Družice ESA INTEGRAL

IBWS Vlašim 2006

RH & ASU HEA team1. astrophysics ESA satellite with Czech participation

• Gamma-ray observatory with concurrent X-ray and optical monitoring.

• INTEGRAL is the ESA Science Programme’s mission launched on October 17, 2002.

• ESA’s 2nd γ-ray mission (COS-B, 1975), will join XMM-Newton in orbit.

• ESA led mission in collaboration with Russia, United States, Czech Rep. and Poland

• Lifetime of at least 5 years.

• Highly eccentric 72 hour orbit.

• Observing programme includes 65-75% open time.

The INTEGRAL The INTEGRAL MissionMission

Images from the Bajkonur cosmodrome: Integral ready for launch with Proton rocket on Oct 17 at 4.41 UT

Integral launch event: ESA MOC, Darmstadt, October 17 from 3.30 UT

TV also via Astra satellite

The INTEGRAL instruments

SPI – The gamma-ray Spectrometer on INTEGRAL. Excellent spectra, good images

Jem-X - The Joint European X-ray Monitor

IBIS – The gamma-ray Imager onboard the INTEGRAL satellite. Excellent Imaging, good spectra

OMC – Optical Monitor Camera.

Instrument Principal Investigators Collaboration

IBISP. Ubertini (I), F. Lebrun (F), G. Di Cocco (I)

Italy, France, Norway, Germany, Spain, USA, Poland, UK

SPIJ.-P. Roques (F), V. Schönfelder (D)

France, Germany, Italy, Spain, Belgium, UK, USA

JEM-X N. Lund (Dk)Denmark, Finland, Spain, Italy, USA, Sweden, UK, Poland, Russia

OMC M. Mas-Hesse (ES) Spain, Ireland, Belgium, UK, Czech Republic

Science Data Centre

T. Courvoisier (CH)Switzerland, France, Germany, Italy, Denmark, UK, Belgium, USA, Czech Republic, Poland

The complex INTEGRAL instruments were built by large collaborations…

The INTEGRAL Science and Data Centre ISDC

• It is the task of the INTEGRAL Science Data Centre in Versoix, Switzerland to make the data from all the instruments available to the scientific community.

• Not only are the instruments built by large collaborations…

• Czech participation: consortium member, Co-I, direct participation to the team, science

ISDC

ISDC - members of the consortium

Integral multispectral imaging: BH candidate Cyg X-1

ESA INTEGRALESA INTEGRAL

Co-aligned onboard instruments:Co-aligned onboard instruments:gamma-ray imager IBISgamma-ray imager IBIS (15 keV–10 MeV, (15 keV–10 MeV,

field 9 deg, field 9 deg, 12 arc min FWHM)12 arc min FWHM)gamma-ray spectrometer SPIgamma-ray spectrometer SPI (12 keV– (12 keV–

8 MeV8 MeV, field 16 deg, field 16 deg) ) X-ray monitor JEM-XX-ray monitor JEM-X (3–35 keV (3–35 keV, field , field

4.8 deg4.8 deg) ) optical monitoring camera OMCoptical monitoring camera OMC

(Johnson (Johnson VV-filter-filter, field 5 deg, field 5 deg) )

Simultaneous information in the optical, medium Simultaneous information in the optical, medium X-ray, hard X-ray, and gamma spectral region (or X-ray, hard X-ray, and gamma spectral region (or at least a suitable upper limit) for each CV in at least a suitable upper limit) for each CV in each scan or field.each scan or field.  Modes of observation:Modes of observation:(a)(a) Regular (weekly) Galactic Plane Scans (GPS) Regular (weekly) Galactic Plane Scans (GPS) (-14(-14oo<<bbIIII<+14<+14oo))

(b)(b) Pointed observations Pointed observations(c) (c) Targets of opportunityTargets of opportunity

Fields of view of Fields of view of the individual the individual instrumentsinstruments

The IBIS/ISGRI image (top; 18-60 keV) shows the inner 3.5 degree by

2.5 degree region of the center of the Galaxy. Contours represent

signal-to-noise levels starting at S/N = 5 and increasing with a

factor 1.4. The image has a total effective exposure time of 2.3 Ms.

The bottom image is the same INTEGRAL image, however, now with

the brightness distribution of the 6.4 keV iron line as determined by

ASCA/GIS, overplotted as contours.

The First Gamma-ray Burst observed by INTEGRAL

GRB030501 "Labor Day GRB"

1st "Czech" lead analyse GRB observed by INTEGRAL (according to negotiated rotation of responsibilities of instrumental teams)

SPI image

Real-time localization by IBIS and IBAS alert response

Non-magnetic cataclysmic variable (CV)Non-magnetic cataclysmic variable (CV)

Non-mag. white dwarfNon-mag. white dwarf

Donor, lobe-filling starDonor, lobe-filling star

Mass streamMass stream

Bright spot (stream Bright spot (stream impact onto disk)impact onto disk)

Accretion diskAccretion disk

Accretion disk – thermal Accretion disk – thermal radiation (UV, optical, IR)radiation (UV, optical, IR)

Opt. thick, geom. thin boundary Opt. thick, geom. thin boundary layer (therm. rad. - soft X-rays) layer (therm. rad. - soft X-rays) (high (high mm))

Opt. thin, geom. thick boundary Opt. thin, geom. thick boundary layer (bremsstrahlung – hard layer (bremsstrahlung – hard X-rays) (low m)X-rays) (low m)

..

..Dominant source of luminosity: Dominant source of luminosity: accretion processaccretion process

Intermediate polar – Intermediate polar – mildly magnetized mildly magnetized white dwarfwhite dwarf

Impact region near the Impact region near the magnetic pole of the WDmagnetic pole of the WD (bremsstrahlung – hard (bremsstrahlung – hard X-rays)X-rays)

Increasing Increasing time-time-averaged averaged mass mass accretion accretion rate rate mm(also (also increasing increasing time-time-averaged averaged luminosity)luminosity)

..

Thermally Thermally unstable diskunstable disk

ThermallyThermallystable diskstable disk(most time)(most time)

quiescencequiescence

outburstoutburst

Non-magnetic CVsNon-magnetic CVs Radial temperature Radial temperature profile of the diskprofile of the disk

(Wood et (Wood et al. 1986)al. 1986)

(Horne & (Horne & Cook 1985)Cook 1985)

Dwarf nova Z ChaDwarf nova Z Cha

flat temperature profile, diskflat temperature profile, disk cool, optically thincool, optically thin

steep temperature profile,steep temperature profile, disk hot, optically thickdisk hot, optically thick

Magnetic CVsMagnetic CVs (polars)(polars)

cyclotron emission from cyclotron emission from accretion column (mainly accretion column (mainly optical and UV)optical and UV)

bremsstrahlung from bremsstrahlung from shocks above impact shocks above impact region on the WD (X-rays)region on the WD (X-rays)

AM Her AM Her ((kTkTbrembrem~31 keV) ~31 keV)

(Rothschild et (Rothschild et al. 1981)al. 1981)

ST LMi – orbital modulation ST LMi – orbital modulation in hard Xrays (1.9-8.5 keV)in hard Xrays (1.9-8.5 keV)((EXOSATEXOSAT))

AM Her – orbial modulationAM Her – orbial modulationtop – soft X-rays (40-120 A)top – soft X-rays (40-120 A)bottom- hard X-rays bottom- hard X-rays (1.9-8.5 keV) ((1.9-8.5 keV) (EXOSATEXOSAT))

Mason (1985)Mason (1985)

Heise et al. (1985)Heise et al. (1985)

hard X-ray sourceshard X-ray sources

IBISIBIS

Typical high and Typical high and low states found low states found by Meinunger and by Meinunger and Hudec, 1976Hudec, 1976

FField of the intermediate polarield of the intermediate polar V1223 SgrV1223 Sgr. .

Co-addedCo-added frames from frames from IBISIBIS. . Start exp. JD 2452730.17Start exp. JD 2452730.17

Integration time: 66 700Integration time: 66 700 sec sec

SSize of the fieldize of the field:: 9.1 9.1oox7.1x7.1oo. . North is up, East to the left.North is up, East to the left.

15 – 25 keV15 – 25 keV 25 – 40 keV25 – 40 keV

40 – 60 keV40 – 60 keV

V1223 SgrV1223 Sgr

IBIS IBIS (25–40 keV)(25–40 keV) image image of of GK PerGK Per ((Integr. time: 79 980Integr. time: 79 980 sec sec Co-added images: 19 March 2003, 27 – 29 July 2003. Co-added images: 19 March 2003, 27 – 29 July 2003. SSize of fieldize of field:: 4.14.1ooxx3.03.0oo. North is up, East to the left.. North is up, East to the left.

GK PerGK Per INTEGRALINTEGRAL

Quiescent X-ray spectrum Quiescent X-ray spectrum Parameters from Ishida et al. (1992)Parameters from Ishida et al. (1992)((kT kT = 32 keV, = 32 keV, NNH H = 10= 102222 cm cm-2-2, , norm. factor: norm. factor: 0.00390.0039+/-+/-0.00020.0002 photonphoton//cmcm22/s/s11//keVkeV))

IBISIBIS

IInterval between outburstsnterval between outbursts:: t = 973 t = 973 daysdaysIBIS obs.:IBIS obs.: start at ~4 start at ~422 percent of this interval (percent of this interval (measured measured since the previous outburst). since the previous outburst). Ishida’s et al. Ishida’s et al. reference spectrum:reference spectrum: t = 983t = 983 days (start days (start at at ~~2929 percent of this interval). percent of this interval).

AAmount of matter arriving to the WD and the parameters mount of matter arriving to the WD and the parameters of the X-ray emitting region on the WD remained almost of the X-ray emitting region on the WD remained almost the same during these phases of the quiescent intervals.the same during these phases of the quiescent intervals.

FluxFlux ((1515 –– 4040 keVkeV)) = (2.= (2.77 +/- +/- 1.1.2) x 2) x 1010-4-4 photon photon//cmcm22//s s LL (15 – 40 keV) = 4.6 x 10 (15 – 40 keV) = 4.6 x 103232 erg/s erg/s

First OMC image from space

OMC Pointing Software OMC PSdeveloped by V. Hudcova at AI Ondrejov

Part of ISOC - Integral Science Operation Centre

Generates telecommands sent to the satellite

Controlls the OMC

Selects objects observed

Transfer of up to 100 objects

Selection of objects in photometric shot

Fotometrický snímek (střed 10.12, 45.12, otočení 10.0)

42.0

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Rektascenze

Deklinace

Gnomonická projekce

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Gnomonická projekce - otočení

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Magnitudy vybraných objektů

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First OMC image from space .... after running the OMC Pointing Software developed by Věra Hudcová with help of Filip Hroch and Jiří

Polcar at HEA Group, Astronomical Institute Ondřejov

Blazars & their powerful jets

Line of sight• Effects of the jet:• Relativistic beaming• Superluminal motion• Featureless continuum• Gamma rays• Rapid variability• High luminosityBlazar observer

Supermassive black holewith accretion disc

Jet (within ~10% AGN). Beam of energetic

particles and magnetic field moving close to the

speed of light

Violent optical variability of BL Lac on a long time time scale

good candidate to be detected at flaring

BL Lac

Historical optical light curve of NRAO530

The source exhibits rare but large amplitude optical flares (Dm~ 4 mag)

Optical R band good tracer for the HE activity of blazars (CGRO experience, Collmar (2004)) - gamma flares can be expected

INTEGRAL ToO Observation

The target and the three additional AGNs in the IBIS FOV (30-

60 keV)

S5 0836+710 Markarian 6

single power law spectrum G~1.5single power law spectrum G~1.3

Hints for a break or cutoff in Markarian 3

IBIS/ISGRI spectrum

Broken power law

Power law with high energy cutoff

INTEGRAL AO-3 ToO observation of 3C454 (z=0.859), preliminary results, L. Foschini et

al. ATEL 2005, PI E. Pian @ large collaboration

ToO triggered by high optical (T. Balonek, VSNET alert) and X-ray (BAT Swift) activity

INTEGRAL observation started May 15, at 18:40 UT, exposure 200 ksec

source clearly detected by IBIS/ISGRI in the 20-40 and 40-100 keV energy bands, with a significance of 20 and 15 sigma

Optical light curve of 3C454.3 (T. Balonek)

Integral observation

INTEGRAL

INTEGRAL IBIS/ISGRI images, 20-40 (left) and 100-200 keV (right)

Secondary INTEGRAL Science and Data Centre, Ondřejov, Czech Republic

•OSA installed and operated, public databases, ...

•assistence can be provided to guest astronomers from Central Europe

•intensive collaboration with ISDC in Versoix

Our students at the 1st INTEGRAL Progress Meeting, Senohraby, October 2002

Hudec, Hrudková, Šmída, Hroch, Polcar, Bašta, Topinka, Jelínek, Štrobl, Stoklasová, Nekola, Kubánek

2nd INTEGRAL&BART Progress Meeting, Kostelní Střímelice, Oct 2003

3rd INTEGRAL/BART Workshop, Chocerady, Nov 1-3, 2004

INTEGRAL Day 2003, Prague, Academy of Sciences of the Czech Republic, May 27

Prof. A. Parmar, ESA: "The contributions from scientists in the Czech Republic to the OMC and ISDC consortia has been very successful and is much appreciated by ESA. We look forward to similar co-operation on XEUS and other missions!"

INTEGRAL future:•lifetime ~ 15 years, smooth operation

•Czech Participation: Decision of ESA PECS Program Committee: prolongation approved for 4 years starting January 2005

•Continued ISDC participation, ISDC2 operations, OMC data analyses, science

•Participation of young Czechs very much appreciated by ESA

Acknowledgements:Acknowledgements:

This study was supported by the projectThis study was supported by the projectss ESA ESA PRODEXPRODEX INTEGRALINTEGRAL 1452714527, ESA , ESA PECS INTEGRAL andPECS INTEGRAL and

partly by the grant 205/05/2167 of the Grant Agency of the Czech Republicpartly by the grant 205/05/2167 of the Grant Agency of the Czech Republic. . WeWehave made use of the visual observations from the AFOEV database operated inhave made use of the visual observations from the AFOEV database operated inStrasbourg, France. We acknowledge using the curve-fitting code HEC13 writtenStrasbourg, France. We acknowledge using the curve-fitting code HEC13 writtenby Dr. Harmanec. We thank F. Hroch for the preparation of a mosaic of V2400 Ophby Dr. Harmanec. We thank F. Hroch for the preparation of a mosaic of V2400 Ophand P. Sobotka for a search in the OMC database. and P. Sobotka for a search in the OMC database. The WWZ code by G. Foster isThe WWZ code by G. Foster isavailable at URL: www.aavso.org/data/software/wwz.shtml. The code AVE for the available at URL: www.aavso.org/data/software/wwz.shtml. The code AVE for the period search, developed by the GEA society, is available at URL:period search, developed by the GEA society, is available at URL:www.astrogea.org/soft/ave/aveint.htm.www.astrogea.org/soft/ave/aveint.htm.