Column | Description |
---|---|

ID | A unique identification string for a simulation. It identifies the collaboration, type of binary, and number. |

Data | Link to the metadata and downloadable data for a simulation. |

m_{1}/m_{2} |
Ratio of the Christodoulou masses at the relaxation time. We use $m_1>m_2$. |

χ_{1,2} |
Dimensionless spin magnitudes at the relaxation time. |

χ_{{1,2}{X,Y,Z}} |
Dimensionless spin vector components at the relaxation time. |

Ecc | Eccentricity estimated by fitting $d\omega_{orb}/dt$ for 2.5 orbits after the relaxation time. |

Mω_{orb} |
Orbital frequency multiplied by the total Christodoulou mass at the relaxation time. |

Orbits | Number of orbits from $t=0$ until the region inside the common horizon is excised. |

Link to e-mail the SXS Collaboration about a particular simulation. |

Various extrapolation orders are provided. The optimal choice depends on the application. For example, the extrapolation with order $N=4$ is usually most useful for data from early in the inspiral; during merger very little extrapolation is needed, so $N=4$ becomes noisy. Convergence tests are generally the best way to decide which extrapolation order to use.

For each extrapolation order, the datasets are contained in an h5-group labeled "Extrapolated_Nx.dir", where "x" is the order of the extrapolating polynomial used. There is also an h5-group labeled "OutermostExtraction.dir", for which no extrapolation was done, though all relevant rescalings were applied. The following datasets are provided in each group:

Dataset | Columns | Description |
---|---|---|

Y_l[L]_m[M].dat | $(t/M_{\text{Ch}}, \Re[R_{\text{areal}}Q_{\ell m}], \Im[R_{\text{areal}}Q_{\ell m}])$ | $Q_{\ell m}$ is the expansion coefficient in the spin-weight $s=-2$ spherical-harmonic decomposition of the gravitational-wave strain ($h/M_{\text{Ch}}$) or Penrose scalar ($M_{\text{Ch}}\Psi_4$). |

The groups and datasets in these files are exactly the same as in the corresponding files above; the only difference is the addition of the "_CoM" suffix in the file names.

These two files contain spin-weighted spherical harmonic coefficients for the gravitational radiation (and related quantities) extracted at various finite radii as a function of coordinate time $t$ in code units (

Dataset | Columns | Description |
---|---|---|

ArealRadius.dat | $(t, R_{\text{areal}})$ | $R_{\text{areal}}$ is the radius computed from the proper area of the extraction sphere. |

AverageLapse.dat | $(t, \bar{N})$ | $\bar{N}$ is the angular average of the lapse function across the extraction sphere. It is computed from the (L,M)=(0,0) mode of a scalar spherical harmonic decomposition of the lapse function on the extraction sphere. |

CoordRadius.dat | $(t, R_{\text{coord}})$ | $R_{\text{coord}}$ is the exact coordinate radius of the extraction sphere. |

Y_l[L]_m[M].dat | $(t, \Re[R_{\text{coord}}Q_{\ell m}], \Im[R_{\text{coord}}Q_{\ell m}])$ | $Q_{\ell m}$ is the expansion coefficient in the spin-weight $s=-2$ spherical harmonic decomposition of the gravitational wave strain ($h$) or Penrose scalar ($\Psi_4$). |

This HDF5 file contains information about the black holes' apparent horizons as a function of coordinate time $t$ in code units (

Dataset | Columns | Description |
---|---|---|

CoordCenterInertial.dat | $(t, x,y,z)$ | $x$,$y$,$z$ are the Cartesian coordinates of the center of the apparent horizon, in the "inertial frame," the asymptotically inertial frame in which the gravitational waves are measured. |

ArealMass.dat | $(t, M_{\text{irr}})$ | $M_{\text{irr}}$ is the areal (irreducible) mass $\sqrt{A/16\pi}$, where $A$ is the horizon surface area. |

DimensionfulInertialSpin.dat | $(t, S_x, S_y, S_z)$ | $S_i$ are the Cartesian vector components of the spin angular momentum measured on the apparent horizon in the "inertial frame". The spin is measured using approximate rotational Killing vectors (see Appendix A in arXiv:0805.4192 for details of the method used to measure the spin). |

DimensionfulInertialSpinMag.dat | $(t, S)$ | $S$ is the Euclidean magnitude of the black-hole spin angular momentum given in DimensionfulInertialSpin.dat, $S^2=S_x^2+S_y^2+S_z^2$. |

ChristodoulouMass.dat | $(t, M)$ | Christodoulou mass $M$, where $M^2 = M_{\text{irr}}^2 + S^2/4{M_{\text{irr}}^2}$ and $S$ is the magnitude of the spin angular momentum of the black hole (as given in DimensionfulInertialSpinMag.dat). |

chiInertial.dat | $(t, \chi_x, \chi_y, \chi_z)$ | $\chi_i = S_i/ M^2$, i.e., the Cartesian components of the spin angular momentum measured in the "inertial frame", made dimensionless by dividing by the square of the Christodoulou mass. |

chiMagInertial.dat | $(t, \chi)$ | $\chi$ is the Euclidean magnitude of the dimensionless spin angular momentum measured on the apparent horizon, $\chi^2 = \chi_x^2+\chi_y^2+\chi_z^2$. |

HorizonsDump.h5 contains one h5-group for each apparent horizon: AhA.dir, AhB.dir, and AhC.dir. The following datasets are provided:

Dataset | Description |
---|---|

CoordsMeasurementFrame.tdm | Inertial Cartesian coordinates of the apparent horizon surface. |

RicciScalar.tdm | The dimensionful Ricci scalar on the hypersurface, given by Eq. B3 in arXiv:0805.4192. |

DimlessRicciScalar.tdm | RicciScalar.tdm scaled by the Christodoulou mass, $M_{Ch}^2R$ |

SpinFunction.tdm | Curl of the angular momentum density. |

WeylB_NN.tdm | Magnetic Weyl tensor normal to the hypersurface, $B_{ij}n^in^j$. This quantity is known as the horizon vorticity. It should be negative at the north pole of a spinning black hole using the current conventions on $B_{ij}$, which are given by (2.2b) in arXiv:1108.5486. The horizon vorticity was first introduced in arXiv:1012.4869, and the physical interpretation of the vorticity can be found in the cited texts. See also arXiv:1208.3034 for its connection to measures of the angular momentum of the horizon. NOTE: The sign convention used for this quantity was switched in SpEC revision 08ac47f4 (Feb. 8, 2016), so all earlier catalog entries will differ by an overall minus sign. |

WeylE_NN.tdm | Electric Weyl tensor normal to the hypersurface, $E_{ij}n^in^j$. This quantity is known as the horizon tendicity, and describes tidal stretching (negative values of WeylE_NN) and compression (positive values) normal to the horizon. It was introduced in arXiv:1012.4869. Our conventions on $E_{ij}$ are given in arXiv:1108.5486, and note that it should be negative at the horizon of a Schwarzschild black hole. See also arXiv:1208.3034 for its connection to the Ricci curvature of the horizon. |

The following files are provided:

File | Description |
---|---|

ID_Ah{A,B}Coefs.dat | Coefficients characterizing the spectral expansion of the horizon surfaces. |

ID_Init_FuncLambdaFactor{A,B,A0,B0}.txt | Initial deformations of the spatial coordinates to conform to the black-hole shapes. These files also include initial velocities of the excision surfaces, which are sometimes nonzero in order to avoid incoming characteristic fields at the beginning of the evolution. |

Domain.input and SpatialCoordMap.input | Specify the initial spatial computational domain. |

Vars*.h5 | HDF5 files containing the initial spatial metric $g$, extrinsic curvature $K$, lapse $N$, and shift $\beta_i$. |