X-ray and gamma ray observations · Accretion disk and a Compton component, ... à avril 2006 (février-avril et ... T. Courvoisier March 2007 X-ray and gamma ray observations 30

T. Courvoisier X-ray and gamma ray observations 1March 2007

X-ray and gamma ray observations

From a fraction of a keV(~ 10 Angstroem,few x 1016 Hz)

to TeVs, i.e. >6 ordersof magnitude

Science that started whenrockets reached space

Most discoveriesunexpected


Below a fraction of a keVinterstellar medium is opaque

abs ~e-σNH

similar transmission at1keV and in the IR domain

Few attemps at measurementsin the 100s Angstroem region(FUSE, EUVITA). 1Ry


X-ray Optics:

Grazing incidencefocusing optics

XMM angular resolution: 10”(conical approximation)

Chandra: 1”

Wolter optics:


XMM:56nestedshells(Ni)


XMM ReflectionGrating SpectrometerResolution 200-8005-35 Angstroem


XMM ESA corner stonelaunched in December1999


Line and continuumcontributions to thermal emission.

X-ray spectroscopyvery importantdiagnostics


Clusters of galaxies

Optical image dominated by galaxies (thausends), X-ray image by hot gasXMM, Briel et al.Kitt Peak


A2052, X-ray spectrum, Kaastra et al.

Gas has been processed in stellarinteriors

Perseus, Boehringer et al.Mass dominated by dark matter


Above ~10keV: no optics (presently)---> Coded masks

INTEGRAL IBIS mask


Coded masks:

-multiple pin holes cameras

-mask pattern such that its autocorelation is a delta function

- sky image is reconstructed through deconvolution depends strongly on the flatness of -sensitivity -background

-signal proportional to area, spread over the whole detector (no focusing)-background proportional to area, therefore noise to size-therefore signal to noise proportional to size.


MeV region: difficult not only in theoptical aspects, but also in the detection:

E, MeV

SPI: spectromètre à haute résolution (500)19 detecteurs en Germanium refroidis à 90 K“annealing” : 100 C

Pis: J.-P Roques (CESR), V. Schoenfelder (MPE). Vedrenne et al. A+A, 2003, vol 411

T. Courvoisier INTEGRAL 13

Pis: P. Ubertini (IAS), F. Lebrun (CEA). Ubertini et al. A+A, 2003, vol. 411

ISGRI: Imageur2 plans de détection: ISGRI, 16384 CdTe detectors PICSIT, 4096 CsI detectors


3C 273: source faibleCrabe: source brillante

Shadowgrammes d'ISGRI


Toutes les données transitent à l'ISDC et y sont analysées

Centre opérationsde l'ESA

ISDC

T. Courvoisier INTEGRAL4 16

T. Courvoisier First results of INTEGRAL 17

IGR J16318-4848Découverte le 29 janvier 2003 lors d'une observation de routine. Première d'une série d'objets engoncés dans un cocon de matière

2°

L es so u r c es o b sc u r es

I G R J1 631 8-4848


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.

T. Courvoisier First results of INTEGRAL 2020March 2005

V 0332+53 in outburst, December 04.Cyclotron lines at 25, 55 and 75 keV Kreykenbaum et al 05

Jem-XISGRISPIonINTEGRAL


Centre de la Galaxie

tous les 3 jours de février 2005à avril 2006

(février-avril et août-octobre)

Image moyenne

Question: d'où viennent les anti-électrons ?

N. Mowlavi INTEGRAL 22

INTEGRAL J. Knödlseder et al.

Électron + anti-électron --> annihilation e- + e+ −−> 2 photons à 511 keV

Anti – électrons


Polar is an instrument to measure the polarisation of gamma ray bursts to understand their physics

“light” project (25 kg, small ressources...) in a prototype stage. Collaboration GE-PSI.


POLAR Compton “optics”


Electron-positron optics

above some 10 MeV up to 100 GeV (but flux becomes very small)create pairs from the gamma ray (> 2mec2) and measure the tracesand energies of the electron and positron

EGRET on CGRO GLAST, to be launched in 2007


Quasar 3C 273: archetype of quasars, z=0.158, L~1048ergs/s

Turler et al. Chernyakova et al.


Above 30-100 GeV: Cerenkov Telescope arrays use the atmosphere as detector and measure the Cerenkov light of particle showers generated by the interaction of gamma rays (or cosmic rays) with atmosphere.

HESS in Namibia


HESS image of a supernovaremnant (RX J1713.7-3946;Aharonian et al. 2006)

10's of sources now detected,perspecive of having 500 ormore with CTA(improved sensitivity).

CH contributions in EPFZ(hardware) andISDC (“observatory”)Measures sites of

particle acceleration

origin of cosmic rays.


Future Challenges of high energy astrophysics:

-Physics of matter in extreme conditions

Formation of first black holes (quasars) very early in the Universe


Need to increase sensitivity by large factor

Current technologies cannot be scaled up(X-ray optics: mass scales with area, i.e. with signalgamma ray optics: mass scales with (s/n)3)XMM and INTEGRAL are as massive as can be launched (in practical terms)

XEUS concept: light weight X-ray optics

Move from Ni shells optics to optics based onX-ray reflecting Si Wafers optics

gain a factor 10 mirror area per unit of mass.


Take a Si Wafer,etch grooves (~1mmx1mm)bend the plates to match optical req.stack them so that Si sticks to Si

Coating for high energy reflectivity

7cm

Reflective surf.

Hasinger et al. SPIE 2006 and ESA docs


Expect ~5-10” angular resolution

Formation flight toincrease focal length

ESA studies for nextlarge X-ray mission


Progress in the 100keV-10MeV domain requiresfocusing....

P. von Ballmoos et al. Toulouse

Problem: monochromatic device


Claire, Von Ballmoos et al.


At very high energies:

observe cosmic rays throughtheir Cerekov light production from above

Flux: rate is ~one per km2 per century at 1020eV

EUSO concept


High energy astrophysics is lively-many results coming in-stems from a combination of adequate funding and competent community

-There are many more questions to be dealt with

-There are technologies to address these questions

but

There is by far not enough funding

Great danger of loosing the community

Documents

X-ray and gamma ray observations · Accretion disk and a Compton component, ... à avril 2006 (février-avril et ... T. Courvoisier March 2007 X-ray and gamma ray observations 30