X-RAY ASTRONOMY: AN OVERVIEW GIORGIO MATT (DIPARTIMENTO DI MATEMATICA E FISICA, UNIVERSITÀ ROMA TRE, ITALY)

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1 X-RAY ASTRONOMY: AN OVERVIEW GIORGIO MATT (DIPARTIMENTO DI MATEMATICA E FISICA, UNIVERSITÀ ROMA TRE, ITALY)

2 THE LANDSCAPE MISSIONS PRESENTLY IN OPERATION: CHANDRA, XMM-NEWTON, INTEGRAL, SWIFT, SUZAKU, NUSTAR MISSIONS TO BE LAUNCHED IN THE NEAR FUTURE : ASTROSAT, erosita, ASTRO-H, NICER MISSIONS UNDER COMPETITION: LOFT, ATHENA+ MISSION CONCEPTS: WFXRT, X-RAY POLARIMETRY, LAUE LENS,

3 ALL CLASSES OF ASTROPHYSICAL SOURCES EMIT SIGNIFICANTLY IN X-RAYS OR WITHOUT X-RAY OBSERVATIONS OUR KNOWLEDGE OF ANY CLASS OF ASTROPHYSICAL SOURCES IS INCOMPLETE

4 NuSTAR The Nuclear Spectroscopic Telescope Array

5 INTEGRAL, Swift BAT NuSTAR Focal spot Grazing incidence optics

6 KEY SCIENCE PROGRAMS Key science goal Observations Time (weeks) Locate massive black holes Study the population of compact objects in our Galaxy Explosion dynamics and nucleosynthesis in core collapse and 1a SNe Understanding relativistic jets in supermassive black holes Deep and wide-field extragalactic surveys (ECDFS, COSMOS, BAT-shallow) Survey Galactic Center and other fields of varied ages (spiral arms, bulge) Pointed observations of young ( < 500 yr) remnants Cas A, SN1987A, GX1+9 ToO observations of nearby SN1a Contemporaneous multiwavelength observations of GeV/TeV blazars Other Objectives Observations Time Varied 33 THANKS TO THE USE OF THE MALINDI STATION, ITALIAN SCIENTISTS ARE INCLUDED IN THE SCIENCE TEAM

7 BASELINE MISSION SCIENCE Science Group Galactic Surveys, Galactic Center Supernovae and ToOs Supernova remnants and Pulsar Wind Nebulae Magnetars and Rotation Powered Pulsars Galactic Binaries Ultraluminous X-ray Sources Extragalactic Surveys Blazars and Radio Galaxies Obscured AGN AGN Physics Galaxy Clusters Starburst Galaxies Solar Physics Working Group Chair Chuck Hailey Steve Boggs Fiona Harrison Vicky Kaspi John Tomsick Fiona Harrison Daniel Stern Greg Madejski, Paolo Giommi Daniel Stern Giorgio Matt Allan Hornstrup, Silvano Molendi Ann Hornschemeier David Smith PLUS MANY OTHER ITALIAN SCIENTISTS

8 FIRST NUSTAR PAPER NGC 1365 (RISALITI ET AL. 2013)

9 ASTROSAT (2013) ASTROSAT WILL CARRY FIVE ASTRONOMY PAYLOADS FOR SIMULTANEOUS MULTI- BAND OBSERVATIONS: TWIN 40-CM ULTRAVIOLET IMAGING TELESCOPES (UVIT) COVERING FAR-UV TO OPTICAL BANDS THREE UNITS OF LARGE AREA XENON PROPORTIONAL COUNTERS (LAXPC) COVERING MEDIUM ENERGY X-RAYS FROM 3 TO 80 KEV WITH AN EFFECTIVE AREA OF 6000 SQ.CM. AT 10 KEV A SOFT X-RAY TELESCOPE (SXT) WITH CONICAL FOIL MIRRORS AND X-RAY CCD DETECTOR, COVERING THE ENERGY RANGE KEV. THE EFFECTIVE AREA WILL BE ABOUT 200 SQ.CM. AT 1 KEV A CADMIUM-ZINC-TELLURIDE CODED-MASK IMAGER (CZTI), COVERING HARD X- RAYS FROM 10 TO 150 KEV, WITH ABOUT 10 DEG FIELD OF VIEW AND 1000 SQ.CM. EFFECTIVE AREA A SCANNING SKY MONITOR (SSM) CONSISTING OF THREE ONE-DIMENSIONAL POSITION-SENSITIVE PROPORTIONAL COUNTERS WITH CODED MASKS. THE ASSEMBLY WILL BE PLACED ON A ROTATING PLATFORM TO SCAN THE AVAILABLE SKY ONCE EVERY SIX HOURS IN ORDER TO LOCATE TRANSIENT X-RAY SOURCES.

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11 erosita (2014) SEVEN IDENTICAL WOLTER-1 MIRROR MODULES, WITH CCD DETECTORS KEV ENERGY RANGE. ANGULAR RESOLUTION OF 15 ON-AXIS, UP TO 30. F.O.V. 1 DEG. IN DIAMETER. EFF. AREA 1500 CM KEV 3 ks pointing COMPLEMENTED BY ART-XC, CODED MASKED TELESCOPES WITH ANGULAR RESOLUTION OF ABOUT 1, F.O.V. OF 30, 6-30 KEV ENERGY RANGE.

12 erosita ALL SKY SURVEY (2-3 KS PER FIELD) DEEP SURVEYS (200 DEG 2, KS) MAIN GOAL: LARGE SCALE STRUCTURE AND DARK ENERGY WITH CLUSTERS OF GALAXIES COSMOS FIELD EXPECTED # OF AGN (0.5-2 KEV) 1.76 X 10 6 (ASS) (DS) EXPECTED # OF AGN (2-10 KEV) (ASS) (DS)

13 ASTRO-H (2015) THIRD JAPANESE MISSION WITH MICROCALORIMETER - FIRST TWO FAILED, BUT THE MICROCALORIMETER WAS TESTED SUCCESSFULLY IN SUZAKU. ENERGY RESOLUTION OF ABOUT 5 EV. IT WILL REVOLUZIONIZE THE IRON LINE STUDIES. MANY INSTRUMENTS AND TELESCOPES, COVERING OVERALL THE KEV BAND ( KEV WITH FOCUSING TELESCOPES, SPATIAL RESOLUTION OF ABOUT 90 ) SIMILARLY TO ASCA AND SUZAKU, A FRACTION OF OBSERVING TIME WILL BE AVAILABLE TO ESA MEMBER STATES VIA GO PROGRAM.

14 ASTRO-H INSTRUMENTS Hard X-ray telescope (HXT) Fixed FL=12 m Optical bench SUN radiator Soft X-ray telescope FL=5.6 m Soft X-ray spectrometer Soft X-ray imager (Micro calorimeter) (X-ray CCD camera) Extended Optical bench Soft Gamma-ray detector Hard X-ray Imager (HXI) Double-sided Si Strip (4 layer) detector + CdTe double strip(1 layer) detector Si/CdTe Compton camera ASTRO-H WILL COVER THE BANDPASS BETWEEN 0.3 KEV TO 600 KEV.

15 ASTRO-H TURBULENT VELOCITY IN CLUSTERS OF GALAXIES FAST VELOCITY OUTFLOWS IN AGN

16 NICER NEUTRON STAR INTERIOR COMPOSITION EXPLORER LAUNCH: 2016 ATTACHED PAYLOAD ABOARD THE INTERNATIONAL SPACE STATION (ISS) GRAZING-INCIDENCE OPTICS COUPLED WITH SILICON DRIFT DETECTORS, WILL PROVIDE SPECTROSCOPY AND TIMING IN THE KEV

17 THE ESA PROGRAM M3 (2022/2024): LOFT, PLATO, ECHO, MARCO POLO-R, STE-QUEST FINAL SELECTION: EARLY 2014 L2/L3 (2028/2034): ATHENA+,.. SUBMISSION OF SCIENTIFIC THEMES/MISSION CONCEPTS: MAY 24, 2013 SELECTION: 4Q 2013 M4 (2026?): CALL IN 2014? SMALL MISSIONS: ANOTHER CALL IN A FEW YEARS?

18 WFXRT 1 DEG 2 F.O.V. WITH A FLAT ~5 PSF

19 X-RAY POLARIMETRY A MATURE TECHNIQUE >

20 LOFT: the Large Observatory For x-ray Timing LOFT Science Team composed of scientists from: Australia, Brazil, Canada, CzechRepublic, Denmark, Finland, France, Germany, Greece, Ireland, Israel, Italy, Japan, thenetherlands, Poland, Spain, Sweden, Switzerland, Turkey, United Kingdom, USA

21 THE LOFT MISSION LOFT is specifically designed to exploit the diagnostics of very rapid X-ray flux and spectral variability in compact objects, yielding unprecedented information on strongly curved spacetimes and matter under extreme conditions of density and magnetic field strength. LOFT will investigate variability from submillisecond QPO s to years long transient outbursts. The LOFT LAD has an effective area ~20 times larger than any largest predecessor, uniquely combined with a CCD-class energy resolution. The LOFT WFM has a few steradian field of view at soft X-rays to discover and localise X-ray transients and impulsive events and monitor spectral state changes, triggering follow-up observations and providing a wealth of science in its own.

22 THE LOFT SCIENCE Neutron Star Structure and Equation of State of ultradense matter: - neutron star mass and radius measurements - neutron star crust properties 4U (582 Hz) Strong gravity and the mass and spin of black holes - QPOs evolution and in the time domain - Fe line reverberation studies in bright AGNs - Relativistic precession RXTE 54ks LOFT 1 ks Observatory Science, for virtually all classes of relatively bright sources, including: X-ray bursters, High mass X-ray binaries, X- ray transients (all classes), Cataclismic Variables, Magnetars, GRBs, Nearby galaxies (SMC, LMC, M31, ), AGNs

23 THE LOFT INSTRUMENTS Effective Area Energy range Energy resolution FWHM Collimated FoV Time Resolution Absolute time accuracy Dead Time Background Max Flux LAD Large Area Detector 4 m 2 kev 8 m 5 kev 10 m 8 kev 1 m 30 kev 2-30 kev primary kev extended kev kev (45% of area) 1 degree FWHM 10 s 1 s <1% at 1 Crab <10 mcrab (<1% syst) 500 mcrab full event info 15 Crab binned mode Energy range WFM- Wide Field Monitor Active Detector Area 1820 cm 2 Energy resolution FOV (Zero Response) Angular Resolution 5 x 5 Point Source Location Accuracy (10-σ) Sensitivity (5-σ, on-axis) Galactic Center, 3 s Galactic Center, 1 day Standard Mode Trigger Mode 2-50 kev primary kev extended 300 ev 6 kev 180 x x90 1 x mcrab 2.1 mcrab 5-min, energy resolved images Event-by-Event (10 s res) Realtime downlink of transient 23 coordinates

24 THE SOYUZ CONFIGURATION SWITCH TO SOYUZ LAUNCHER: HUGE MASS MARGIN, LARGE VOLUME MARGIN, CONFIGURATION OPTIMIZATION

25 L2/L3: THE NEXT GENERATION LARGE X-RAY OBSERVATORY For L2/L3 we need a mission which will give an answer to very fundamental questions which can be addressed only in X-rays and at the same time will ensure a progress in our understanding of all classes of astrophysical sources. We need a Large X-ray Observatory to provide in X-rays the same leap forward provided at other wavelenghts by SKA, ALMA, JWST, ELT, CTA, etc

26 Athena+: Revealing the Hot and Energetic Universe

27 The Hot and Energetic Universe Where are the hot baryons and how do they evolve? How do black holes grow and shape the Universe? The Astrophysics of the Hot and Energetic Universe Cosmic Web Feedback Processes Black Hole Accretion [ Athena+ ] Advanced Telescope for High Energy Astrophysics

28 1. Where are the hot baryons and how do they evolve? Reveal and map the first viralised baryonic structures Wide field X-ray imaging, imaging X-ray spectroscopy Determine their dynamical, thermal and chemical evolution Spatially-resolved X-ray spectroscopy, wide field imaging Complete the census of baryons in the local Universe High resolution X-ray spectroscopy Understand the physics of clusters and groups Imaging X-ray spectroscopy, wide field of view imaging Structure Formation Baryonic Evolution Cosmic Web Cluster Physics [ Athena+ ] Advanced Telescope for High Energy Astrophysics

29 2. How do black holes grow and influence the Universe? Reveal the causes and effects of cosmic feedback Imaging X-ray spectroscopy, high resolution spectroscopy Understand the physics of accretion onto compact objects Fast spectral timing, high throughput spectroscopy Track obscured accretion through the epoch of galaxy High throughput wide field X-ray imaging, high throughput spectroscopy Perform a census of black hole growth at high redshift Deep wide field X-ray imaging XMM-Newton Cosmic Feedback Accretion physics Obscured accretion High z SMBH [ Athena+ ] Advanced Telescope for High Energy Astrophysics

30 3. The Astrophysics of the Hot and Energetic Universe Compact Objects X-ray binaries, neutron star and pulsars, white dwarfs Stellar Evolution Young stars, stellar winds, stellar activity, supernovae, GRBs The Milky Way Galactic centre, interstellar dust and gas, hot gas halo Planets and the solar system Planets, exoplanets, comets, solar wind Neutron Stars Stellar Activity Galactic Centre Charge Exchange [ Athena+ ] Advanced Telescope for High Energy Astrophysics

31 Science Requirements Requirement Driver Effective Area 2m 1 kev (goal 2.5m 2 ) 0.25m 6 kev (goal 0.3m 2 ) Angular Resolution 5 (goal of 3 ) Fields of view WFI: 40 diameter (goal 50 ) XMS: 5 x 5 (goal 7 x 7 ) Spectral resolution Count rate capability kev (WFI) 2.5 ev (X-IFU) goal 1.5 ev Hot Baryons Black hole evolution Accretion Physics Black Hole Evolution Hot Baryons Hot Baryons Black Hole Evolution Black Hole Evolution Hot Baryons >1 Crab Accretion Physics Timing resolution 50 s Accretion Physics TOO response 8 hours (2 hours goal) Hot Baryons [ Athena+ ] Advanced Telescope for High Energy Astrophysics 31

32 Notional Athena+ Mission Profile Ariane V launch to L2, 5yr nominal mission Payload Focal plane Service Module 12m Fixed Focal Length Wide Field Imager (Si-based DEPFET) X-ray Integral Field Unit (TES calorimeter) ESA Silicon Pore Optics 5 (3 ) resolution Mirror Assembly [ Athena+ ] Advanced Telescope for High Energy Astrophysics

33 ESA L-class process Cornerstone approach for large missions (as H2000) Budget ~ 0.9bn ESA cost (plus ~ 200M ESA MS) ESA-led, max. ~20% non-critical int. contribution OK Senior Committee to select single science theme for L2 (2028) and single theme for L3 (2034) L-class call-to-launch assumption: 14 years Timeline: May 24th: white papers on science themes, mission concept September 2-3: Open workshop on science themes mid-november: Selection of L2 and L3 based on SC/ESA recommendation L2 mission call in 2014 (L3 in ~2020) [ Athena+ ] Advanced Telescope for High Energy Astrophysics

34 X-ray Observatories: Timeline Chandra 1999 NuSTAR 2012 Astro-H 2014 Uncertain Future? Athena XMM-1999 Suzaku 2005 Spektr-RG ASTROSAT (India), HXMT (China) [ Athena+ ] Advanced Telescope for High Energy Astrophysics

35 A (PERSONAL) CONCLUSION THE X-RAY COMMUNITY (AND THE ASTROPHYSICAL COMMUNITY AT LARGE) NEEDS THE NEXT GENERATION LARGE X-RAY OBSERVATORY IN A HEALTHY, SCIENTIFICALLY-DRIVEN LONG TEM PROGRAM THIS SHOULD NOT BE SEEN IN COMPETITION WITH FOCUSED EXPERIMENTS WHICH MAY HAPPEN TO BE PERFORMED IN X-RAYS