## Section V. Astrophysical implications

Short explanation of files in the data release


### `popsummary_BNS-NSBHrates.h5`

popsummary file containing the distribution of NSBH and BNS local rate estimates under the hyperparameters keys: `['BNS']`, `['NSBH3Msun']`

### `default_O4A_population_MD_rate_stochfinal.npy`

This file contains the posterior samples for the hyperparameters from the population inference after stochastic rejection sampling. The hyperparameters are stored under the following keys:

Primary mass: **Broken Power Law + 2 Peaks model**  
`alpha1`: negative spectral index of the 1st power law  
`alpha2`: negative spectral index of the 2nd power law  
`mBreak`: power law break location  
`m̀u_m1`: location of the first peak  
`sig_m1`: width of the first peak  
`m̀u_m2`: location of the second peak  
`sig_m2`: width of the second peak  
`m1_min`: lower edge of taper function  
`m1_max`: maximum mass  
`dm1_min`: mass range of low mass tapering  
`fPeak1`: Mixing fraction in first peak  
`fPeak2`: Mixing fraction in second peak  

Mass ratio: **Power Law model**  
`bq`: spectral index of mass ratio power law  
`m2_min`: lower edge of taper function  
`dm2_min`: mass range of low mass tapering  

Spin distribution: **Gaussian component spins model**  
`mu_chi`: location of the spin magnitude distribution  
`sig_chi`: width of the spin magnitude distribution  
`mu_cost`: location of the Gaussian component of the spin tilt distribution  
`sig_cost`: width of the Gaussian component of the spin tilt distribution  
`f_iso`: fraction in the isotropic part of the spin tilt distribution  

Redshift distribution: **Broken Power Law model**  
`R0`: local rate at redshift 0  
`alpha_z`: spectral index of the low redshift power law  
`beta_z`: spectral index of the high redshift power law  
`zPeak`: peak of the merger rate history  

### `omegas_o4a_default_spin_planck15lal_final.npy`

This file contains the BBH energy density spectra after stochastic rejection sampling. A corresponding frequency array is stored under the key `['freqs']`, while the individual spectra are found under the key `['omega_gw']`.