1. X/  -ray Instrumentation The development of high-energy astrophysics X-ray and  -ray instrumentation 4. The development of high- energy Astrophysics Xavier Barcons Instituto de Física de Cantabria (CSIC-UC)

2. X/  -ray Instrumentation The development of high-energy astrophysics Index Some historical remarks The early days: rockets & balloons The first orbiting observatories The telescopes The current epoch: –Chandra –XMM-Newton –Integral

3. X/  -ray Instrumentation The development of high-energy astrophysics Riccardo Giacconi (Genoa 1931) 1962 2002

4. X/  -ray Instrumentation The development of high-energy astrophysics R. Giacconi: greatest hits Post-degree in experimental particle physics (Milano). 1959: Member and later CEO of ASE (American Science & Engineering Corporation) in Cambridge (USA). 1962: Discovery of the first X-ray source outside the Solar System (Sco X-1) and of the Cosmic X-ray Background 1970: Launch of UHURU, the first orbiting X-ray observatory 1978: Launch of Einstein, the first orbiting X-ray observatory equipped with X-ray focusing optics. 1981-1992: Director general of Space Telescope Science Institute 1992-1999: Director general of European Southern Observatory 1999- : Chairman of Associated University Inc. Researcher of many Astrophysical problems related to X-ray Astronomy, in particular the X-ray background, clusters of galaxies, Cosmology, active galaxies and the Sun.

5. X/  -ray Instrumentation The development of high-energy astrophysics The beginning of high-energy Astronomy 18-June-1962: Giacconi and collaborators fly an Aerobee rocket beyond 80 km altitude during > 5 minutes with 3 X-ray detectors Goal: To detect X-rays reflected in the Moon from the Sun Two surprising discoveries: An extremely bright X-ray source, which is very inconspicuous in the optical (Sco X-1) Diffuse radiation from all directions in the Universe (the cosmic X-ray Background) And of course, no trace from the Moon… … until 1990!

6. Sco X-1 FRX

7. X/  -ray Instrumentation The development of high-energy astrophysics A brief history of high-energy Astronomy 1962: Discovery of Sco X-1 and of the Cosmic X- ray background 1962-1970:Rockets with detectors 1970-1980: Orbiting collimators (resolution ~ degrees) 1980-1990: First soft X-ray telescopes (Einstein, EXOSAT) 1990-now:First hard X-ray telescopes (Chandra, XMM-Newton) and  -ray observatories (Granat, CGRO, Integral)

8. X/  -ray Instrumentation The development of high-energy astrophysics Orbiting collimators: UHURU Launched 12 Dec 1970 from Kenya Payload weighted 56 kg! Scanned the full sky at a resolution of several degrees Produced the first catalogue with hundreds of X-ray sources UHURU (1970-73)

9. X/  -ray Instrumentation The development of high-energy astrophysics HEAO-1 All-sky survey in 2-60 keV band with various instruments. Bright sources positioned with modulation collimator to 1 arcmin resolution Intensity and spectrum of the X-ray background

10. X/  -ray Instrumentation The development of high-energy astrophysics Soft X-ray telescopes: Einstein IPC: Imaging proportional counter: –1.5’ resolution –  E/E~2 HRI: High resolution imager –Few “ resolution –No spectral resolution SSS: Solid State Spectrometer BCS: Bragg Crystal Spectrometer Einstein Observatory (1979-83) 0.3-3.5 keV First deep surveys Extragalactic sky

11. X/  -ray Instrumentation The development of high-energy astrophysics ROSAT Position Sensitive Proportional Counter (PSPC) –30” resolution –  E/E~4 High Resolution Imager (HRI): –4” resolution –No spectral resolution ROSAT (1990-98) 0.1-2.4 keV All sky survey (6 months) 10 years of pointed observing

12. X/  -ray Instrumentation The development of high-energy astrophysics ASCA SIS0 & SIS1 (CCD detectors) –  E/E~10-20 –Field of view 20’ GIS1 & GIS2 (Gas scintillator proportional counters) –Somewhat lower  E/E –Field of view 50’ ASCA (1993-2001) 0.5-10 keV (long focal) Thin foil mirrors, 2-3’ res First observatory in hard X-rays: Fe lines First broad Fe line detected in MCG-6-30-15

13. X/  -ray Instrumentation The development of high-energy astrophysics Rossi X-ray Timing Explorer (RXTE): 1995-

14. X/  -ray Instrumentation The development of high-energy astrophysics RXTE Very high timing resolution (1  s) Very broad energy band (2-200 keV) Low-earth orbit Limited positional information. Designed to observe bright sources in (timing) Proportional Counter Array (PCA): 2-20 keV High Energy X-ray Timing Experiment (HEXTE): 20- 250 keV –Both with a collimator ~1º All Sky Monitor (ASM): ~80% of sky every orbit (~90min)

15. X/  -ray Instrumentation The development of high-energy astrophysics The big observatories

16. X/  -ray Instrumentation The development of high-energy astrophysics Chandra NASA: (23-VII-1999, Columbia) High spatial resolution (0.5“), low resolution spectroscopic (E/  E~20- 50) imaging Medium to high spectral resolution (0.02-0.04 Ang) dispersive spectroscopy (~0.5-7 keV)

17. X/  -ray Instrumentation The development of high-energy astrophysics Chandra High Resolution Camera (HRC): MCP Advance CCD Imaging Spectrometer (ACIS) Low Energy Transmission Grating (LETG): 0.08-2 keV, E/  E=30-2000 (+HRC-S) High Energy Transmission Grating (HETGS): 0.4-10 keV, E/  E  1000 (+ACIS-S)

18. X/  -ray Instrumentation The development of high-energy astrophysics XMM-Newton

19. X/  -ray Instrumentation The development of high-energy astrophysics XMM-Newton ESA (10-XII-1999): Moderate spatial resolution (~12-15”) medium spectral resolution (E/  E~20-50 ) imaging over 0.2-12 keV and large field of view. Medium to high resolution spectroscopy (~0.06 Ang) Optimised for X-ray spectroscopy and surveys

20. X/  -ray Instrumentation The development of high-energy astrophysics Instruments: EPIC Spectroscopic imaging in the 0.2-12 keV band 2 MOS + 1 pn Spectral resolution: 20-50 Field of view: 30 arcmin Sensitivity (100 ks) ~ 10 -15 erg cm -2 s -1 (confusion limited)

21. X/  -ray Instrumentation The development of high-energy astrophysics Instruments: RGS Dispersive spectroscopy, in the range 5-35 Angstrom. RGS1 + RGS2, in several orders Spectral resolution ~200- 500 (0.02-0.08 Angstrom) Sensitivity (100 ks) ~ 10 -11 erg cm -2 s -1 (photon starved)

22. X/  -ray Instrumentation The development of high-energy astrophysics Instruments: OM Optical/UV equipped with grisms, filters and detector (counter) in the range 1600 - 6600 Ang. Field of view: 17’ PSF~1.3-2.5” Sensitivity (1000 seg)~ 23.5 mag

23. X/  -ray Instrumentation The development of high-energy astrophysics Science operations All instruments operated simultaneously Data are delivered to the observation’s PI de la within ~1 month, including the Observation Data File (ODF) and the reduced data (Pipeline products): –Calibrated event files (EPIC+RGS+OM) –Images (EPIC+RGS+OM) –Spectra (RGS+EPIC?) –Source lists, etc. ESA-funded SOC also provides and supports the SAS package (+calibration files), specifically designed for XMM-Newton. SAS is a joint effort of SOC and the nationally funded Survey Science Centre (SSC). Calibration is a joint effort of SOC and nationally funded instrument teams.

24. X/  -ray Instrumentation The development of high-energy astrophysics The XMM-Newton Survey Science Centre (SSC) Consortium of 10 European Institutes, PI: M.G. Watson, Leicester University (UK) Tasks: –Develop SAS (Science Analysis Software) in conjunction with ESA’s SOC –Pipeline process all data –Conduct an identification programme of serendipitous X-ray sources (incl source catalogue)

25. X/  -ray Instrumentation The development of high-energy astrophysics The SSC consortium University of Leicester, UK Astrophysikalisches Institut Potsdam, D IoA, Cambridge, UK Observatoire Astronomique de Strasbourg, F Max-Planck Institut für Extraterrestrische Physik, D Mullard Space Science Laboratory, UK Instituto de Física de Cantabria, E CEA/Saclay, F CESR, Toulouse, F Osservatorio Astronomico di Brera, I PI: Mike Watson

26. X/  -ray Instrumentation The development of high-energy astrophysics SAS: Software development Distributed task development (SSC+SOC) and integration (SOC) Daily build of various SAS versions (development, etc) on various platforms (SOC+SSC) Maintenance (SOC+SSC) Helpdesk assistance (SOC) User training courses (SOC)

27. X/  -ray Instrumentation The development of high-energy astrophysics XMM-Newton SOC Pipeline Processing: Data Products XMM-Newton Science Archive XMM-Newton data flow PI PPS: Pipeline Data processing

28. X/  -ray Instrumentation The development of high-energy astrophysics OAS Strasbourg Automated processing Archive searches Screening of Data products XMM SOC IFCA Santander LU Leicester PPS:The SSC bit Support/backup: MPE, LU, CESR

29. X/  -ray Instrumentation The development of high-energy astrophysics XID: The XMM-Newton serendipitous sky survey Every new XMM-Newton pointing (with EPIC in full window mode) discovers ~30- 150 serendipitous X-ray sources. About 50,000 new X-ray sources/year XMM-Newton SSC tasks –Identifications –Source catalogue

30. X/  -ray Instrumentation The development of high-energy astrophysics dMe Star QSO z=0.565 Sy 2 z=0.238 NGC 4291 z=0.0058 QSO z=2.649 Sy 1 z=0.330

31. X/  -ray Instrumentation The development of high-energy astrophysics The XMM-Newton Science Archive (XSA) Archive all ODFs (raw data) and up-to-date pipeline products (PPS) Guarantee data rights of PIs Provide easy, friendly-access to non-experts Archive XMM source catalogue Next version: on-the-fly data selection and reduction

32. X/  -ray Instrumentation The development of high-energy astrophysics Feedback from the community: XMM-Newton Users Group XMM-Newton Users group. Advise the “Project Scientist” on the views and suggestions of the scientific community about the XMM-Newton project. J. Schmidt (Chair) R. Pallavicini R. Mushotzky J. Bergeron R. Griffiths P. Charles X. Barcons A. Comastri M. Van der Kliss M. Turner (EPIC) B. Aschenbach (TS) J. Kaastra (RGS) K.O. Mason (OM) M.G. Watson (SSC) M. Longair (OTAC) F. Jansen (PS) N. Schartel (SOC)

33. X/  -ray Instrumentation The development of high-energy astrophysics Comparison of Chandra and XMM-Newton XMM-Newton : Mirror area 0.4 m 2 Spatial resolution 15 ’’ HEW Limiting sensitivity: 10 -15 erg cm -2 s -1 Chandra: Mirror area 0.08 m 2 Spatial resolution 0.5 ’’ HEW Limiting sensitivity: 10 -16 erg cm -2 s -1

34. X/  -ray Instrumentation The development of high-energy astrophysics INTEGRAL Launch: 17 Oct 2002 Range: 20 keV – 10 MeV

35. X/  -ray Instrumentation The development of high-energy astrophysics INTEGRAL instruments SPI:  -ray spectrometer –Coded mask –High spectral resolution, low spatial resolution IBIS:  -ray imager –Coded mask –Low spectral resolution, higher spatial resolution and large field of view (12º) JEM-X: X-ray, monitor –Coded mask –Microstrip positional counters OMC: Optical Monitor Camera –Optical telescope –Imaging and time resolved photometry of pre-selected areas in the field of view

36. X/  -ray Instrumentation The development of high-energy astrophysics The INTEGRAL Science Data Centre (ISDC) Consortium of European Institutes located in Geneva (Switzerland) Receive and process all raw data Create catalogue of Gamma-ray sources Develop scientific analysis software, with the help of instrument teams