This archive is a catalogue of the maximum density evolution of 136 supernova core collapse models as described in detail in this paper: 1. Dimmelmeier, H., Ott, C.D., Marek, A., and Janka, H.-T., "The gravitational wave burst signal from stellar core collapse and bounce", Phys. Rev. D, submitted, (2008). It contains the following files: signal_e15a_shen.dat signal_e15a_ls.dat signal_e15b_shen.dat signal_e15b_ls.dat signal_e20a_shen.dat signal_e20a_ls.dat signal_e20b_shen.dat signal_e20b_ls.dat signal_s11a1o01_shen.dat signal_s11a1o01_ls.dat signal_s11a1o05_shen.dat signal_s11a1o05_ls.dat signal_s11a1o07_shen.dat signal_s11a1o07_ls.dat signal_s11a1o09_shen.dat signal_s11a1o09_ls.dat signal_s11a1o13_shen.dat signal_s11a1o13_ls.dat signal_s11a2o05_shen.dat signal_s11a2o05_ls.dat signal_s11a2o07_shen.dat signal_s11a2o07_ls.dat signal_s11a2o09_shen.dat signal_s11a2o09_ls.dat signal_s11a2o13_shen.dat signal_s11a2o13_ls.dat signal_s11a2o15_shen.dat signal_s11a2o15_ls.dat signal_s11a3o05_shen.dat signal_s11a3o05_ls.dat signal_s11a3o07_shen.dat signal_s11a3o07_ls.dat signal_s11a3o09_shen.dat signal_s11a3o09_ls.dat signal_s11a3o12_shen.dat signal_s11a3o12_ls.dat signal_s11a3o13_shen.dat signal_s11a3o13_ls.dat signal_s11a3o15_shen.dat signal_s11a3o15_ls.dat signal_s15a1o01_shen.dat signal_s15a1o01_ls.dat signal_s15a1o05_shen.dat signal_s15a1o05_ls.dat signal_s15a1o07_shen.dat signal_s15a1o07_ls.dat signal_s15a1o09_shen.dat signal_s15a1o09_ls.dat signal_s15a1o13_shen.dat signal_s15a1o13_ls.dat signal_s15a2o05_shen.dat signal_s15a2o05_ls.dat signal_s15a2o07_shen.dat signal_s15a2o07_ls.dat signal_s15a2o09_shen.dat signal_s15a2o09_ls.dat signal_s15a2o13_shen.dat signal_s15a2o13_ls.dat signal_s15a2o15_shen.dat signal_s15a2o15_ls.dat signal_s15a3o05_shen.dat signal_s15a3o05_ls.dat signal_s15a3o07_shen.dat signal_s15a3o07_ls.dat signal_s15a3o09_shen.dat signal_s15a3o09_ls.dat signal_s15a3o12_shen.dat signal_s15a3o12_ls.dat signal_s15a3o13_shen.dat signal_s15a3o13_ls.dat signal_s15a3o15_shen.dat signal_s15a3o15_ls.dat signal_s20a1o01_shen.dat signal_s20a1o01_ls.dat signal_s20a1o05_shen.dat signal_s20a1o05_ls.dat signal_s20a1o07_shen.dat signal_s20a1o07_ls.dat signal_s20a1o09_shen.dat signal_s20a1o09_ls.dat signal_s20a1o13_shen.dat signal_s20a1o13_ls.dat signal_s20a2o05_shen.dat signal_s20a2o05_ls.dat signal_s20a2o07_shen.dat signal_s20a2o07_ls.dat signal_s20a2o09_shen.dat signal_s20a2o09_ls.dat signal_s20a2o13_shen.dat signal_s20a2o13_ls.dat signal_s20a2o15_shen.dat signal_s20a2o15_ls.dat signal_s20a3o05_shen.dat signal_s20a3o05_ls.dat signal_s20a3o07_shen.dat signal_s20a3o07_ls.dat signal_s20a3o09_shen.dat signal_s20a3o09_ls.dat signal_s20a3o12_shen.dat signal_s20a3o12_ls.dat signal_s20a3o13_shen.dat signal_s20a3o13_ls.dat signal_s20a3o15_shen.dat signal_s20a3o15_ls.dat signal_s40a1o01_shen.dat signal_s40a1o01_ls.dat signal_s40a1o05_shen.dat signal_s40a1o05_ls.dat signal_s40a1o07_shen.dat signal_s40a1o07_ls.dat signal_s40a1o09_shen.dat signal_s40a1o09_ls.dat signal_s40a1o13_shen.dat signal_s40a1o13_ls.dat signal_s40a2o05_shen.dat signal_s40a2o05_ls.dat signal_s40a2o07_shen.dat signal_s40a2o07_ls.dat signal_s40a2o09_shen.dat signal_s40a2o09_ls.dat signal_s40a2o13_shen.dat signal_s40a2o13_ls.dat signal_s40a2o15_shen.dat signal_s40a2o15_ls.dat signal_s40a3o05_shen.dat signal_s40a3o05_ls.dat signal_s40a3o07_shen.dat signal_s40a3o07_ls.dat signal_s40a3o09_shen.dat signal_s40a3o09_ls.dat signal_s40a3o12_shen.dat signal_s40a3o12_ls.dat signal_s40a3o13_shen.dat signal_s40a3o13_ls.dat signal_s40a3o15_shen.dat signal_s40a3o15_ls.dat The equation of state used during the evolution is either the one of Shen et al. (Shen EoS) or the one by Lattimer and Swesty (LS EoS). The initial model is the presupernova stellar model e15a/e15b/e20a/e20b/s11.2/s15/s20/s40, where the e15a/e15b/e20a/e20b have an angular momentum distribution from stellar evolution calculations, while the s11.2/s15/s20/s40 models rotate at prescribed different rates with various profiles. Each collapse model is specified by two parameters, A and O: A1: A = 5.0 * 10^9 cm A2: A = 1.0 * 10^8 cm A3: A = 5.0 * 10^7 cm A1O01: Omega_c,i = 0.45 rad/s A1O05: Omega_c,i = 1.01 rad/s A1O07: Omega_c,i = 1.43 rad/s A1O09: Omega_c,i = 1.91 rad/s A1O13: Omega_c,i = 2.71 rad/s A2O05: Omega_c,i = 2.40 rad/s A2O07: Omega_c,i = 3.40 rad/s A2O09: Omega_c,i = 4.56 rad/s A2O13: Omega_c,i = 6.45 rad/s A2O15: Omega_c,i = 7.60 rad/s A3O05: Omega_c,i = 4.21 rad/s A3O07: Omega_c,i = 5.95 rad/s A3O09: Omega_c,i = 8.99 rad/s A3O12: Omega_c,i = 10.65 rad/s A3O13: Omega_c,i = 11.30 rad/s A3O15: Omega_c,i = 13.31 rad/s Only for the s20 model, this corresponds to the following rotation rates beta_rot_ini (with the 'old' notation): O01 --> B0.05: beta_rot_ini = 0.05% O05 --> B0.25: beta_rot_ini = 0.25% O07 --> B0.50: beta_rot_ini = 0.50% O09 --> B0.90: beta_rot_ini = 0.90% O12 --> B1.60: beta_rot_ini = 1.60% O13 --> B1.80: beta_rot_ini = 1.80% O15 --> B2.50: beta_rot_ini = 2.50% All signals have been obtained by using the quadrupole 'first momentum of momentum density formula', Column 1 is the coordinate time 't' in units of milliseconds. Column 2 is the dimensionless signal amplitude 'h^TT' at a distance of 10 kpc with optimal orientation of the source (i.e. measured in the equatorial plane). This waveform catalogue can be obtained freely from this URL: http://www.mpa-garching.mpg.de/rel_hydro/ ----------------------------------------------------------------- 27 February 2008, Harald Dimmelmeier (harrydee@mpa-garching.mpg.de).