mariano mendez - sron the cooling-flow problem bremsstrahlung emission ) l / n 2 ) center parts cool...
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Mariano Mendez - SRON
The cooling-flow problemBremsstrahlung emission ) L / n2 ) center parts cool faster.Pressure equilibrium ) mass in-flow ) density increases.
Sersic 159-03EPIC Radial Profiles
Abel 1835RGS Spectra
Mariano Mendez - SRON
The cooling-flow problemHeating mechanism: Magnetic reconnection? Central AGN? Turbulence?Spatially-resolved, high-resolution spectra to map out the temperature distribution and the dynamics of the gas in the center.
500£500 2-eV resolution spectrum of the nucleus of a cluster of galaxies with XEUS.
Instrument requirements: FoV = As large as possible (goal 10 £ 10). Mosaic observations.
E = 2 eV (v ¼ few 100 km/s) E range= 0.3 – 12 keV (0.3 keV to reach up to z ¼ 0.05)
Mariano Mendez - SRON
Warm-hot intergalactic medium (WHIM)
Missing baryons at z ¼ 0
baryon; WMAP = 0.0440barion; observed = 0.0124
Mass Temperature
OVII
Simulations of structure formation
Mariano Mendez - SRON
Warm-hot intergalactic medium (WHIM)XMM-Newton: Soft excessemission in Cl. of Galaxies.Possible infalling groups.
Properties of the emitting gas:
kT ¼ 0.2 keV
[O] ¼ 0.1 [O¯]
Mass ¼ MassCl. of Galaxies
XEUS: Simulated observationfor A 2052.
Other lines: CVI, NVII, OVIII and the Fe-L complex. Abundance up to z ¼ 0.5 (after that, problems with background lines)
Mariano Mendez - SRON
Warm-hot intergalactic medium (WHIM)WHIM can also be detected in absorption to higher redshifts, provided enough bright background sources exist.
Instrument requirements:FoV = Not a driver. Snapshots of outskirts of Clusters or bright
background sources.E = 2 eV (weak narrow lines) E range= 0.1 – 2 keV (0.1 keV ! N up to z ¼ 0.5 and O up to z ¼
2)
Mariano Mendez - SRON
Active Galactic NucleiMildly-ionized material in the vicinity of an AGN (warm absorber)
- Broadened lines ! vturbulent & 600 km/sec- Outflow velocity = 200 km/sec- Two photo-ionisation components
Mariano Mendez - SRON
Active Galactic NucleiTime-resolved spectroscopy of Seyfert 1 galaxies with sufficient spectral resolution to determine outflow velocities down to a few 100 km/s.
Changes in the plasma parameters related to changes in the X-ray luminosity provide information about the location of the absorbing plasma.
NGC 5548 - 100-s with XEUS
Instrument requirements:Effective area (»100-s time-scale variability)E = 2 eV (v ¼ few 100 km/s) E range= 0.3 – 12 keV (constrain continuum / Fe line at ¼ 6.5 keV)
Mariano Mendez - SRON
Extreme gravity and NS equation of state Close to NS or black holes, gravitational energy is comparable to rest-mass energy. This regime has so far not been tested.
Inside NS, & 10 £ nuclear. Possible exotic particles, like strangeness-bearingbaryons, pions and kaon condensates, or deconfined quarks.
Only possibility, since the Big Bang, to find those particles in nature.
Suppermassive BH
Solar-mass BH
Intermediate-mass BH
Galactic rotationStrong lensing/
Shapiro DelayDeflection of light/
Terrestrial LabsGravity Probe B
Hulse-Taylor Pulsar
Neutron starredshifted linesand QPOs
Black Hole QPOs
Precession of Mercury
Microlensing
/
Mariano Mendez - SRON
Neutron star equation of state Composition of NS from Mass-Radius measurements – Possible Quark stars – Physics of nuclear interactions
OV
II x
y
OV
II E
dge
OV
II K
OV
II K
O
VII
I L
y
Ne
IX w
NV
II L
y
OV
II w O
VII
xy
NV
I K
NV
II L
yN
VI
K
CV
I L
yC
VI
Ly
CV
I L
yN
VI
w
FeX
XV
23
(z
0.3
5)
FeX
XV
I H
(
z
0.3
5)
OV
III
Ly
(z
0.3
5)
z 0.35
Mariano Mendez - SRON
Redshift ! M/RLine width ! M/R2
30-second exposures of the early part of a single X-ray burst, for 3 different spin frequencies of the neutron star.
R (km)
L
0 5 10 15 20
1
2
0
. oM
(M
)
Quark
KC
APR98
AFPS
AUM
Neutron star equation of state Composition of NS from Mass-Radius measurements – Possible Quark stars – Physics of nuclear interactions
Instrument requirements:Effective area!!!E = 2 eV (to measure line width) E range= 0.3 – 2 keV (»10 keV ! redshifted Fe XXVI Ly)
Mariano Mendez - SRON
Life cycle of the elements SNe and SNR. Explosive nucleosynthesis.
Cas A – 1 Ms with Chandra
Doppler maps
Mariano Mendez - SRON
Life cycle of the elements
XMM-Newton
XEUS
Rare elements – ISM enrichment
Instrument requirements:Detector uniformity/stability. FoV less importantE = 2 eV (shock dynamics) E range= 0.3 (to include C-K edge) to »10 keV (Fe-K edge)