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attend!

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The NHXM consortium

Hardware team

Denmark: National Space Institute, Technical University of DenmarkFinland: University of HelsinkiGermany: Tübingen UniversityItaly: 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, INTAUK: University of LeicesterUSA: SAO-CfA & MSFC + Yale, PSU, GSFC, OSU, JHU …

A strong international scientific support from various countries, institutes and scientists

New Hard X-ray Mission main features

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• Single satellite with extendable bench

o Four high quality (XMM-like) mirrors with multilayer coatings sensitive in the band 0.2-80(120) keV

o Three Telescope Modules dedicated to broad band imaging & spectroscopy

o One telescope Module dedicated to imaging polarimetry (2-35 keV)

oA Wide Field X-ray monitor (2-50 keV)

o LEO (equatorial) low internal background

Mission Configuration

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NHXM: NHXM: Core scientific objectivesCore scientific objectives

• Black hole cosmic evolution and accretion physics

• Acceleration mechanisms and non-thermal emission

- 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

- 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

unobscured

obscured C-thin

obscured C-thick

ROSATXMM-NewtonChandra

NHXM

Compton thick AGNs and the X-ray cosmic background

Compton thick AGNs and the X-ray cosmic background

NHXM NHXM NuStarNuStar Astro-H Astro-H 20-40keV20-40keV

..

2-10 keV Chandra/XMM2-10 keV Chandra/XMM

Gilli et al.

Treister et al.

The Galactic Centre

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

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.

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Missing SMBH

Geometry of the torus: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

Polarimetric sensitivity

Soft X-ray channel

Hard X-ray channel

Two polarimetric channels (2 – 10 keV and 10 – 35 keV) for an effective diagnostic of the emission mechanisms

Cross correlation with the spectroscopy data between 2 and 36 keV!

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NHXM: top-level scientific requirementsNHXM: top-level scientific requirements

Baseline and goal mirrors effective area

10% spider vignetting

Flux Sensitivity (1 Ms)

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Hard X-ray Imaging capability

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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).

Key parameters of future hard X-ray missions

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1 keV 40 keV

EM3:EM3: optics calibration @ optics calibration @ Panter/MPEPanter/MPE

Panter measurements Panter measurements of EM1, EM2 & EM3of EM1, EM2 & EM3

EM1

EM2

HEW

Effective Area

NHXM Focal Planes

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3 mirror modules with a hybrid focal plane

CCD, CdTe array, anticoincidence system (NaI or CsI)

one mirror module with a photoelectric imaging polarimeter

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Two independent and compact detector modules

NHXM: Low Energy detector

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E2v CCD

Back-illuminated with high low QE

120 µm depletion

(150 goal)

NHXM: High Energy detector

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NHXM: High Energy detector

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NHXM: High Energy detector

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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.

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NHXG (New Hard X-ray Gravitas)

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1 single module = 1 NHXM + 1 GRAVITAS units (nested together)

MASS (1 MODULE)≈ 200 kg

6 mirror modules