X/ -ray Instrumentation The development of high-energy astrophysics X-ray and -ray instrumentation 4. The development of high- energy Astrophysics.

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)



Index

• Some historical remarks• The early days: rockets & balloons• The first orbiting observatories• The telescopes• The current epoch:

– Chandra– XMM-Newton– Integral



Riccardo Giacconi (Genoa 1931)

1962

2002



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.



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!

Sco X-1

FRX



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)



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)



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



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



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



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 inMCG-6-30-15



Rossi X-ray Timing Explorer (RXTE): 1995-



RXTE

• Very high timing resolution (1s)

• 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)



The big observatories



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)



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/E1000 (+ACIS-S)


The development of high-energy astrophysicsXMM-Newton



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



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)



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)



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



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.



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)



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



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)



XMM-Newton SOC Pipeline Processing:Data Products

XMM-NewtonScience Archive

XMM-Newton data flow

PI

PPS: Pipeline Data processing



OAS StrasbourgAutomatedprocessing

Archive searches

Screening of Data products

XMMSOC

IFCA Santander

LU Leicester

PPS:The SSC bit

Support/backup:MPE, LU, CESR



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



dMe Star

QSOz=0.565

Sy 2z=0.238

NGC 4291z=0.0058

QSOz=2.649

Sy 1z=0.330



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



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. PallaviciniR. MushotzkyJ. BergeronR. GriffithsP. CharlesX. BarconsA. ComastriM. 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)



Comparison of Chandra and XMM-Newton

XMM-Newton:

•Mirror area 0.4 m2

•Spatial resolution 15’’ HEW•Limiting sensitivity: 10-15 erg cm-2 s-1

Chandra:

•Mirror area 0.08 m2

•Spatial resolution 0.5’’ HEW•Limiting sensitivity: 10-16 erg cm-2 s-1



INTEGRAL

Launch: 17 Oct 2002

Range: 20 keV – 10 MeV



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



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

X/ -ray Instrumentation The development of high-energy astrophysics X-ray and -ray instrumentation 4. The development of high- energy Astrophysics.

Documents

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cosmic xray background1970

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