1. Overview on XTP sciences Zhang Shu (on behalf of the XTP science team) Institute of High Energy Physics

2. 2/81 XTP: an ambitious mission in future Missions crowed but short of: large area, polarization.

3. Selected for Phase 0/A in 2011, expected launch in around 2020. 3/26 XTP satellite

4. 3 m 55cm 1.8 m 45cm 4/26 SDD or DEPFETCZT, SDD or DEPFET XTP payload layout

5. Key properties of XTP Main requirements scientific drivers Effective area: ~0.9m 2 EOS, BH spins, GR effect Energy Coverage 1-100 keV broadband spectrum multi-wavelength variability Energy resolution 150eV@6keV broad Iron line measurement Time resolution <100μs sub-millisecond variability Polarization 3% @ 0.1 mCrab B, emission mechanism; emission geometry

6. 6/26 Collimated Detectors Imagers Polarimeters Effective Area

7. Effective Area Comparison XTP Collimated Detectors XTP total focusing XMM PN RXTE HEXTE NuSTAR 7/26

8. Key Sciences of XTP: One singularity (BH) Two stars (NS or quark star) Three extremes (gravity, density, magnetism)

9. Via observing extreme objects and studying extreme physics XTP will answer: are the fundamental physical laws universal?

10. The fundamentals/pillars of modern physics: 1, General relativity theory: large scale interaction valid under extreme gravity? 2, Quantum chromodynamics theory strong interaction, quark and gluon scale valid under extreme matter density? 3, Quantum electrodynamics theory interaction of electron and photon valid under extreme magnetic field?

11. 1, what are the condition for planet formation and the emergency of life? 2, how does the solar system work? 3, what are the fundamental physical laws of the universe? (XTP, LOFT, Athena, Nicer) 4, how did the universe originate and what is it made of? Athena? Nice Athena? Nicer (rather) than Athena? XTP? LOFT?

12. Competition with Athena and Nicer: Nicer specialized to study EOS : high time resolution, energy below 1 keV, detection area 2000 cm^2 XTP: covers < 1 keV band? Athena: even a larger detection area(2m^2@1keV) & extremely good energy resolution (calorimeter) XTP: earlier launch time and possible heritage from LOFT

13. More landscapes of astrophysics explored by XTP 1, To observe the entire outbursts of XRBs 2, BH accretion process and formation of jets: disk reflection, reverberation mapping, soft X-ray excess, disentangle the jet/corona X-rays, ULX 3, XRB timing, QPO, burst oscillation, accreting pulsar 4, Extremely violent events (burst and outburst) in the universe : gamma-ray burst, type-I burst, AXP and SGR 5, Diffuse emission, local bubble, SNR nebular 6, X-ray polarimetry 7, Heavily obscured AGN (Compton thick AGN)

14. Summarized into XTP science classes: two Key sciences: 1, GR effect (extreme gravity, BH, NS & QS) 2, EOS (extreme density, NS & QS) one important science: 3, Physics under extreme magnetism (AXP & SGR) one new astronomical window: 4, Physics of X-ray polarization four sciences as an observatory: 5, ULX 6, Diffuse emission and SNR 7, Extremely violent event like GRB 8, Physics in XRB evolution

15. Goal of 2014: come up with 8 XTP science supporting files Format of each file will be similar to Athena’s. 1, Execution summary propose 3-4 key issues be addressed in that science the corresponding observational targets or source features 2, Scientific threads and simulations perform simulations on every interesting scientific objects; probe the scientific potential of XTP; guide the design of the instrument ; optimize the configuration of the payload. 3,summary XTP will bring breakthrough

16. Files to be accomplished by XTP science team (so far over than 20 members) Subdivided into 7 individual scientific groups;

17. XTP key science: GR effect Key science key problems obs. & simu. GR under extreme gravity (1) how the most efficient energy release mechanism in the Universe works ？ (2) how strong gravity affects the behaviour of matter and radiation ？ (3) how the physics of accretion and ejection are related ？ (4) whether or not BHs are spinning, which in turn tells us about the history of their growth ？ GR test ； Disk/corona ； Inner dynamic of disk ; BH spin

18. Probe GR/BH: relativistically broadened iron line

19. Corona/disk structure of (Reverberation mapping) Time lag between 1-4keV and 0.3-1keV, Comparison between Athena and XMM 1H0707-495 IC4329A 1H0707-495: time lag to probe the transfer structure of corona

20. Inner structure, dynamic and spin of BH

21. XTP key science : probe EOS Mass precisely measured in radio Requirement to NS radius measurement: a precision of 5-10%

22. NS RADIUS MEASUREMENTS Iron lines: E. CackettQPOs: D. Barret Again, multiple complementary methods can be employed

23. Strategies in probing EOS key science: 1, Nicer strategy need cover < 1keV ; 2, XTE strategy need even larger detection area ; 3, XMM strategy the absorption lines in NS atmosphere, helpful for solving the basic problems of the color factor and the red shift.

24. XTP new science window: X-ray polarimetry Accreting black holes Black hole binaries: accretion geometry, BH spin Blazars: emission mechanism, jet composition? Radio quiet AGNs: corona geometry, unification model Strong magnetism Rotation-powered: acceleration regions PWN: B-field accretion powered pulsars: accretion and emission geometry Shell-type SNRs: particle acceleration, B-field Fundamental physics GR effect: space curvature, space-time frame dragging QED: vacuum polarization 冯骅， XTP 研讨会，西峰山庄

25. XTP important science: Physics under extreme magnetism Science target key issues obs. & simu. Physics under extreme magnetism ？ Cyclotron absorption line ？ polarization ？ Pulse profile ？ others ？ 1. structure of multi-pole magnetic field ？ 2. NS or QS ？ 3. magnetar property ？ 4. extreme outburst ？

26. Preliminary results of hunting for XTP scientific objectives and mining in simulations (see the following three talks)

27. Thank you ! Thank you !