Double Compact Objects: Upper Limits

All of the presented models and their properties are described in Dominik et al. 2015

Each group contains a tar.gz archive consisting of files: for NS-NS, BH-NS and BH-BH systems. The naming format is as follows:
waveform/instrument_id.model.system_type.metallicity_scenario.dat.
For example, the IMRPhenomCAdLIGOZDHP_20Hz.stan.nsns.high.dat file contains the data for the PhenomC, inspiral-merger-ringdown waveforms for Advanced LIGO with Zero-Detuning-High-Power sensitivity curve, cutoff at 20 Hz for NS-NS systems in the Standard Model for the high-end metallicity scenario. WARNING! The tar.gz files can be over 500 MB in size. The output format is:

• col. 1) time of birth in Myrs (0 Myrs is Big Bang).
• col. 2) redshift "z" corresponding to the time in col. 1.
• col. 3) time of merger in Myrs (0 Myrs is Big Bang).
• col. 4) redshift "z" corresponding to the time in col. 3.
• col. 5) delay time of a binary in Myrs, counted from the birth of the system to its merger.
• col. 6) non-redshifted mass of the primary (initially more massive) component.
• col. 7) non-redshifted mass of the secondary (initially less massive) component.
• col. 8) merger rate density in Gpc-3yr-1 (per comoving volume, per comoving time) contributed by the system.
• col. 9) absolute metallicity (Z) at which the system was born (Z=0.02 is solar metallicity).
• col. 10) signal-to-noise ratio for an optimally oriented and located binary with respect to the instrument.
• col. 11) horizon redshift for an optimally oriented and located binary.
• col. 12) location and orientation averaged contribution of the binary to the observed rate in yr-1 (sum over all to get the total rate).