Data files for "Tracing the evolution of eccentric precessing binary black holes: a hybrid approach"

The following tab-separated files accompany the scientific paper accessible here, providing the data plotted in that paper. The first 7 files are generated using the tilts_at_infinity code which is publically accessible here. The first five files contain the parameters for 2000 simulated binary black holes (BBHs) and results of applying that code to the binaries. Files 6 and 7 contain the results of evolving one binary each. File 8 comes from the Belczynski et al. scientific publication. The full list of files and their description is given below. We recommend importing and analyzing these files as pandas dataframes by using the command df=pd.read_table(filename). The columns for evolved data are not included for binaries that don't evolve successfully. One gets np.nan for these values by default when loading the data with pandas.

1. eccentric_collated_tilts_spinO4_phaseO6_vtrans_figs_1_to_6.txt

This file contains a simulated dataset of 2000 binary black holes, which are evolved from a reference frequency of 20 Hz to the empirically determined transition orbital velocity (vtrans). The following table introduces all columns and their physical interpretation.

m1, m2
Component masses of the binary black holes, in solar masses

chi1, chi2
Dimensionless spin magnitudes of black hole 1 (BH1) and black hole 2 (BH2) respectively (bounded between 0 and 1)

tilt1_ini,

tilt2_ini

Initial spin tilt angles (in radians) of BH1 and BH2 at the reference frequency

psi1, psi2
Azimuthal spin orientation angles (in radians) for BH1 and BH2 at the reference frequency.

fref
Reference frequency at which the binary evolution begins (fixed at 20 Hz)

ecc
Initial orbital eccentricity (e_t) at the reference frequency

spinO, phaseO
Twice the PN order of spinning and non-spinning terms respectively. The spinO is fixed to 4 in all files and the phaseO is fixed to 6 for all files except the third one.

tilt1_vtrans, 

tilt2_vtrans

Spin tilt angles of BH1 and BH2 (in radians) at the empirically determined transition orbital velocity (vtrans).

phi12_vtrans
Relative azimuthal angle (psi2 - psi1; in radians) between the two spin vectors at vtrans

tilt1_final_hyb,

tilt2_final_hyb

Spin tilt angles at infinity (in radians) using hybrid evolution code

Runtime
Time taken to perform the evolution for this binary (in seconds).

code
Four digit code representing the physical condition which the code terminated with (see table I in this paper). Binaries which did not start their evolution contain the conditions d_L0_dt_positive (initial time derivative of binary's orbital angular momentum is positive), ini_epsilon_negative (binary is initially unbound), or d_epsilon_dt_ini_negative (initial time derivative of the binary's energy is positive; only in file 3)

e_vtrans
Eccentricity (e_t) at vtrans

This file has been used in creating figures 1 to 6 in the paper.

2. eccentric_collated_tilts_spinO4_phaseO6_0p5_vtrans_fig_1_and_2.txt

This file contains the same set of 2000 simulated binaries as in file 1, except that the spin angles (tilt1_vtrans, tilt2_vtrans, and phi12_vtrans) and tilts at infinity (tilt1_final_hyb and tilt2_final_hyb) are at half of vtrans. This file has been used in creating Figs. 1 and 2 in the paper.

3. eccentric_collated_tilts_spinO4_phaseO5_vtrans_fig_3.txt

his file contains the same set of 2000 simulated binaries as in file 1, except that phaseO=5 in this case. This file has been used in creating Fig. 3 in the paper.

4. quasi_circular_collated_tilts_spinO4_phaseO6_vtrans_fig_5.txt

This file contains the same set of 2000 simulated binaries as in file 1, but the tilts at infinity are obtained using the quasi-circular hybrid evolution code. This file has been used in creating Fig. 5 in the paper.

5. eccentric_collated_tilts_spinO4_phaseO6_prec_only_fig_6.txt

This file contains the same set of 2000 simulated binaries as in file 1, except that it uses only precession-averaged evolution rather than the full hybrid evolution. This file has been used in creating Fig. 6 in the paper.

6. eccentric_collated_tilts_ecc_0p05_fig_7.txt

This file contains the spin tilts obtained for a single binary whose eccentricity at fref=20 Hz is fixed at 0.05. Rather than using the empirical value of vtrans, each row corresponds to a different value of the vtrans. This file has been used in creating Fig. 7 in the paper.

7. eccentric_collated_tilts_ecc_0p00625_fig_7.txt

This file contains the spin tilts obtained for a single binary whose eccentricity at fref=20 Hz is fixed at 0.00625. Rather than using the empirical value of vtrans, each row corresponds to a different value of the vtrans. This file has been used in creating Fig. 7 in the paper.

8. dyn_and_iso_formation_delta_cos_tilt_bw_10Hz_and_formation_fig_8.txt

This file contains the data plotted in Fig 8. The columns give the population considered (dynamical or isolated), the formation channel for the dynamically formed population (three-body induced binary, binary-single capture, or ZLK remnant binary), the jittered horizontal axis position in Fig. 8 for tilts 1 and 2, and the differences in the cosines of the tilts between formation and 10 Hz.

The dynamical binaries are drawn from the open data published here from Kritos et al., which samples binary black holes formed in dense stellar environments such as globular clusters.

The isolated binaries originate from the file IMRPhenomDAdLIGOMidHigh.dat_m30.sfrL.dat, which represents a population formed through isolated binary stellar evolution, is from Belczynski et al. scientific publication. 

Each row in the file corresponds to a single binary and includes the population type, the x-axis positions used in the associated scatter plots, and the quantities δcosθ₁ and δcosθ₂. 

9. IMRPhenomDAdLIGOMidHigh.dat_m30.sfrL.dat

This .dat file contains the binary black holes formed through isolated formation scenario from the Belczynski et al. scientific publication. A total of 500 randomly sampled binaries from the full dataset have been used to generate parts of Fig. 8 in the scientific publication. This was originally available, and we are grateful to the authors of the paper for allowing us to republish this data. A description of the dataset and the assumptions underlying it is provided in the file named IMRPhenomDAdLIGOMidHigh.dat_m30.sfrL.dat_description.txt