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Waveform Catalogue¤

This catalogue lists the waveform models available in ripple and the physical assumptions that distinguish them. The model names below are the names used by ripple.

Terminology¤

  • Aligned-spin models assume that both component spins are parallel or antiparallel to the orbital angular momentum.
  • Precessing-spin models allow spin directions that cause the orbital plane to precess.
  • Higher-order modes include radiation beyond the dominant quadrupole mode; they can be important for unequal-mass binaries and for systems viewed away from face-on.
  • Tidal effects describe the deformation of neutron stars by their companions.

Compact-binary coalescences¤

These models describe radiation from two compact objects in a quasi-circular orbit. All compact-binary-coalescence waveforms in ripple are provided in the frequency domain at the moment.

TaylorF2¤

TaylorF2 is a post-Newtonian, aligned-spin waveform with tidal effects. It models the inspiral only and does not include merger or ringdown.

Earlier IMRPhenom models¤

Waveform Spin treatment Higher-order modes Tidal effects
IMRPhenomD Aligned-spin No No
IMRPhenomHM Aligned-spin Yes No
IMRPhenomPv2 Precessing No No
IMRPhenomD_NRTidalv2 Aligned-spin No NRTidalv2

IMRPhenomX family¤

The IMRPhenomX models are the newer IMRPhenom models.

Waveform Spin treatment Higher-order modes Tidal effects
IMRPhenomXAS Aligned-spin No No
IMRPhenomXHM Aligned-spin Yes No
IMRPhenomXP Precessing No No
IMRPhenomXPHM Precessing Yes No
IMRPhenomXAS_NRTidalv3 Aligned-spin No NRTidalv3

Bursts¤

SineGaussian is a short-duration burst model that describes a sine-Gaussian waveform in the time domain.

Continuous waves¤

These models describe long-lived, nearly periodic signals from pulsars.

Waveform Source Timing treatment
ExactPulsarSignal Isolated pulsar Geometric barycentric corrections
PulsarSignal Isolated pulsar Full barycentric corrections
BinaryPulsarSignal Pulsar in a binary Full barycentric corrections and orbital modulation