Outline made by GN and Sterl Phyinney years ago for planned LRR

====== Galactic LISA science ======

  - Abstract
  - General properties of stellar binaries that make LISA sources
    - orbital periods 3mins-hour. -> not main sequence. Must involve spiral-in (in Galaxy) or capture (dense clusters)
    - Ultra compact binaries:  white dwarf, neutron star, black hole
  - Verification binaries -guaranteed LISA calibration sources
    - Known sources.
    - Observational plans that could lead to more known sources.
  - Order of magnitude estimates of disk/bulge populations, and identificationof what these are sensitive to:
     - White dwarf binaries:
        - double spiral-in, double-degenerate channel(cf central binaries in planetary nebulae, CVs as evidence for spiral-in). 1-2.5Msun progenitors, initial separation=red giant-AGB star radii.
        - single-degenerate, `Tutukov/Podsiadlowski' channel
        - Sensitivity to spiral-in physics/parameters.  Observational and theoretical constraints.
        - Detached and semi-detached (AM CVn) systems. -Sensitivity to tides/transfer stability.
     - Neutron star binaries
        - Double spiral-in.  >10Msun progenitors.
        - Sensitivity to spiral-in physics/parameters and NS natal kicks.
     - Black hole binaries
     - The universal dN/df ~ f^{-11/3} frequency spectrum for GW inspiral sources.
  - LISA measurements/quick overview of data analysis
     - Source f, fdot, fddot position determination precision
     - Source confusion -3mHz and individual sources > vs background+spikes <
     - Mock data challenge results demonstrating feasibility.
     - What do GW add to EM observations
         - Completeness -no extinction, no selection, whole galaxy. Populations!
         - Polarisations -> orbit inclinations (may check 1 or 2 nearby cases with SIM-like interferometers -otherwise big help on mass determinations for EM id's), position angles.
         - If pure 2 point mass systems, f, fdot -> chirp mass; fddot -> mass ratio and hence M1, M2
     - Joint EM-GW data
  - Gravitational wave signal
     - Pure 2 point mass GW (f, fdot -> distance -> galactic structure.
     - vs tides (no distance
         - Tidal effects on fdot, fddot.
         - Tidal heating -electromagnetic consequences (deep-none; shallow-bright)
     - mass transfer (no distance, but
         - RXJ0806 wrong fdot sign... -confusion -can't tell pure 2 point mass from mass transfer from GW alone. Need GW+EM.
  - Detailed population synthesis estimates and observational constraints for disk/bulge populations:
      - White dwarf binaries I: double white dwarfs
        - Formation, population estimates (obs. & theory)
        - Uncertainties
        - LISA science: foreground (#, masses) indiv. sources (#, parameters), distribution, tidal interaction
      - White dwarfs binaries II: AM CVn stars
        - Formation, population estimates (obs. & theory)
        - Uncertainties
        - LISA science: #, parameters, distribution, mass transfer stability
      - Neutron star binaries (inc. UCXBs)
        - Types, formation, population estimates (obs & theory)
        - Uncertainties
        - LISA science: #, eccentricities, kicks, progenitor masses?
      - Black hole binaries
        - Types, formation, population estimates (theory)
        - Uncertainties
        - LISA science: existence, numbers, kicks, progenitor masses?
      - Others: CVs, WD+Mstar, W UMa's, sdB binaries
  - Formation processes in dense stellar clusters
     - Tidal capture (UCXBs)
     - Exchange
     - Other (collision, gw capture...)
     - Galactic Center (brown dwarfs EMRIs -cf Freitag)
  - Galactic sources that are not binaries
    - Strongly magnetised rapidly spinning WDs
  - Galactic structure
    - Components: discs(s), spiral arms, bulge, Halo, Galactic center(?)
    - LISA science: tracing mass distribution, (Halo) binary fraction, IMF and star formation history , globular clusters, open clusters(?)
  - Extra-galactic sources
    - Discrete sources (LMC, SMC, M31, M87...)
    - Cosmological background
    - LISA science...
    - Connections to BBO/Decigo rates
  - Connecting LISA and LIGO/VIRGO
    - Possibilities, sources
    - Combined science
  - Summary for each source category, of
    - unique LISA science (cf 5)
    - convolved LISA science (e.g. populations+synthesis trace bulge/disk, binary fractions, IMF, star formation history)
    - Joint EM-GW science (e.g. inclinations, tidal heating)
  - Conclusions and outlook