開発版ドキュメント · 0.2.3 30c2f8ba · 入門例の検証対象 0.2.3 · 版情報 · 既知の制限

Astrophysics Utilities

Astrophysics-related tools including binary inspiral range calculations.

gwexpy.astro.burst_range(psd: FrequencySeries, snr: float = 8, energy: float = 0.01, fmin: float = 100, fmax: float = 500) → units.Quantity

Calculate the integrated GRB-like GW burst range from a strain PSD.

パラメータ:

• psd (~gwpy.frequencyseries.FrequencySeries) -- The instrumental power-spectral-density data.

• snr (float, optional) -- The signal-to-noise ratio for which to calculate range.

• energy (float, optional) -- The relative energy output of the GW burst.

• fmin (float, optional) -- The lower frequency cutoff of the burst range integral.

• fmax (float, optional) -- The upper frequency cutoff of the burst range integral.

戻り値:

range -- The GRB-like-burst sensitive range [Mpc (default)].

戻り値の型:

~astropy.units.Quantity

サンプル

Grab some data for LIGO-Livingston around GW150914 and generate a PSD

>>> from gwpy.timeseries import TimeSeries
>>> hoft = TimeSeries.fetch_open_data("H1", 1126259446, 1126259478)
>>> hoff = hoft.psd(fftlength=4)

Now we can calculate the burst_range():

>>> from gwpy.astro import burst_range
>>> r = burst_range(hoff, fmin: float = 30)
>>> print(r)
42.5055584195 Mpc

gwexpy.astro.burst_range_spectrum(psd: FrequencySeries, snr: float = 8, energy: float = 0.01) → FrequencySeries

Calculate the frequency-dependent GW burst range from a strain PSD.

パラメータ:

• psd (~gwpy.frequencyseries.FrequencySeries) -- The instrumental power-spectral-density data.

• snr (float, optional) -- The signal-to-noise ratio for which to calculate range.

• energy (float, optional) -- The relative energy output of the GW burst.

戻り値:

rangespec -- The burst range FrequencySeries [Mpc (default)].

戻り値の型:

~gwpy.frequencyseries.FrequencySeries

gwexpy.astro.inspiral_range(psd: FrequencySeries, snr: float = 8, mass1: float = 1.4, mass2: float = 1.4, fmin: float | None = None, fmax: float | None = None, *, horizon: bool = False, **kwargs) → units.Quantity

Calculate the cosmology-corrected inspiral sensitive distance.

This method returns the distance (in megaparsecs) to which a compact binary inspiral with the given component masses would be detectable given the instrumental PSD. The calculation is defined in Belczynski et. al (2014):

https://dx.doi.org/10.1088/0004-637x/789/2/120

パラメータ:

• psd (~gwpy.frequencyseries.FrequencySeries) -- The instrumental power-spectral-density data.

• snr (float, optional) -- The signal-to-noise ratio for which to calculate range.

• mass1 (float, ~astropy.units.Quantity, optional) -- The mass of the first binary component (float assumed in solar masses).

• mass2 (float, ~astropy.units.Quantity, optional) -- The mass of the second binary component (float assumed in solar masses).

• fmin (float, optional) -- The lower frequency cut-off of the integral, default: psd.df.

• fmax (float, optional) -- The maximum frequency limit of the integral, defaults to the rest-frame innermost stable circular orbit (ISCO) frequency.

• horizon (bool, optional) -- If True, return the maximal 'horizon' luminosity distance, otherwise return the angle-averaged comoving distance.

• **kwargs -- Additional keyword arguments to ~inspiral_range.waveform.CBCWaveform.

戻り値:

range -- The calculated inspiral range [Mpc].

戻り値の型:

~astropy.units.Quantity

サンプル

Grab some data for LIGO-Livingston around GW150914 and generate a PSD:

>>> from gwpy.timeseries import TimeSeries
>>> hoft = TimeSeries.fetch_open_data("H1", 1126259446, 1126259478)
>>> hoff = hoft.psd(fftlength=4)

Now, we can calculate the inspiral_range():

>>> from gwpy.astro import inspiral_range
>>> r = inspiral_range(hoff, fmin: float = 30)
>>> print(r)
70.4612102889 Mpc

参考

sensemon_range

For the method based on LIGO-T030276, also known as LIGO SenseMonitor.

inspiral-range

The package which does heavy lifting for waveform simulation and cosmology calculations.

gwexpy.astro.inspiral_range_psd(psd: FrequencySeries, snr: float = 8, mass1: float = 1.4, mass2: float = 1.4, *, horizon: bool = False, **kwargs) → FrequencySeries

Calculate the cosmology-corrected inspiral sensitive distance PSD.

This method returns the power spectral density (in Mpc**2 / Hz) to which a compact binary inspiral with the given component masses would be detectable given the instrumental PSD. The calculation is defined in Belczynski et. al (2014):

https://dx.doi.org/10.1088/0004-637x/789/2/120

パラメータ:

• psd (~gwpy.frequencyseries.FrequencySeries) -- The instrumental power-spectral-density data.

• snr (float, optional) -- The signal-to-noise ratio for which to calculate range.

• mass1 (float, ~astropy.units.Quantity, optional) -- The mass of the first binary component (float assumed in solar masses).

• mass2 (float, ~astropy.units.Quantity, optional) -- The mass of the second binary component (float assumed in solar masses).

• horizon (bool, optional) -- If True, return the maximal 'horizon' luminosity distance, otherwise return the angle-averaged comoving distance.

• **kwargs -- Additional keyword arguments to ~inspiral_range.waveform.CBCWaveform.

戻り値:

rspec -- The calculated inspiral sensitivity PSD [Mpc^2 / Hz].

戻り値の型:

~gwpy.frequencyseries.FrequencySeries

参考

sensemon_range_psd

For the method based on LIGO-T030276, also known as LIGO SenseMonitor.

inspiral-range

The package which does heavy lifting for waveform simulation and cosmology calculations.

gwexpy.astro.range_spectrogram(hoft: TimeSeries | Spectrogram, stride: float | None = None, fftlength: float | None = None, overlap: float | None = None, window: str | numpy.ndarray = 'hann', method: str = 'median', nproc: int = 1, range_func: Callable | None = None, **rangekwargs) → Spectrogram

Calculate the average range spectrogram (Mpc or Mpc^2 / Hz) from strain.

パラメータ:

• hoft (~gwpy.timeseries.TimeSeries or ~gwpy.spectrogram.Spectrogram) -- record of gravitational-wave strain output from a detector

• stride (float, optional) -- number of seconds in a single PSD (i.e., step size of spectrogram), required if hoft is an instance of TimeSeries

• fftlength (float, optional) -- number of seconds in a single FFT

• overlap (float, optional) -- number of seconds of overlap between FFTs, defaults to the recommended overlap for the given window (if given), or 0

• window (str, numpy.ndarray, optional) -- window function to apply to timeseries prior to FFT, see scipy.signal.get_window() for details on acceptable formats

• method (str, optional) -- FFT-averaging method, defaults to median averaging, see spectrogram() for more details

• nproc (int, optional) -- number of CPUs to use in parallel processing of FFTs, default: 1

• fmin (float, optional) -- low frequency cut-off (Hz), defaults to 1/fftlength

• fmax (float, optional) -- high frequency cut-off (Hz), defaults to Nyquist frequency of hoft

• range_func (callable, optional) -- the function to call to generate the range for each stride, defaults to inspiral_range unless energy is given as a keyword argument to the range function

• **rangekwargs (dict, optional) -- additional keyword arguments to burst_range_spectrum() or inspiral_range_psd() (see "Notes" below), defaults to inspiral range with mass1 = mass2 = 1.4 solar masses

戻り値:

out -- time-frequency spectrogram of astrophysical range

戻り値の型:

~gwpy.spectrogram.Spectrogram

メモ

This method is designed to show the contribution to a gravitational-wave detector's sensitive range across frequency bins as a function of time. It supports the range to compact binary inspirals and to unmodelled GW bursts, each a class of transient event.

If inspiral range is requested and fmax exceeds the frequency of the innermost stable circular orbit (ISCO), the output will extend only up to the latter.

参考

gwpy.timeseries.TimeSeries.spectrogram

for the underlying power spectral density estimator

inspiral_range_psd

for the function that computes inspiral range integrand

burst_range_spectrum

for the function that computes burst range integrand

range_timeseries

for TimeSeries trends of the astrophysical range

gwexpy.astro.range_timeseries(hoft: TimeSeries | Spectrogram, stride: float | None = None, fftlength: float | None = None, overlap: float | None = None, window: str | numpy.ndarray = 'hann', method: str = 'median', nproc: int = 1, range_func: Callable | None = None, **rangekwargs) → TimeSeries

Estimate timeseries of astrophysical range (Mpc).

パラメータ:

• hoft (~gwpy.timeseries.TimeSeries, ~gwpy.spectrogram.Spectrogram) -- Detector (strain) data from which to estimate range.

• stride (float, optional) -- Desired step size (seconds) of range timeseries, required if hoft is an instance of TimeSeries.

• fftlength (float, optional) -- Number of seconds in a single FFT.

• overlap (float, optional) -- Number of seconds of overlap between FFTs, defaults to the recommended overlap for the given window (if given), or 0.

• window (str, numpy.ndarray, optional) -- Window function to apply to timeseries prior to FFT, see scipy.signal.get_window() for details on acceptable formats.

• method (str, optional) -- FFT-averaging method, defaults to median averaging, see spectrogram() for more details

• nproc (int, optional) -- number of CPUs to use in parallel processing of FFTs, default: 1

• range_func (callable, optional) -- the function to call to generate the range for each stride, defaults to inspiral_range unless energy is given as a keyword argument to the range function

• **rangekwargs (dict, optional) -- additional keyword arguments to burst_range() or inspiral_range() (see "Notes" below), defaults to inspiral range with mass1 = mass2 = 1.4 solar masses

戻り値:

out -- timeseries trends of astrophysical range

戻り値の型:

~gwpy.timeseries.TimeSeries

メモ

This method is designed to quantify a gravitational-wave detector's sensitive range as a function of time. It supports the range to compact binary inspirals and to unmodelled GW bursts, each a class of transient event.

参考

gwpy.timeseries.TimeSeries.spectrogram

for the underlying power spectral density estimator

inspiral_range

for the function that computes inspiral range

burst_range

for the function that computes burst range

range_spectrogram

for a ~gwpy.spectrogram.Spectrogram of the range integrand

gwexpy.astro.sensemon_range(psd: FrequencySeries, snr: float = 8, mass1: float = 1.4, mass2: float = 1.4, fmin: float | None = None, fmax: float | None = None, *, horizon: bool = False) → units.Quantity

Approximate the inspiral sensitive distance from a GW strain PSD.

This method returns the distance (in megaparsecs) to which a compact binary inspiral with the given component masses would be detectable given the instrumental PSD. The calculation is as defined in: LIGO-T030276.

パラメータ:

• psd (~gwpy.frequencyseries.FrequencySeries) -- The instrumental power-spectral-density data

• snr (float, optional) -- The signal-to-noise ratio for which to calculate range.

• mass1 (float, ~astropy.units.Quantity, optional) -- The mass of the first binary component (float assumed in solar masses).

• mass2 (float, ~astropy.units.Quantity, optional) -- The mass of the second binary component (float assumed in solar masses).

• fmin (float, optional) -- The lower frequency cut-off of the integral, default: psd.df.

• fmax (float, optional) -- The maximum frequency limit of the integral, defaults to innermost stable circular orbit (ISCO) frequency

• horizon (bool, optional) -- If True, return the maximal 'horizon' sensitive distance, otherwise return the angle-averaged range.

戻り値:

range -- the calculated inspiral range [Mpc]

戻り値の型:

~astropy.units.Quantity

サンプル

Grab some data for LIGO-Livingston around GW150914 and generate a PSD:

>>> from gwpy.timeseries import TimeSeries
>>> hoft = TimeSeries.fetch_open_data("H1", 1126259446, 1126259478)
>>> hoff = hoft.psd(fftlength=4)

Now we can calculate the sensemon_range():

>>> from gwpy.astro import sensemon_range
>>> r = sensemon_range(hoff, fmin: float = 30)
>>> print(r)
70.4612102889 Mpc

gwexpy.astro.sensemon_range_psd(psd: FrequencySeries, snr: float = 8, mass1: float = 1.4, mass2: float = 1.4, *, horizon: bool = False) → FrequencySeries

Approximate the inspiral sensitive distance PSD from a GW strain PSD.

This method returns the power spectral density (in Mpc**2 / Hz) to which a compact binary inspiral with the given component masses would be detectable given the instrumental PSD. The calculation is defined in: LIGO-T030276.

パラメータ:

• psd (~gwpy.frequencyseries.FrequencySeries) -- The instrumental power-spectral-density data.

• snr (float, optional) -- The signal-to-noise ratio for which to calculate range.

• mass1 (float, ~astropy.units.Quantity, optional) -- The mass of the first binary component (float assumed in solar masses).

• mass2 (float, ~astropy.units.Quantity, optional) -- The mass of the second binary component (float assumed in solar masses).

• horizon (bool, optional) -- If True, return the maximal 'horizon' sensitive distance, otherwise return the angle-averaged range.

戻り値:

rspec -- The calculated inspiral sensitivity PSD [Mpc^2 / Hz].

戻り値の型:

~gwpy.frequencyseries.FrequencySeries