gravpy.interferometers.
AdvancedLIGO
(frequencies=None, configuration=None, obs_time=None)[source]¶The advanced LIGO Interferometer.
Supported configurations are
Configuration 
Description 

O1 
First observing run sensitivity 
A+ 
The advancedplus design sensitivity 
See also
InitialLIGO
The initial LIGO interferometer
Examples
Specific configurations can be loaded by passing the configuration keyword argument.
>>> aligo = ifo.AdvancedLIGO(configuration="O1")
It’s straightforward to plot the sensitivity curve for the detector at design sensitivity.
>>> import matplotlib.pyplot as plt
>>> import gravpy.interferometers as ifo
>>> aligo = ifo.AdvancedLIGO()
>>> f, ax = plt.subplots(1)
>>> aligo.plot(ax)
Which should produce an output along the lines of
(Source code, png)
A specific configuration for a given interferometer. This allows for the sensitivity from a given run to be used, or from a specific tuning.
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

Calculate the onesided power spectral desnity for a detector. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
noise_spectrum 
gravpy.interferometers.
BDecigo
(frequencies=None, configuration=None, obs_time=None)[source]¶The BDecigo noise curve [R743444ceb418arxivcurve].
References
arxiv:1802.06977
Examples
(Source code, png)
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

Calculate the onesided power spectral desnity for a detector. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
psd
(self, frequencies)[source]¶Calculate the onesided 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.
An array of frequencies where the PSD should be evaluated.
The configuration of the detector for which the curve should be returned.
gravpy.interferometers.
BigBangObservatory
(frequencies=None, configuration=None, obs_time=None)[source]¶The Big Bang Observatory.
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

The power spectrum density of the detector, taken from equation 6 of arxiv:1101.3940. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
gravpy.interferometers.
Decigo
(frequencies=None, configuration=None, obs_time=None)[source]¶The full, original Decigo noise curve, from arxiv:1101.3940.
Examples
(Source code, png)
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

The power spectrum density of the detector, taken from equation 5 of arxiv:1101.3940. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
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

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

The squareroot of the PSD. 
energy_density
(self, frequencies=None)[source]¶Produce the sensitivity curve of the detector in terms of the energy density.
An array of frequencies, in units of Hz
An array of the dimensionless energy density of the sensitivity of the detector.
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.
An array of frequencies, in units of Hz
An array of the noise amplitudes correcsponding to the input frequency values
gravpy.interferometers.
ET
¶gravpy.interferometers.
EinsteinTelescope
(frequencies=None, configuration=None, obs_time=None)[source]¶The Einstein Telescope Interferometer
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

Calculate the onesided power spectral desnity for a detector. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
psd
(self, frequencies=None)[source]¶Calculate the onesided 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.
An array of frequencies where the PSD should be evaluated.
The configuration of the detector for which the curve should be returned.
gravpy.interferometers.
EvolvedLISA
(frequencies=None, configuration=None, obs_time=None)[source]¶The eLISA Interferometer
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

Calculate the onesided power spectral desnity for a detector. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
psd
(self, frequencies)[source]¶Calculate the onesided 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.
An array of frequencies where the PSD should be evaluated.
The configuration of the detector for which the curve should be returned.
gravpy.interferometers.
GEO
(frequencies=None, configuration=None, obs_time=None)[source]¶The GEO600 Interferometer
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

Calculate the onesided power spectral desnity for a detector. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
noise_spectrum 
gravpy.interferometers.
InitialLIGO
(frequencies=None, configuration=None, obs_time=None)[source]¶The iLIGO Interferometer
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

Calculate the onesided power spectral desnity for a detector. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
noise_spectrum 
gravpy.interferometers.
Interferometer
(frequencies=None, configuration=None, obs_time=None)[source]¶The base class to describe an interferometer.
A specific configuration for a given interferometer. This allows for the sensitivity from a given run to be used, or from a specific tuning.
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

Calculate the onesided power spectral desnity for a detector. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
antenna_pattern
(self, theta, phi, psi)[source]¶Produce the antenna pattern for a detector, given its detector tensor, and a set of angles.
The altitude angle.
The azimuthal angle.
The polarisation angle. If psi is a list of two angles the returned antenna patterns will be the integrated response between those two polsarisation angles.
The antenna response to the ‘+’ polarisation state.
The antenna response to the ‘x’ polsarisation state.
The combined antenna response (sqrt(F+^2 + Fx^2)).
psd
(self, frequencies=None)[source]¶Calculate the onesided 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.
An array of frequencies where the PSD should be evaluated.
The configuration of the detector for which the curve should be returned.
skymap
(self, nx=200, ny=100, psi=[0, 3.141592653589793])[source]¶Produce a skymap of the antenna repsonse of the interferometer.
The number of locations along the horizontal axis to produce the map at defaults to 200.
The number of locations along the vertical axis to produce the map at defaults to 100
The polarisation angle to produce the map at. If a list is given then the integrated response is given between those angles.
The x values for the map
The y values for the map
The values of the sensitivity in the + polarisation
The values of the sensitivity in the x polarisation
The values of the combined polarisation sensitivities
gravpy.interferometers.
LISA
(frequencies=None, configuration=None, obs_time=None)[source]¶The LISA Interferometer in its missionaccepted state, as of 2018
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

The noise created by unresolvable galactic binaries at low frequencies. 

Produce the sensitivity curve of the detector in terms of the energy density. 

Calculate the noise due to the singlelink optical metrology, from arxiv:1803.01944. 

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 the noise curve for this detector. 

The power spectral density. 

The acceleration noise for a single test mass. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
confusion_noise
(self, frequencies, observation_time=0.5)[source]¶The noise created by unresolvable galactic binaries at low frequencies.
gravpy.interferometers.
TAMA
(frequencies=None, configuration=None, obs_time=None)[source]¶The TAMA Interferometer
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

Calculate the onesided power spectral desnity for a detector. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
noise_spectrum 
gravpy.interferometers.
TimingArray
[source]¶A class to represent a pulsar timing array.
Methods

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

The squareroot of the PSD. 
Pn 

Sn 

noise_spectrum 

psd 
gravpy.interferometers.
Virgo
(frequencies=None, configuration=None, obs_time=None)[source]¶The Virgo Interferometer
Methods

Produce the antenna pattern for a detector, given its detector tensor, and a set of angles. 

Produce the sensitivity curve of the detector in terms of the energy density. 

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 the noise curve for this detector. 

Calculate the onesided power spectral desnity for a detector. 

Produce a skymap of the antenna repsonse of the interferometer. 

The squareroot of the PSD. 
noise_spectrum 