x. barcons, xeus sagxeus: physics of the hot evolving universe xeus: the physics of the hot evolving...

X. Barcons, XEUS SAG XEUS: Physics of the hot evolving Universe

XEUS: The Physics of the hot Evolving Universe

Xavier Barcons


Index

• The Science Case for a “Next Generation X-ray Observatory”

• The (current) XEUS mission scenario

• Implementation: towards a global mission


Acknowledgements

• The XEUS Science Advisory Group: Monique Arnaud, Johan Bleeker, Günther Hasinger, Hajime Inoue, Giorgio Palumbo, Arvind Parmar and Martin Turner.

• The XEUS Astrophysics Working Group, especially Didier Barret

• The XEUS Instrument Working Group, especially Dave Lumb

• The XEUS Telescope Working Group, especially Marcos Bavdaz

XEUS: Physics of the hot evolving UniverseX. Barcons, XEUS SAG

Physics of the hot evolving Universe• Probing matter under extreme conditions

• The origin and growth of the first massive black holes in the early Universe

• The formation of the first gravitationally bound, dark matter dominated systems, i.e. small groups of galaxies and their evolution

• The characterisation of the true intergalactic medium, containing ½ of the baryonic matter in the Universe

• The origin and cosmic evolution of the chemical elements in the Universe


Relativistically broadened Fe reflection lines in AGN

MCG-6-30-15


Relativistic Fe line broadening

Schwarzschild

Kerr

Fabian et al 91


Measuring the spin of the Black Hole


NASA

Approaching the Black Hole

Light-bending effects Chris Reynolds

ASCA relativistic Fe-line(Tanaka et al. 1995)

Simulation of precessing binary accretion disks in 3C273 with XEUS (Torres et al., 2004)

Wilms et al 2001


General Relativity frequencies in Quasi-Periodic Oscillations

Very large collecting area neededD. Barret


XMM-Newton detection of the gravitationalredshift in the surface of a neutron star

Constraining the equation of state in neutron stars (now)

z

z z


Constraining the equation of state in neutron stars (the future)


The formation of the first supermassive Black Holes

• Current theories predict that the first massive black holes formed at redshifts of ~5-10 with masses of 106-7 Mo, corresponding to X-ray luminosities of 1043-44 erg s-1.

• Furthest known massive black holes (QSOs) are at z = 6.5. Claimed galaxy at z = 10.

• A prime goal of XEUS is to study the evolution of the early universe using Active Galactic Nuclei (AGN) as probes.


Lockman Hole800 ks XMM-Newton observation

XEUS will be able to determine redshifts and study Fe lines individually

Average rest-frame spectra show relativistic Fe-lines

type-1 AGNEW~700eV

Streblyanskaya et al., 2004

type-2 AGNEW~500eV


XEUS: The first accreting BHs

z=3.0 z=5.0

z=7.0 z=10.0


NGC 6240

Binary BH mergers - efficient accretion

NASA/CXC/Komossa

Biggest problem: how to funnel down large amount of gas over a galactic scale on a very short timescales

Observations tell us, that gas-rich mergers can do the

trick.

Binary Black Holes expected in powerful obscured quasars.

XEUS needed!


Clusters of Galaxies:Largest Objects in the

Universe

courtesy V. Springel MPA


XEUS – The first groups and clusters• XEUS will detect and study the first and most

distant groups of galaxies formed in the Universe, precursors of today’s massive clusters.

Credit: H. Böhringer


Dark Matter (23%) X-ray Gas (4%)

The missing baryons

Warm/hot intergalactic medium (WHIM) in absorption

QSO or GRB line of sight

Cen&Ostriker 1999


Elements formed at z>1.3!

Abundance independent of z

Hashimoto et al, ‘04

Best X-ray spectrum of a z>1 cluster

kT~5 keVXMM 800 ks

First clusters: creation of chemical elements


XEUS – Key ParametersParameter Specification

Energy Range 0.05 – 80 keV

Telescope focal length 50 m

Mirror area @ 1 keV 10 m2

Mirror area @ 8 keV 3 m2

Fields of view 15’ (WFI) 1’ (NFI)

Energy resolution @ 1 keV 50 eV (WFI) 2 (1) eV (NFI)

Energy resolution @ 8 keV 100 eV (WFI) 5 (2) eV (NFI)


Mission concept

• 2 Spacecraft in flight formation:– Mirror S/C (MSC)– Detector S/C (DSC),

icnluding active alignement systems

• Operations at L2• DSC can be replaced

with updated instruments


The mirror technology – the big challenge


The pore optics concept

Bavdaz et al(2004)


Stacking of Si ribbed plates

Beijersbergen et al 2004


Building the X-ray telescope and MSC

Bavdaz et al 04


MSC concept


Mirror effective area

Lumb et al 04


Comparison of X-ray mirror technologies


XEUS instruments

• Narrow Field Instrument 1 (Superconducting Tunnelling Junction):– FOV:0.5-1’– 0.05-3 keV– Spectral res: 1 eV @ 1 keV

• Narrow Field Instrument 2 (Transition Edge Spectrometer)– FOV: 0.5-1’– 2-15 keV– Spectral res: 3 eV @ 6keV

• WFI (Wide-field imager):– CCD/DEPFET (5’)– Conventional CCDs (15’)– High-energy detector– High count rate detector– Polarimetry?


Implementing the mission

• ESA/JAXA collaboration since 1996• Technically ready for launch in 2015, if

development continues• Proposed to ESA’s “Cosmic Vision 2015”

exercise, to implement the theme “The violent evolving Universe”

• Constructive talk with the USA towards a single global ESA/NASA/JAXA mission.

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