Gravitational Waves from Dark Matter admixed Binary Neutron Star Mergers

This dataset contains Gravitational Waves (GW)s data from numerical relavity simulations of dark matter (DM) admixed binary neutron stars (BNS), presented in the preprint: "Numerical Relativity Simulations of Dark Matter Admixed Binary Neutron Stars". The simulations were performed using the BAM code and explore the dynamics of BNS systems where the neutron stars contain a fraction of non-interacting fermionic DM. This dataset contains time-series data for GW strain h and the Weyl scalar $\Psi_4$. Each data file (e.g., Rh_l2_m0_r00300) typically begins with a header section, which provides global parameter for the specific simulation run and extraction. Header Information: `# r=X.XXXXe+XX`: GW extraction radius in units solar masses ($M_\odot$). `# M=X.XXXXe+XX`: Total ADM mass of the initial binary system, in solar masses ($M_\odot$). `# Umerger=X.XXXXe+XX indxmerg=Y`: Scaled approximate retarded time coordinate of the merger ($u/M$), and its corresponding index in the data array. Data Columns: Following the header, each row represents a data point at a specific time. The columns are ordered as follows: 0: 'u/M', approximate retarded time coordinate divided by ADM mass 1: 'Reh/M', Real part of the GW strain times extraction radius divided by ADM mass 2: 'Imh/M', Imaginary part of the GW strain times extraction radius divided by ADM mass 3: 'Redh', Real part of the GW strain derivative times extraction radius 4: 'Imdh', Imaginary part of the GW strain derivative times extraction radius 5: 'Momega', instantenous GW frquency times ADM mass 6: 'A/M', GW amplitude divided by ADM mass 7: 'phi', Phase of the GW strain 8: 't/M', simulation time divided by ADM mass Naming Convention: Folders are named after the corresponding simulation using the following approach: "DMFraction_MassConfiguration_Resolution". Two distinct file types are available: those with and without the _cut suffix in their filenames. The _cut version contains the GW signal obtained by truncating the end of the simulation data before the strain computation. Files are named following a pattern like: "Rh/Rpsi4_l_m_ExtractionRadius.txt" For details on the extraction methodology and scaling, please refer to the associated preprint: Numerical Relativity Simulations of Dark Matter Admixed Binary Neutron Stars".