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Joint discussion on scientific requirements

Joint discussion on scientific requirements. WHIM in emission emission properties highly dependant on modeling. Low density or even median overdensity emission would be difficult to measure. Emission measurements mostly give info on high overdensity.

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Joint discussion on scientific requirements

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  1. Joint discussion on scientific requirements • WHIM in emission • emission properties highly dependant on modeling. Low density or even median overdensity emission would be difficult to measure. Emission measurements mostly give info on high overdensity. • resolution better than 4 eV to resolve lines, (temperature and ionization stage diagnostics) • 2 eV goal to disentangle WHIM from foreground and allows detection of weaker lines (lower overdensity) • Need at least 1000cm2 • fov around 20’ • Work in progress: check (M.Galeazzi) using newer (Borgani et al) simulations • Go beyond the simple collisional equilibrium approx • Local emission (E. Branchini)

  2. WHIM in absorption • low density sampled with absorption lines. Going to higher z (vs the bright agn sample) with GRB increases the chances to have more filaments, and allow complementary measurements of the same filament in absorption and emission when the afterglow dies away. • Need resolution better than 2 eV: combined with area (1000 cm2), wide field GRB monitor and fast response build up a sample of about 100 los in 3 years. This is important to put a constraint on Omega B at the level of few percent (Fiore). • Energy resolution: Goal <1eV to allow kinematics test (comparison with temperature braodening: test models)

  3. Cluster cores and soft excess • Requirements as for WHIM in emission • Cluster outer regions • Large FOV 1 degree goal, requirement 30-40’ • Large Eff. Areas >1000 cm2 • Low Instrumental bkg and Low CXB : Spatial resolution around 5-10” needed to subtract from the bgk discrete sources. Can we achieve a comparable result selecting narrow line emission ? Is it possible to use triplets to get density estimation? : Fiore, Molendi) • High. Res. Spectroscopy: metal abundances in the outer part: Iron complex at low energy, Si, Mg, kinematics

  4. Cluster (continued): • For the continuum temperature need to go up to at least 3-4 keV. Spectroscopy of Fe complex @ 6-7 kev mostly useful for kinematics • - Absorption studies using GRB through cluster/supercluster medium. What is the probability ? What is the EW through a cluster, (S. Molendi)

  5. Can we constrain dark matter origin ? • From WHIM: Through distribution of filaments ? Need too many • Through cluster survey (but uncertainties in the mass estimate of the cluster. Need high spatial resolution for faint distant clusters). C.f.r. Rosita performances (Molendi) • Direct X-ray signatures (Colafrancesco) • Dark energy • GRB Hubble diagram ? (need spectrum up to 500 keV- 1MeV: Amati)

  6. Converging towards a joint mission concept • Core mission (WHIM driven): • Telescope with A>1000cm2 with fov 30-60’ • Microcalorimeter TES as focal plane to cover the FOV (possibility of smaller pixels in the central part to increase the spatial resolution) • Energy extension from 0.1 to 2 keV • Fast slewing and WFM for transient localization • Additional benefit: science on clusters + GRB & transients, brings in a very wide community • Options to be studied : TES in the central part, ccd in the outer part (or two telescopes) • Trade off on focal lenght and/or multilayer coating for higher energies(cluster continuum temperature, Iron line, polarimeter)

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