andrea santangelo, iaat paris 1.03, 2007towards a cta fp7 design study the kev – tev connection...

Paris 1.03, 2007 Towards A CTA FP7 Design Study Andrea Santangelo,IAAT

The keV – TeV Connection

eRosita, Simbol X and the others… X-ray Observatories in the CTA era

Andrea Santangelo

IAAT


Outline of the talk

• The KeV – TeV Connection: a few reasons of the “science case” (not exhaustive)

• A golden age for X-ray astronomy– eRosita– Simbol X– The Others (MIRAX, HXMT, NEXT,

EXIST…) (not exhaustive)

• Considerations

Only some of planned/designed/studied X-ray Observatories will be introduced…


Identification of Sources

Association is certainly spatial/morphology coincidence…

(Funk et al., astro-ph/0609586)

Hess ~2’ (Aharonian et al., 2006) ASCA AX J1813-178, highly absorbed, Hard (~1.8), extended INTEGRAL IGRJ18135-1751 (Ubertini et al., 2006), softer than ASCASwift-XRT (Landi 2006), hard source, highly absorbed VLA 20 and 90 cm young (~ 1ky) shell like SNR 2.5’ diameter (G12.82-0.02) coincident with HESS (Brogan 2005)XMM spectral and morphological studies, (Funk et al. 2006), compact core, extended tail, non thermal, highly absorbed

X-ray observation tracing the synchrotron emission of relativistic electrons are well suited to the identification of VHE Gamma Ray emitters


Identification of Sources (2)

XMM-Newton map around HESS J1813-178

(Funk et al., astro-ph/0611646)

It’s the positional and morphological coincidence that allows identification

Compact X- ray core Extended with a hard tail toward North-East Embedded in the radio shell type SNR G12.82-0.02 Hard Spectrum

Pulsar Wind Nebula, Composite SNR,

even if ….


Identification of sources (3)It’s not so easy, the case of Unidentified sourcesmay be very faint

Aharonian et al. -HEGRA collab.-, 2005

Prototype of Unidentified sources discovered by HESS Spectrum is a power law (~1.9), extended Gamma Ray Excess from Cygnus, Milagro (Abdo et al., 2006)Radio Emission (Peredes 2006X-ray studies, (Butt 2006, Mukherjee 2006)A deep, 50 ksec XMM Analysis is on going… (Horns et al., submitted)

Search for faint extended emission,

high sensitivity for low surface brightness

HESS 1303-631, HESS J1614-518, HESS 1702-420, HESS J1708-410…


A multimavelength coherent picture

Identification, that is understanding, implies that a coherent multiwavelength scenario must emerge

(Aharonian et al., astro-ph/0611813)

HESS map of RX J1713.7-3946

Contours are from ASCA (1-3 keV band) Correlation is amazing A single electron population generates both the X (Sync.) and the Gamma (IC) radiation Particle acceleration up to 100 TeV is required Model interpretation is not so easy (Lemoine et al., 2006)

See also RX J0852.0-4622


Spatially resolved spectral capability at X-rays is key

A key example: synchrotron cooling


HESS J1825-137H.E.S.S. 0.25-30 TeV

XMM 2-10 keV

20 pc

Aharonian et al., A&A 2006

Malizia et al., A&A 2006

TeVX-rays

Middle age PWN (21 kyears) The Pulsar powers an asymmetric synchrotron nebula, arcmin size in X-rays The VHE emitting region is wider shorter range of X-rays electrons due to synchrotron cooling

Gensler et al., 2003


Vela X

ROSATcontours

no emission from Vela pulsar detected

Vela pulsarPSR B0833−45

Aharonian et al., 448 A&A, 2006

•It coincides with the X-ray emission features observed with ROSAT and ASCA (2-10 keV) Map below

Middle age PWN (11 kyears) The Pulsar powers an asymmetric synchrotron nebula, observed in X-rays The VHE emitting region is slightly wider Leptonic or Hadronic production ? (Horns et al., 2006)


Hadronic interpretation Horns, D. et al. 2006, A&A


Spatially resolved spectral capability at Hard X-rays is essential


Timing…LSI +61 303, LS 5039

W. Hermsen, 2006

Albert et al., 2006


An “amazing” effort…


High-Energy Observatories 2004-2020

2004 20082006 2016 2018 2020 2010 20142012

Chandra

XMM-Newton

Swift

Suzaku

Integral

GLAST

(NeXT)

(XEUS)Con-X

(SIMBOL-X)

2004 20082006 2016 2018 2020 2010 20142012

Agile

NASA

ESA

JAXA

Europe

SRG/ROSITA/Lobster

HMXT

China

MIRAX

Brasil


eROSITAeROSITA

ART-XCART-XC

LobsterLobster

Sun direction

Rotation axis

30

Platform

Spectrum X-Gamma eRosita (X-ray mirror Telescope) Germany

LOBSTER (UK) wide field monitor

ART (IKI, Russia) Hard X-ray concentrator

GRB detector (IKI, Russia)


eRosita: history

~200,000 new X-ray sourcesDiffuse emission on all scales

ROSAT (1990 – 1998)

ABRIXAS (1999)

7 Wolter-Teles., 27 shells each

sharing 1 pn-CCD Camera

Rosita ISS (2000)

7 Wolter-Teles., 27 shells

7 pn-CCD Camera – Extension of RASS towards 10 keV

– Detection of obscured AGN


E

N

Proposal to NASA (SMEX, not accepted)

Wide Survey 6,000 deg2 (SDSS)~ 8,000 clusters of galaxies < z~ 0.7

Deep Survey 176 deg2

~ 1,800 clusters of galaxies < z ~ 1.2

DUO-Simulation 1 deg2

Rosita evolved into DUO (2004)

Constrain the equation of state of the dark energy and the dark matter density, and measure how they evolve with time in the local Universe, using clusters of galaxies as mass tracers

Cosmology comes in:

Luminous baryons give information about the distribution of Dark Matter,


– 7 Mirror Systems 35 cm (ABRIXAS 16 cm)

• 54 gold-coated nickel-shells

• PSF < 20 arcsec (goal 15 arcsec)

• Aeff ~ 2400 cm2 (1 keV, on-axis)

• Grasp 700 cm2 deg2 at 1 keV

– 7 individual cameras

• 256 × 256 pixel, 75µm

• 41 × 41 arcmin2 FoV

• framestore area

• energy range 0.2-12.0 keV

• energy resolution 130 eV at 6 keV

ABRIXAS

eROSITA

eRosita on SRG (2005)

Funds already in the DLR budget, expected by JuneMOU will be signed soon, Launch date, late 2010-2011.


eRosita: science goals Study the equation of state of DE with 100,000 Clusters• Numbers of Clusters as a function of redshift

• Cluster power spectrum on large scales: p(k)

• Baryonic acoustic oscillation in the cluster distribution (BAO)

Detect 1 Million Active Black Holes, many hiding behind obscuring gas and dust clouds

• All sky survey is a factor of 50 deeper than ROSAT (0.5-2 keV)

• A factor of 100 deeper than HEAO-1 (2-10 keV)

• Study coeval evolution of Black Holes and galaxies (BAO)

Study of accretion and acceleration processes in a large variety of galactic sources

• X-ray Binaries, Isolated Neutron Star, Cataclysmic variables

•Coronal Stars, embedded protostars, interstellar medium

•Supernova Remnants


Effective area [cm2] Grasp [cm2 deg2]

ART-XCART-XC

Grasp of 7 eROSITA telescopes is 3-4 x higher than 3 XMM-Newton telescopes in the energy range 0.3-2 keV!

At energies 5-15 keV, ART-XC is taking over significantly.

Effective Area & Grasp


Three surveys are planned in the eROSITA mission:

• All-Sky Survey: 42000 deg42000 deg22 in 1 year in 1 year

• Extragalactic Survey: 20000 deg 20000 deg22 in 2.5 years in 2.5 years

• Deep Survey: 200 deg200 deg22 in 1/2 year in 1/2 year

• Pointed Observations

Mission Concept


0.5-2 keV 2-10 keV

– a factor of 30 deeper than ROSAT (0.5-2 keV) – a factor of 100 deeper than HEAO-1 (2-10 keV)– expect ~ 100,000 clusters, – 3.4 Mio AGN (0.5-2 keV)– 250,000 AGN (2-10 keV) – and > 100,000 stars

Expect [450,120, 36, 10] AGN@z >[ 6, 7, 8, 9]

The eRosita survey


- Concentrator Kumakhov optics, polycapillary glass, diameter of capillaries ~1 m, capillaries ~2·1010

- Energy range 5-80 keV,

- FOV 465 keV - 2.880 keV

- Effective area of optics ~1150 cm2 30 keV

- Energy resolution 1 keV 60 keV ,

- Grasp 150 deg2*cm2 10 keV

ART-XC: an X-ray Concentrator

Faint spectroscopy at Hard X-raysObscured sources (AGN and more) Cosmic Hard X-ray BackgroundTi-44 line in SNR Hard spectra of Binaries


Sun sensor

StarTracker

Front Back

OpticModule

– Wide field X-ray monitor, 6 modules (60 MCP), FOV22.5162

– 0.1 - 4.0 keV (TBD)– Angular resolution 4 (FWHM)– Energy resolution E/E 20%– a grasp 104 cm2 deg2 at 1 keV– 0.15 mCrab for day

Consortium: UK (hardware) LU and MSSL, (science) Southampton. Finland U of Helsinki, Switzerland ISDC, Netherland SRON, Italy (GRBM), Spain?

Lobster: all the sky, all the time Monitor

4.000 Transients at 10-10 erg cm-2 s-1

36.000 at 10-11 erg cm-2 s-1

Daily Monitoring 400 AGN, typical timescalesCatalogue: 250.000 sources


Simbol-X

a focusing telescope for hard X–ray astrophysics

Courtesy of Philippe Ferrando

CEA/SAp & APC laboratory

0.5 – 80 keV

formation flight


Participating laboratories

Short history

F : CEA/Saclay, CESR/Toulouse, APC/Paris,LAOG/Grenoble, Obs.Paris/MeudonIt : (INAF :) O.A.Brera, Roma, Palermo, IASF Milano, Bologna D : MPE Garching, I.A.A.Tübingen, Obs. Bamberg of Erlangen-Nuremberg Uni

• End ‘01 : First ideas & discussions CEA/Saclay & O.A.Brera• End ‘03 : CNES call for scientific ideas using formation flight• Mid ‘04 : Selection of 4 missions for assesment phase (phase 0)• End ‘05 : Simbol-X recommended for phase A (alone)

End ’06: Completion of Phase A


A pointed telescope with the XMM angular resolution and sensitivity in the INTEGRAL/ISGRI energy range

30 degrees

Eventually focusing at Hard X-ray!

INTEGRAL, Coded Masks

30 arcmin

XMM, Focusing Optics


Major science goals

Particle acceleration

Mechanisms ?

Maximum energy ?

Accreting Black Holes

Physics in single objectsPhysics in single objects

Census in UniverseCensus in Universe


~50 % resolved in sources in the 7–10 keV band

Census of Super Massive Black Holes: where are the Obscured AGN ?

But less than a few % resolved beyond 10 keV

CXRB models : major contribution from obscured AGNs, but parametres are not constrained (evolution, energy cut-off, absorption) we need to resolve some of the 50% of the sources above 10 keV…


SIMBOL-X

Accretion physics in Super Massive B.H.

X-ray source

Accretion disc

« Secondary » components

Black Hole

G.R. effects

access to quiescence state, and follow and characterize the change of state (« ADAF » vs jets ? Difference between neutron stars and black holes ?)

V404 Cyg - Simbol–X 100 ks


With Simbol-X :• mapping of the synchrotron emission, • determination of spectral shape (and break) with X-ray alone • correlation with GeV and TeV emissions

SX SX


Acceleration: electrons in SNRs shocks

Simbol-X : E > 10 keV100 ks / 10x15 arcmin2

SN1006 XMM 2-4.5

keV

Spatially Resolved spectroscopy


other astrophysics topics…

Cyclotron lines

Non thermal cluster emission

Gamma-ray bursts follow up

Young Stellar Objects

Explosive nucleosynthesis yield

(Fusco-Femiano et al. 2000)

A2256/Beppo-SAX


Simbol-X scientific requirements

Large effective area, excellent angular resolution, very low background

Continuum sensitivity [1 Ms, 3 ] : 10-14 erg/cm2/s [20-40 keV] (1 μCrab)

Line sensitivity : 10-7 ph/cm2/s @ 68 keV


With very long focal length possible thanks to formation flight

The only way to go : focusing

Emax 1/θ Focal Length

20 to 30 m

Low energy detector (450 mm Silicon)

High energy detector (2 mm Cd(Zn)Te)

Active anticoincidence shield


NeXT mission NeXT mission (2012~)(2012~)

12m F. L. (HXT)

9m F. L. (SXT)

Hard X-rayTelescopes

(2 sets)

EOB

Hard X-ray Imaging+

High resolutionspectroscopy

Soft X-rayTelescopes

(2 sets)Energy

Soft X-rayImaging(1 set)

SXI

Soft γ-raydetector

SGD

Hard X-rayImaging(2 sets)

HXI

300keV0.3keV 3keV 30keV

High ResolutionSpectrometer

(He dewar)

SXS

Slide from T. Takahashi, 2006


Overview of BHFP-EXIST Science and Design

Hard X-ray (~3-600 keV) all-sky imagingHard X-ray (~3-600 keV) all-sky imaging

Mission DesignMission Design parameters:parameters:•Extend ROSAT sens. (~5 x 10-13cgs) to 3-150 keV with 0.9-5’ resolution & ~10” positions•Two wide-field coded aperture telescopes: 10-600 keV (6m2 CZT) & 3-30 keV (1m2 Si)

http://EXIST.gsfc.nasa.gov

e.g., EXIST measures Cen-A every orbit: characteristic time variability (QPOs) constrain BH mass

High Energy

Telescope

HET (10-600keV)

(6 x 3 coded aperture telescopes;131o x 65o FoV)

Low Energy Telescope

LET (3-30 keV)

(4 arrays of 7 x 1 coded aperture telescopes;116o x 64o FoV)

IMDC designDec. 2004

Slides from J. Grindlay


MIRAX a Brazilian satellite

SXIHXI(2)

APS star camera

Status Approved mission, phase A running, Launch 2011 (?) by Brazilian VLS

Instrument parameters

Hard X-ray Imager (HXI)

Soft X-ray Imager (SXI)

Energy range 10-200 keV 2-28 keV

Angular Res. 7 arcmin 5 arcmin

Localization < 1 arcmin (10) < 1 arcmin (10)

Field-of-view 58o x 26o FWHM 20o x 20o FWHM

Sensitivity < 2.2 mCrab (1 day, 5 ) < 5 mCrab (1 day, 5 )


MIRAX SCIENCEContinuous broadband imaging spectroscopy of a large source sample (~9 months/yr)

• Complete history of transient sources

• X-ray bursts – superburst recurrence times and emergence of normal bursts

after superbursts

• Spectral state transitions and evolution on accreting compact objects

• Accretion torques on neutron stars

accreting pulsars, pulsed period evolution, ms-pulsar recurrent outbursts

• Relativistic jets on microquasars and other systems

X-ray light curves during radio ejections

• Flaring X-ray sources and fast transients (many INTEGRAL sources)

• Gamma-ray bursts (~1/month), especially XRFs

simultaneous X-ray AGs

• AGN variability (obscured AGNs)


HXMT

China's First X-ray Astronomy Satellite: Hard X-ray Modulation Telescope Mission


Before 2010, there is no other space astronomy mission approved internationally to have the capabilities of HXMT

Angular Resolution 15’ < 5’ 14’

Source Location 2’ < 1’ 3’

Sensitivity (10^-7 / cm^2 s keV) 10 3 30 Observation Mode

All sky survey no yes yes

Selected sky deep survey yes yes no

Narrow field pointing observation no yes no

Integral HXMT Swift


Conclusions• The next decade will possibly be again a golden age in X-ray

astronomy with many observatories in orbit

• The main goals appears to be – A very deep survey of the soft-medium X-ray Universe for

cosmology and astrophysics (eRosita)– A survey of the Hard sky (HXMT, EXIST)– The imaging of the Hard X-ray sky with soft-like sensitivity

(Simbol X, NEXT)– Broad Band spectra / Timing studies (Spectrum X-Gamma,

Simbol X, NEXT, MIRAX)– A deep “all sky all time” monitoring in the soft (Lobster,

MAXI), medium-hard (Exist) , time variability of Binaries, AGN

– Deep Study (Simbol X) and continous monitoring (MIRAX) of our Galaxy


Conclusions• These observatories will provide a perfect

complement at soft-medium-hard X-ray to TeV Observations

– Constraining SED in the broad X-ray band (… and therefore models!)

– Providing detailed morphology in the broad X-ray band – Providing spatially resolved spectroscopy in the broad X-

ray band – Allowing a continuous time monitoring of e.g. Blazars

• To seek the collaborative support of the High Energy Astrophysics community at large for CTA is mandatory

• As it is mandatory to shape CTA as an observatory, which is always the best way to maximize any scientific output…


Simbol X the Movie


Mission parameters for the newest configuration

Parameters EXIST HET EXIST LET

Energy 10 – 600 keV 4 - 30 keV

Modules 8+5+8=19 6+10+10+6=32

Mask (W) 5mm thick, 2.5 mm pix 0.05mm thick, 0.2mm pix.

Detector (CZT) 5 mm thick, 1.25mm pix 1mm thick, 0.16 mm strip.

Det. Area (Mod./Tot.) 56x56 cm2 /5.96 m2 20x20cm2/ 1.28 m2

F.C. FoV (Mod./Tot.) 21º x21º / 65º x 154º 16º x16º / (32º64º) x 160º

Ang. Res./5σ Loc. 5.7/ 1.2 0.95/ 11

Mask-Det. Sep. 1.5 m 0.72 m

Temporal Res. < 1 ms < 1 ms

ShieldsCsI/passive side,

CsI rear shieldsPassive

Sensitivity

(5σ)

0.05mCrab (<150 keV, ~1yr)

0.5mCrab (>150 keV, ~1yr)0.05mCrab


X-ray Clusters for Precision Cosmology: six good reasons

1. Cluster mass function mainly depends on the matter density m and the amplitude of the primordial power spectrum 8

2. Evolution of mass function N(z) gives sensitive constraints on DM and DE

3. Cluster Power Spectrum amplitude and shape depend on DM and DE

4. Baryonic Wiggles due to acoustic oscillations at recombination give tight constraints on space curvature

5. Cluster baryon fraction as a function of redshift provides constraints on DM and DE

6. Clusters provide direct distance measurements due to combined X-ray and SZ-measurements

Courtesy of G. Hasinger (2006)


– Launch in the 2010-2011 timeframe by Soyuz-2 – Two launch options, 600 km circular orbit:

Baikonur – inclination 30 as baselineKourou – inclination 5 as option

– Medium size spacecraft:Navigator (Lavochkin, under development, baseline)Yamal (Energia, several similar S/C in operation)

– Payload:eROSITA (Germany), X-ray mirror telescopes

Lobster (UK), wide field X-ray monitor

ART (IKI, Russia), X-ray concentrator based on Kumakhov optics

GRB (IKI, Russia), gamma ray burst detector

The new Spectrum-X-Gamma Mission

andrea santangelo, iaat paris 1.03, 2007towards a cta fp7 design study the kev – tev connection...

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