D. Choi (KISTI):
In the first lecture, my intention is to give a general overview of the binary black hole merger simulations. I will start with motivation, and highlight some recent results. Then, I will turn to a rough overview of the technical aspects of the simulations. I will also try to illustrate basic concepts of numerical analysis using model equation.
In the second lecture, I will focus on an important application of BBH merger simulations: calculation of recoil kicks and its impact on astrophysics community. If time allows, I will touch on non-GW application of BBH simulations.

G. Faye (IAP):
In this series of four lectures, we propose to show how the post-Newtonian perturbative approach allows one to investigate the near and far zone dynamics of isolated systems. We shall first introduce a convenient description for the waveform in terms of two sets of radiative multipole moments. Their calculation will be explained in the context of the Blanchet-Damour post-Minkowkian multipole algorithm: it consists, starting from a linear vacuum solution parameterised by some additional "source" moments, in deriving the non-linear corrections of the gravitational field by solving iteratively the Einstein equations that have been truncated at the appropriate post-Minkowskian order; the explicit expression of the source moments is found by matching the exterior field with the metric computed in the near zone by means of a post-Newtonian iteration. Next, we shall present two alternative approaches to obtain the equations of motions of the isolated system. The first one uses the conservation of the stress energy tensor, whereas the second approach is based on the ADM Hamiltonian scheme. The Hamiltonian formulation has numerous practical applications, including the
effective-one-body resummation of the two point-mass dynamics.

G. Gonzalez (LIGO Scientific Collaboration & LSU):
Lectures on "Detection of Gravitational Waves"
These lectures will give a brief overview of the goals, status, and future prospects of the effort on detection of gravitational waves with ground-based interferometric detectors.
Lecture I : "Astrophysical sources of gravitational waves and expected signals"
Reference: "AN OVERVIEW OF GRAVITATIONAL-WAVE SOURCES", Cutler C., Thorne, K, GR16 Proceedings, Bishop N., Maharaj, S, eds., World Scientific, 2002, Arxiv preprint gr-qc/0204090
Lecture II: "Interferometric gravitational wave detectors: present and future"
Latest progress talks: http://gwdaw12.mit.edu/program.html
Lecture III: "Results from current LSC searches for gravitational waves"
References: www.ligo.org --> Observational Results

E. Gourgoulhon (LUTH):
LECTURE 1: 3+1 formalism of general relativity
1. 3+1 foliation of spacetime
2. 3+1 decomposition of Einstein equation
3. The Cauchy problem
4. Conformal decomposition
LECTURE 2: The initial data problem for 3+1 numerical relativity (1/2)
1. The initial data problem
2. Conformal transverse-traceless method
3. Conformal thin sandwich method
LECTURE 3: The initial data problem for 3+1 numerical relativity (2/2)
1. Helical symmetry for binary systems
2. Initial data for orbiting binary black holes
3. Initial data for orbiting binary neutron stars and BH/NS systems
LECTURE 4: Trapping horizon approach to black holes
1. Local approaches to black holes
2. Viscous fluid analogy
3. Angular momentum and area evolution laws
4. Applications to numerical relativity
Suggested references:
Lectures 1 to 3 :
[1]. M. Alcubierre : "Introduction to 3+1 Numerical Relativity", Oxford University Press (2008) http://www.oup.com/uk/catalogue/?ci=9780199205677
[2]. R. Bartnik and J. Isenberg : "The Constraint Equations", in "The Einstein Equations and the Large Scale Behavior of Gravitational Fields --- 50 years of the Cauchy Problem in General Relativity", edited by P.T. Chrusciel and H. Friedrich, Birkhauser Verlag, Basel (2004), p.~1.
[3]. T.W. Baumgarte and S.L. Shapiro : "Numerical relativity and compact binaries", Phys. Rep. 376, 41 (2003).
[4]. G.B. Cook : "Initial data for numerical relativity", Living Rev. Relativity 3, 5 (2000) http://www.livingreviews.org/lrr-2000-5
[5]. E. Gourgoulhon: "3+1 Formalism and Bases of Numerical Relativity", Lectures given at the General Relativity Trimester held in the Institute Henri Poincare (Paris, Sept.-Dec. 2006) http://arxiv.org/abs/gr-qc/0703035
[6]. E. Gourgoulhon : "Construction of initial data for 3+1 numerical relativity", Journal of Physics : Conference Series 91, 012001 (2007) http://arxiv.org/abs/0704.0149
[7]. H.P. Pfeiffer : "The initial value problem in numerical relativity", in "Proceedings Miami Waves Conference 2004" http://arxiv.org/abs/gr-qc/0412002
[8]. J.W. York : "Kinematics and dynamics of general relativity", in "Sources of Gravitational Radiation", edited by L.L. Smarr, Cambridge University Press, Cambridge (1979), p.~83.
Lecture 4 :
[9]. A. Ashtekar and B. Krishnan : "Isolated and dynamical horizons and their applications", Living Rev. Relativity 7, 10 (2004) http://www.livingreviews.org/lrr-2004-10
[10]. I. Booth : "Black hole boundaries", Canadian J. Phys. 83, 1073 (2005) http://arxiv.org/abs/gr-qc/0508107
[11]. E. Gourgoulhon and J.L. Jaramillo : "A 3+1 perspective on null hypersurfaces and isolated horizons", Phys. Rep. 423, 159 (2006)
[12]. E. Gourgoulhon and J. L. Jaramillo : "New theoretical approaches to black holes", New Astronomy Reviews 51, 791 (2008) http://arxiv.org/abs/0803.2944
[13]. B. Krishnan : "Fundamental properties and applications of quasi-local black hole horizons", to appear in the Proceedings of the 18th International Conference on General Relativity and Gravitation (Sidney, Australia, 8-13 July 2007) http://arxiv.org/abs/0712.1575

M. Shibata (Tokyo U.):
In the first two lectures, I focus on reviewing the astrophysical sources of gravitational waves. First, I will summarize scenarios for evolution of binary neutron stars and black hole neutron star binary. In particular, details about hydrodynamical properties and elementary processes which could play an important role in the merger phase will be explained. Then, I will review on the current scenario for gravitational collapse of massive stars and subsequent supernova explosion. Elementary processes which play an important role will be explained.
In the third lecture, hydrodynamic equations are summarized. Not only the Euler and continuity equations but also MHD equations and equations to be solved when the microphysical processes are taken into account are briefly reviewed. Numerical method for solving standard hydro equations will be reviewed by Luca Baiotti in the subsequent lectures.
In the fourth lecture, current status for numerical relativity simulations will be reviewed. In particular, I will present numerical results for merger of black hole and neutron star in detail.