The Interferometers Module¶

class 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 advanced-plus 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 straight-forward 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)

Attributes

configurationstr, optional: 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

`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.
`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`(self[, frequencies])	The square-root of the PSD.

noise_spectrum

class gravpy.interferometers.BDecigo(frequencies=None, configuration=None, obs_time=None)[source]¶

The B-Decigo noise curve [R743444ceb418-arxivcurve].

References

R743444ceb418-arxivcurve: arxiv:1802.06977

Examples

(Source code, png)

Attributes

configuration

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.
`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`(self[, frequencies])	The square-root of the PSD.

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

frequenciesndarray: An array of frequencies where the PSD should be evaluated.
configurationstr: The configuration of the detector for which the curve should be returned.

class gravpy.interferometers.BigBangObservatory(frequencies=None, configuration=None, obs_time=None)[source]¶

The Big Bang Observatory.

Attributes

configuration

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.
`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`(self[, frequencies])	The square-root of the PSD.

psd(self, frequencies)[source]¶: The power spectrum density of the detector, taken from equation 6 of arxiv:1101.3940.

class 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)

Attributes

configuration

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.
`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`(self[, frequencies])	The square-root of the PSD.

psd(self, frequencies)[source]¶: The power spectrum density of the detector, taken from equation 5 of arxiv:1101.3940.

class 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`(self[, frequencies])	The square-root of the PSD.

energy_density(self, frequencies=None)[source]¶

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

Parameters

frequenciesndarray: An array of frequencies, in units of Hz

Returns

energy_densityndarray: 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.

Parameters

frequenciesndarray: An array of frequencies, in units of Hz

Returns

noise_amplitudendarray: An array of the noise amplitudes correcsponding to the input frequency values

plot(self, axis=None, **kwargs)[source]¶: Plot the noise curve for this detector.

srpsd(self, frequencies=None)[source]¶: The square-root of the PSD.

gravpy.interferometers.ET¶: alias of gravpy.interferometers.EinsteinTelescope

class gravpy.interferometers.EinsteinTelescope(frequencies=None, configuration=None, obs_time=None)[source]¶

The Einstein Telescope 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.
`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`(self[, frequencies])	The square-root of the PSD.

psd(self, frequencies=None)[source]¶

Parameters

frequenciesndarray: An array of frequencies where the PSD should be evaluated.
configurationstr: The configuration of the detector for which the curve should be returned.

class gravpy.interferometers.EvolvedLISA(frequencies=None, configuration=None, obs_time=None)[source]¶

The eLISA Interferometer

Attributes

configuration

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.
`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`(self[, frequencies])	The square-root of the PSD.

psd(self, frequencies)[source]¶

Parameters

frequenciesndarray: An array of frequencies where the PSD should be evaluated.
configurationstr: The configuration of the detector for which the curve should be returned.

class gravpy.interferometers.GEO(frequencies=None, configuration=None, obs_time=None)[source]¶

The GEO600 Interferometer

Attributes

configuration

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.
`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`(self[, frequencies])	The square-root of the PSD.

noise_spectrum

class gravpy.interferometers.InitialLIGO(frequencies=None, configuration=None, obs_time=None)[source]¶

The iLIGO Interferometer

Attributes

configuration

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.
`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`(self[, frequencies])	The square-root of the PSD.

noise_spectrum

class gravpy.interferometers.Interferometer(frequencies=None, configuration=None, obs_time=None)[source]¶

The base class to describe an interferometer.

Attributes

configurationstr, optional: 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

`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.
`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`(self[, frequencies])	The square-root 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.

Parameters

thetafloat: The altitude angle.
phifloat: The azimuthal angle.
psifloat or list: 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.

Returns

F+float: The antenna response to the ‘+’ polarisation state.
Fxfloat: The antenna response to the ‘x’ polsarisation state.
|F|float: The combined antenna response (sqrt(F+^2 + Fx^2)).

psd(self, frequencies=None)[source]¶

Parameters

frequenciesndarray: An array of frequencies where the PSD should be evaluated.
configurationstr: 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.

Parameters

nxint: The number of locations along the horizontal axis to produce the map at defaults to 200.
nyint: The number of locations along the vertical axis to produce the map at defaults to 100
psifloat or list: The polarisation angle to produce the map at. If a list is given then the integrated response is given between those angles.

Returns

xndarray: The x values for the map
y: ndarray: The y values for the map
antennapndarray: The values of the sensitivity in the + polarisation
antennaxndarray: The values of the sensitivity in the x polarisation
antennacndarray: The values of the combined polarisation sensitivities

class gravpy.interferometers.LISA(frequencies=None, configuration=None, obs_time=None)[source]¶

The LISA Interferometer in its mission-accepted state, as of 2018

Attributes

configuration

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.
`plot`(self[, axis])	Plot the noise curve for this detector.
`psd`(self, frequencies)	The power spectral density.
`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`(self[, frequencies])	The square-root of the PSD.

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]¶: The power spectral density.

single_mass_noise(self, frequencies)[source]¶: The acceleration noise for a single test mass.

class gravpy.interferometers.TAMA(frequencies=None, configuration=None, obs_time=None)[source]¶

The TAMA Interferometer

Attributes

configuration

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.
`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`(self[, frequencies])	The square-root of the PSD.

noise_spectrum

class 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.
`srpsd`(self[, frequencies])	The square-root of the PSD.

Pn
Sn
noise_spectrum
psd

class gravpy.interferometers.Virgo(frequencies=None, configuration=None, obs_time=None)[source]¶

The Virgo Interferometer

Attributes

configuration

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.
`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`(self[, frequencies])	The square-root of the PSD.

noise_spectrum