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The cooling-flow problem

Sersic 159-03 EPIC Radial Profiles. Abel 1835 RGS Spectra. The cooling-flow problem. Bremsstrahlung emission ) L / n 2 ) center parts cool faster. Pressure equilibrium ) mass in-flow ) density increases.

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The cooling-flow problem

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  1. Sersic 159-03 EPIC Radial Profiles Abel 1835 RGS Spectra The cooling-flow problem Bremsstrahlung emission )L/n2) center parts cool faster. Pressure equilibrium ) mass in-flow ) density increases. Mariano Mendez - SRON

  2. 500£500 2-eV resolution spectrum of the nucleus of a cluster of galaxies with XEUS. The cooling-flow problem Heating 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. Instrument requirements: - FoV = As large as possible (goal 10£ 10). Mosaic observations. - DE = 2 eV (v¼ few 100 km/s) -E range = 0.3 – 12 keV (0.3 keV to reach up to z¼ 0.05) Mariano Mendez - SRON

  3. Simulations of structure formation Missing baryons at z ¼ 0 Wbaryon; WMAP = 0.0440 Wbarion; observed = 0.0124 Mass Temperature OVII Warm-hot intergalactic medium (WHIM) Mariano Mendez - SRON

  4. XMM-Newton: Soft excess emission in Cl. of Galaxies. Possible infalling groups. XEUS: Simulated observation for 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) Warm-hot intergalactic medium (WHIM) Properties of the emitting gas: kT¼ 0.2 keV [O] ¼ 0.1 [O¯] Mass ¼ MassCl. of Galaxies Mariano Mendez - SRON

  5. 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. - DE = 2 eV (weak narrow lines) -E range = 0.1 – 2 keV (0.1 keV ! N up to z¼ 0.5 and O up to z¼ 2) Mariano Mendez - SRON

  6. Active Galactic Nuclei Mildly-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

  7. NGC 5548 - 100-s with XEUS Active Galactic Nuclei Time-resolved spectroscopy of Seyfert 1 galaxies with sufficient spectral resolution to determine outflow velocities down to a few 100 km/s. Instrument requirements: - Effective area (»100-s time-scale variability) - DE = 2 eV (v¼ few 100 km/s) -E range = 0.3 – 12 keV (constrain continuum / Fe line at ¼ 6.5 keV) Changes in the plasma parameters related to changes in the X-ray luminosity provide information about the location of the absorbing plasma. Mariano Mendez - SRON

  8. 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, r& 10 £rnuclear. Possible exotic particles, like strangeness-bearing baryons, pions and kaon condensates, or deconfined quarks. Only possibility, since the Big Bang, to find those particles in nature. Mariano Mendez - SRON

  9. OVII xy FeXXVI Ha (z = 0.35) OVIII Lya (z = 0.35) OVII xy OVII Edge OVIII Lya NVII Lya NVII Lyb FeXXV 2-3 (z = 0.35) OVII Kb CVI Lyb OVII Kg Ne IX w NVI Kb NVI Kg NVI w CVI Lyd CVI Lyg OVII w Neutron star equation of state Composition of NS from Mass-Radius measurements – Possible Quark stars – Physics of nuclear interactions z = 0.35 Mariano Mendez - SRON

  10. 30-second exposures of the early part of a single X-ray burst, for 3 different spin frequencies of the neutron star. Neutron star equation of state Composition of NS from Mass-Radius measurements – Possible Quark stars – Physics of nuclear interactions Instrument requirements: - Effective area!!! - DE = 2 eV (to measure line width) -E range = 0.3 – 2 keV (»10 keV ! redshifted Fe XXVI Lya) Redshift !M/R Line width !M/R2 Mariano Mendez - SRON

  11. Doppler maps Life cycle of the elements SNe and SNR. Explosive nucleosynthesis. Cas A – 1 Ms with Chandra Mariano Mendez - SRON

  12. XMM-Newton XEUS Life cycle of the elements Rare elements – ISM enrichment Instrument requirements: - Detector uniformity/stability. FoV less important - DE = 2 eV (shock dynamics) -E range = 0.3 (to include C-K edge) to »10 keV (Fe-K edge) Mariano Mendez - SRON

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