sorry for not being able to attend!

1. sorry for not being able to attend!

2. The NHXM consortium A strong international scientific support from various countries, institutes and scientists • Hardware team • Denmark: National Space Institute, Technical University of Denmark • Finland: University of Helsinki • Germany: Tübingen University • Italy: Various INAF institutes, INFN-Pisa, Universita’ di Roma3, • Politecnico di Milano • Poland: N.Copernicus Astronomical Center, Space Research Center Spain: University of Valencia, University of Alicante, IFCA, INTA • UK: University of Leicester • USA: SAO-CfA & MSFC + Yale, PSU, GSFC, OSU, JHU … 2

3. New Hard X-ray Mission main features • Single satellite with extendable bench • Four high quality (XMM-like) mirrors with multilayer coatings sensitive in the band 0.2-80(120) keV • Three Telescope Modules dedicated to broad band imaging & spectroscopy • One telescope Module dedicated to imaging polarimetry (2-35 keV) • A Wide Field X-ray monitor (2-50 keV) • LEO (equatorial)  low internal background 3

4. Mission Configuration

5. NHXM: Core scientific objectives • Black hole cosmic evolution and accretion physics • resolve at least 60-70% of the CXB in the energy range where it peaks (20 -30 keV) • constrain the physics of the accretion flow onto both SMBH and solar mass BH • solve the puzzle on the origin of the hard X–ray emission from the Galactic centre • Acceleration mechanisms and non-thermal emission • constrain acceleration processes in relativistic Jets of blazars and GRB • measure the maximum energy of electron acceleration in supernova remnants shocks • Shock development and cosmic ray production in SNR and intra-cluster medium • Physics of matter under extreme conditions • Behaviour of matter in extreme gravitational and magnetic fields • Emission line profiles, continuum shape and polarization properties used to estimate BH spin • Polarization measurements & Broad cyclotron resonance in high magnetic field X-ray pulsars to study the transfer of radiation and determine field geometry

6. ROSAT Compton thick AGNs and the X-ray cosmic background XMM-Newton Chandra NHXM obscured C-thin obscured C-thick unobscured

7. NHXM NuStarAstro-H 20-40keV . 2-10 keV Chandra/XMM Gilli et al. Treister et al. Compton thick AGNs and the X-ray cosmic background

8. The Galactic Centre

9. Acceleration mechanisms • Jet emission is due to both synchrotron and IC, both BB components and strongly polarized. • Therefore, multi-band (IR,O,X-ray) spectroscopy and polarimetry can probe • jet structure • nature of jet seed photons • jet power

10. X-ray Polarimetry with imaging capabilities The possibility to associate to the polarimetric sensitivity also an imaging capability is of paramount importance in the case of extended sources investigation, like e.g. the SN remnants and the GC region. 10

11. Missing SMBH Geometry of the torus: the polarization angle will give us the orientation of the torus, to be compared with IR results, and with the ionization cones

12. Polarimetric sensitivity Soft X-ray channel Two polarimetric channels (2 – 10 keV and 10 – 35 keV) for an effective diagnostic of the emission mechanisms Hard X-ray channel Cross correlation with the spectroscopy data between 2 and 36 keV! 12

13. NHXM: top-level scientific requirements

14. Baseline and goal mirrors effective area 10% spider vignetting

15. Flux Sensitivity (1 Ms) 15

16. Hard X-ray Imaging capability 2-Ms 10-40 keV simulations of a 10’ region of the CDFS HEW=15” HEW=45” Two input source catalogs have been used: 1) sources detected by Chandra in the 2-10 keV band (Luo et al. 2008, ApJS, 179,19); 2) the candidate highly obscured AGN selected in the mid-infrared by Fiore et al. (2008, ApJ, 672, 94). 16

17. Key parameters of future hard X-ray missions

18. EM3: optics calibration @ Panter/MPE 1 keV 40 keV

19. EM1 EM2 Panter measurements of EM1, EM2 & EM3 HEW Effective Area

20. NHXM Focal Planes 3 mirror modules with a hybrid focal plane one mirror module with a photoelectric imaging polarimeter CCD, CdTe array, anticoincidence system (NaI or CsI)

21. Two independent and compact detector modules 21

22. NHXM: Low Energy detector E2v CCD Back-illuminated with high low QE 120 µm depletion (150 goal) 22

23. NHXM: High Energy detector 23

24. NHXM: High Energy detector 24

25. NHXM: High Energy detector 25

26. Summary The discovery space of the NHXM mission is extremely wide; also thanks to the addition of simultaneous imaging polarimetry and wide field X-ray monitor. This is achievable by the small/medium-size NHXM project, exploiting already available technology in mirror and detector manufacturing, well within the next decade. NHXM is a big step forward following on the hard X-ray focusing missions NUSTAR and ASTRO-H and on the polarimetric GEMS mission. NHXM will also be a good precursor for IXO, testing various technologies that are foreseen on a much larger scale for IXO. All technologies have old and strong roots, building up on the BeppoSAX, XMM, INTEGRAL, AGILE & Swift heritage and on the recent technological advance made for the mirrors, polarimeter, detectors and truss. The NHXM proposal submitted to ESA was based on 50% of the M3 budget with a launch in the time frame 2020. A strong international team has been formed. 26

27. 1 single module = 1 NHXM + 1 GRAVITAS units (nested together) MASS (1 MODULE)≈ 200 kg + 6 mirror modules NHXG (New Hard X-rayGravitas)