X-ray and gamma ray observations

Transcription

1 From a fraction of a kev (~ 10 Angstroem, few x 1016 Hz) to TeVs, i.e. >6 orders of magnitude Science that started when rockets reached space Most discoveries unexpected 1

2 Below a fraction of a kev interstellar medium is opaque abs ~e-σnh similar transmission at 1keV and in the IR domain Few attemps at measurements in the 100s Angstroem region (FUSE, EUVITA). 1Ry 2

3 X-ray Optics: Wolter optics: Grazing incidence focusing optics XMM angular resolution: 10 (conical approximation) Chandra: 1 3

4 XMM: 56 nested shells (Ni) 4

5 XMM Reflection Grating Spectrometer Resolution Angstroem 5

6 XMM ESA corner stone launched in December

7 Line and continuum contributions to thermal emission. X-ray spectroscopy very important diagnostics 7

8 Clusters of galaxies Kitt Peak XMM, Briel et al. Optical image dominated by galaxies (thausends), X-ray image by hot gas 8

9 A2052, X-ray spectrum, Kaastra et al. Perseus, Boehringer et al. Mass dominated by dark matter Gas has been processed in stellar interiors 9

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

11 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. 11

12 MeV region: difficult not only in the optical aspects, but also in the detection: E, MeV 12

13 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). INTEGRAL Vedrenne et al. A+A, 2003, vol

14 ISGRI: Imageur 2 plans de détection: ISGRI, CdTe detectors PICSIT, 4096 CsI detectors Pis: P. Ubertini (IAS), F. Lebrun (CEA). INTEGRAL Ubertini et al. A+A, 2003, vol

15 Shadowgrammes d'isgri Crabe: source brillante INTEGRAL 3C 273: source faible 15

16 Toutes les données transitent à l'isdc et y sont analysées Centre opérations de l'esa ISDC INTEGRAL4 16

17 IGR J Découverte le 29 janvier 2003 lors d'une observation de routine. Première d'une série d'objets engoncés dans un cocon de matière 2 First results of INTEGRAL 17

18 L es so u r c es o b sc u r es I G R J

19 GX5-1, Neutron star binary system A. Paizis et al. Accretion disk and a Compton component, hard tails are not a signature of the presence of black holes. First results of INTEGRAL 19

20 V in outburst, December 04. Cyclotron lines at 25, 55 and 75 kev Kreykenbaum et al 05 Jem-X ISGRI SPI on INTEGRAL March 2005 First results of INTEGRAL 2020

21 Centre de la Galaxie tous les 3 jours de février 2005 à avril 2006 (février-avril et août-octobre) Image moyenne First results of INTEGRAL 21

22 Anti électrons Électron + anti-électron --> annihilation e- + e+ > 2 photons à 511 kev Question: d'où viennent les anti-électrons? INTEGRAL J. Knödlseder et al. N. Mowlavi INTEGRAL 22

23 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. 23

24 POLAR Compton optics 24

25 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 traces and energies of the electron and positron EGRET on CGRO GLAST, to be launched in

26 Quasar 3C 273: archetype of quasars, z=0.158, L~1048ergs/s Turler et al. Chernyakova et al. 26

27 Above 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 27

28 HESS image of a supernova remnant (RX J ; Aharonian et al. 2006) 10's of sources now detected, perspecive of having 500 or more with CTA (improved sensitivity). Measures sites of particle acceleration CH contributions in EPFZ (hardware) and ISDC ( observatory ) origin of cosmic rays. 28

29 Future Challenges of high energy astrophysics: -Physics of matter in extreme conditions Formation of first black holes (quasars) very early in the Universe 29

30 Need to increase sensitivity by large factor Current technologies cannot be scaled up (X-ray optics: mass scales with area, i.e. with signal gamma 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 on X-ray reflecting Si Wafers optics gain a factor 10 mirror area per unit of mass. 30

31 7cm Reflective surf. 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 Hasinger et al. SPIE 2006 and ESA docs 31

32 Expect ~5-10 angular resolution Formation flight to increase focal length ESA studies for next large X-ray mission 32

33 Progress in the 100keV-10MeV domain requires focusing... P. von Ballmoos et al. Toulouse Problem: monochromatic device 33

34 Claire, Von Ballmoos et al. 34

35 At very high energies: observe cosmic rays through their Cerekov light production from above Flux: rate is ~one per km2 per century at 1020eV EUSO concept 35

36 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 36