gravpy.interferometers.
AdvancedLIGO
(frequencies=None, configuration=None, obs_time=None)[source]¶The aLIGO Interferometer
Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self[, frequencies]) |
Calculate the one-sided power spectral desnity for a detector. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |
gravpy.interferometers.
BDecigo
(frequencies=None, configuration=None, obs_time=None)[source]¶Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self, frequencies) |
Calculate the one-sided power spectral desnity for a detector. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |
psd
(self, frequencies)[source]¶Calculate the one-sided power spectral desnity for a detector. If a particular configuration is specified then the results will be returned for a spline fit to that configuration’s curve, if available.
Parameters: |
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gravpy.interferometers.
BigBangObservatory
(frequencies=None, configuration=None, obs_time=None)[source]¶The Big Bang Observatory.
Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self, frequencies) |
The power spectrum density of the detector, taken from equation 6 of arxiv:1101.3940. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |
gravpy.interferometers.
Decigo
(frequencies=None, configuration=None, obs_time=None)[source]¶The full, original Decigo noise curve, from arxiv:1101.3940.
Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self, frequencies) |
The power spectrum density of the detector, taken from equation 5 of arxiv:1101.3940. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |
gravpy.interferometers.
Detector
[source]¶This is the base class for all types of detectors, and contains the conversion methods between the various different ways of expressing the noise levels (sensitivity) of any detector.
Methods
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
srpsd |
energy_density
(self, frequencies=None)[source]¶Produce the sensitivity curve of the detector in terms of the energy density.
Parameters: |
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Returns: |
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noise_amplitude
(self, frequencies=None)[source]¶The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal.
Parameters: |
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Returns: |
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gravpy.interferometers.
EvolvedLISA
(frequencies=None, configuration=None, obs_time=None)[source]¶The eLISA Interferometer
Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self, frequencies) |
Calculate the one-sided power spectral desnity for a detector. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |
psd
(self, frequencies)[source]¶Calculate the one-sided power spectral desnity for a detector. If a particular configuration is specified then the results will be returned for a spline fit to that configuration’s curve, if available.
Parameters: |
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gravpy.interferometers.
GEO
(frequencies=None, configuration=None, obs_time=None)[source]¶The GEO600 Interferometer
Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self[, frequencies]) |
Calculate the one-sided power spectral desnity for a detector. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |
gravpy.interferometers.
InitialLIGO
(frequencies=None, configuration=None, obs_time=None)[source]¶The iLIGO Interferometer
Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self[, frequencies]) |
Calculate the one-sided power spectral desnity for a detector. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |
gravpy.interferometers.
Interferometer
(frequencies=None, configuration=None, obs_time=None)[source]¶The base class to describe an interferometer.
Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self[, frequencies]) |
Calculate the one-sided power spectral desnity for a detector. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |
antenna_pattern
(self, theta, phi, psi)[source]¶Produce the antenna pattern for a detector, given its detector tensor, and a set of angles.
Parameters: |
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Returns: |
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noise_spectrum
(self, x)[source]¶Return the default noise spectrum for the interferometer.
Parameters: |
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Returns: |
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psd
(self, frequencies=None)[source]¶Calculate the one-sided power spectral desnity for a detector. If a particular configuration is specified then the results will be returned for a spline fit to that configuration’s curve, if available.
Parameters: |
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skymap
(self, nx=200, ny=100, psi=[0, 3.141592653589793])[source]¶Produce a skymap of the antenna repsonse of the interferometer.
Parameters: |
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Returns: |
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gravpy.interferometers.
LISA
(frequencies=None, configuration=None, obs_time=None)[source]¶The LISA Interferometer in its mission-accepted state, as of 2018
Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
confusion_noise (self, frequencies[, …]) |
The noise created by unresolvable galactic binaries at low frequencies. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
metrology_noise (self, frequencies) |
Calculate the noise due to the single-link optical metrology, from arxiv:1803.01944. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self, frequencies) |
Calculate the one-sided power spectral desnity for a detector. |
single_mass_noise (self, frequencies) |
The acceleration noise for a single test mass. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |
confusion_noise
(self, frequencies, observation_time=0.5)[source]¶The noise created by unresolvable galactic binaries at low frequencies.
metrology_noise
(self, frequencies)[source]¶Calculate the noise due to the single-link optical metrology, from arxiv:1803.01944.
psd
(self, frequencies)[source]¶Calculate the one-sided power spectral desnity for a detector. If a particular configuration is specified then the results will be returned for a spline fit to that configuration’s curve, if available.
Parameters: |
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gravpy.interferometers.
TAMA
(frequencies=None, configuration=None, obs_time=None)[source]¶The TAMA Interferometer
Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self[, frequencies]) |
Calculate the one-sided power spectral desnity for a detector. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |
gravpy.interferometers.
TimingArray
[source]¶A class to represent a pulsar timing array.
Methods
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
Pn | |
Sn | |
noise_spectrum | |
psd | |
srpsd |
gravpy.interferometers.
Virgo
(frequencies=None, configuration=None, obs_time=None)[source]¶The Virgo Interferometer
Methods
antenna_pattern (self, theta, phi, psi) |
Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. |
energy_density (self[, frequencies]) |
Produce the sensitivity curve of the detector in terms of the energy density. |
noise_amplitude (self[, frequencies]) |
The noise amplitude for a detector is defined as $h^2_n(f) = f S_n(f)$ and is designed to incorporate the effect of integrating an inspiralling signal. |
noise_spectrum (self, x) |
Return the default noise spectrum for the interferometer. |
plot (self[, axis]) |
Plot the noise curve for this detector. |
psd (self[, frequencies]) |
Calculate the one-sided power spectral desnity for a detector. |
skymap (self[, nx, ny, psi]) |
Produce a skymap of the antenna repsonse of the interferometer. |
srpsd |