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--- ondesgravitationnelles [2023/03/02 17:17] – daniele.steer
+++ ondesgravitationnelles [2023/03/08 15:08] (current) – daniele.steer
@@ Line 20: / Line 20: @@
         * developments to higher PN, with spins and tidal effects, all needed for future detectors especially LISA. Computation of both conservative equations of motion plus effects of gravitational radiation reaction. Computation of waveforms (modes, especially the dominant quadrupole mode 22) and flux balance equations for secular evolution of the binary.
         * Inclusion of eccentricity to higher PN, unbound hyperbolic orbits etc. Relation between unbound and bound (elliptical) orbits including tail effects.
-        * Effective Field theory techniques, amplitudes. These, together with ``classical'' PN approach, will probably develop together. Develop dictionary between the two approaches. [e.g. Asymptotic symmetries: synergy between these symmetries at null infinity and the waveform. Important for non-linear- and spin- memory effects + tails. ]
+        * Effective Field theory techniques, amplitudes. These, together with ``classical'' PN approach, will probably develop together. Develop dictionary between the two approaches. [e.g. Analysis of asymptotic symmetries: synergy between these symmetries at null infinity and the waveform. Important for non-linear- and spin- memory effects + tails. ]
         * Effective one body: under-developed in France, but crucial to match inspiral to ringdown waveforms and for practical implementation of data analysis.
         * Numerical relativity. Tremendous progress over the last decades. A field which is under-developed in France. Connection with the community working of neutron star equations of state.
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 **Astrophysics, Cosmology with GWs (and other messengers)**
+In the next decade the number of GW events which will be detected will rapidly increase.
+  * O4 2023-2025 -- order 1000-10^4 BBH and BNS
+  * O5 2026-2028 -- 10^5 BBH or more
+  * O6? 2030-2032 -- 10^6 BBH or more.
+With this data, it should be possible to determine, amongst other things, the population of BH in the local universe (mass and redshift distribution), as well as test GR in the strong field regime to high precision.
+Regarding Astrophysics and Cosmology:
   * Using individual sources to measure the Hubble constant and other cosmological parameters (e.g. equation of state of DE), see [[cosmologie|cosmologie]]. Unless there are many GW events with EM counterparts, this goes necessarily hand in hand with astrophysics (Galaxy surveys, cross correlation with LSS, mass distribution of black holes...)
   * probing anisotropic expansion or the cosmological principle with GW data