on October 17 2002 by a Proton Rocket from Baikonour

INTEGRAL had beenproposed in 1989,accepted in 1993 byESA



INTEGRAL is an ESA mission with Russian launcherand one US ground station (part time)

Instruments provided throughnational funding.

Bus is identical to XMM-Newton


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

Maximises time outside the electron belts


High energy instruments are based on coded mask optics:

IBIS tungsten mask in constructionCoded mask principle


3C 273 shadowgrammeCrab shadowgramme

ISGRI shadowgrammes for single pointings


SPI: spectrometer resolution 500angular resolution 2.7 degreescontinuum sensitivity: 1.2E-6 ph/cm2skeV

19 cooled Germanium detectors

Pis: J.-P Roques (CESR), V. Schoenfelder (MPE). Vedrenne et al. A+A in Press


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). Ubertini et al. A+A in press


JEM-X extends the energy coverage down to 5 keVPI: N.Lund (DSRI), Lund et al. A+A in press


OMC provides optical (V) coverage of sources in the FOVPI: M. Mas-Hesse (LAEFF), Mas-Hesse et al. A+A in press


Main instrument characteristics

E-range E-resolution FOV(deg) ang.Res.

SPI 20keV-8MeV 500 16 2.5 degIBIS 15keV-10MeV 9 9 12'JEM-X 5KeV-30keV 10 4.8 3'OMC V --- 5 17''

FOV: Fully coded area diameter or side of squareang.Res of OMC is the pixel sizePoint source location considerably better than the angular resolution


INTEGRAL sensitivity compared with previous instruments


INTEGRAL sensitivity compared with previous instruments


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


The INTEGRAL Science Data Centre

Consortium institutes, there isclose collaboration with inst. teams

ISDC hosted by Geneva Observatory, 35 staff workin Versoix near geneva

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


Structure of the scans

Distribution of scans in the plane

Core programme: Galactic plane scans, every 12 days


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


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 realtime analysis

The data reach the observers in about 6 weeks -2months.


Cygnus X-1 early images

ISGRI 15-40 keV SPI


Cygnus X-1 Observations in PV phase (Pottschmidt et al. A+A in press):

RXTE and INTEGRAL data obtained simultaneouslyrevolutions 11,14,16,18,25 (November 16-December 29)

Cygnus X-1 switched from soft to hard state mid October 2002

Counts spectra.

RXTE-PCA

IBIS/ISGRI

RXTE-HEXTE

SPI

JEM-X


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.


IGR J16318-4848Discovered January 29 2003 in scan of the Galaxy. Observed in subsequent pointed observation and by XMM-Newton


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 distanceof centre of the Galaxy.

Possible strong contributionto the X-ray background.

Walter et al. A+A in pressMatt+Guainazzi, 2003Revnivtsev et al. AL in press

XMM-Newton INTEGRAL


There are 11 published bright sources discovered byINTEGRAL in the first half of galactic centre observationsof the core programme.

Some are transients, some present but very weak in earlier datavariable, often absorbed.

Many more to come

courtesy Walter, ISDC


Low Mass X-ray Binaries during core programme(Paizis et al. A+A in press)

ISGRI 20-40 40-60 keV


GX17+2, comptonised black body, evidence foradditional 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.


Le micro-quasar GRS 1915+105

D. Hannikainen et al.


Core Programme composite map (revolutions 40-67), max exp:790ks

1216 pointings, ISGRI 15-40 keV, Courtesy R. Walter, ISDC


Central regions:

0

0

10 degrees


Central regions:Le centre de notre galaxie: Sgr A*


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.


3C 273 INTEGRAL,XMM-Newton, RXTEJanuary 03

ratio of normalisations toXMM PN camera:

RXTE-PCA: 1.34+-.02RXTE-HEXTE: 1.05+-.06JEM-X: 0.61+-.05ISGRI: 1.76+-.2SPI: 0.95 +-.3


Using the cross calibration:continuum single power lawGamma = 1.74+-0.015,Norm. at 1keV: 2.24+-0.05 10-2

ph/cm2skeV

Weaker and steeper than previously

Big Bang

Hydrogène + Helium

Fer 60 : ~ 2 000 000 ansAluminium 26 : ~ 1 000 000 ansTitane 44 : ~ 90 ansSodium 22 : ~ 4 ansCobalt 56, 57 : ~ 100, 400 joursNickel 56, 57 : ~ 8, 2 jours

Genèsedes

éléments

Tous les autres élémentsfabriqués dans les étoiles,dont certains sont radioactifs

Étoiles


GAMMA Ray bursts: 6 in the IBIS Field of view.

Localisation to 2-4 arcminutes.


Burst positions are sent automatically to the communityby the IBAS system (Mereghetti et al. A+A in press)Best performance to date:



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 willbe discussed by ESA-SPC in November

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T. Courvoisier