Interferometers supported by gravpy¶

Initial LIGO¶

Initial Virgo¶

GEO¶

Advanced LIGO¶

The design sensitivity noise curve for the advanced LIGO detector is available in the ifo.AdvancedLIGO class, and it can be used in a program by assigning the class to a variable:

aligo = ifo.AdvancedLIGO()

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

Advanced Virgo¶

The design sensitivity of advanced Virgo is available in gravpy using the AdvancedVirgo class.

(Source code)

Kagra¶

(Source code)

Einstein Telescope¶

Cosmic Explorer¶

LISA¶

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.

eLISA¶

Decigo¶

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.

BDecigo¶

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

The B-Decigo noise curve [arxivcurve].

References

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.

TianQin¶

Big Bang Observatory¶