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Table of Contents
Inference of gravitational-wave signals
A Bayesian analysis of a gravitational-wave signal which is not accompanied by electromagnetic signals can be performed within nmma following two main steps:
1) setting up a config.ini file and running the command
nmma_gw_generation config.ini
2) perform the analysis or parameter estimation using:
nmma_gw_analysis <name_of_analysis>_data_dump.pickle
Below, we provide an example of a gravitational-wave inference setup using observational data of GW170817 and another example for an injection based analysis.
Inference of an observed GW signal: GW170817
1) We start to set up a config.ini file and adapt it to our specific case. An example is shown below:
################################################################################
## Data generation arguments
################################################################################
trigger_time = 1187008882.43
################################################################################
## Detector arguments
################################################################################
detectors = [H1, L1, V1]
psd_dict = {H1=data/GW170817/h1_psd.txt, L1=data/GW170817/l1_psd.txt, V1=data/GW170817/v1_psd.txt}
channel_dict = {H1=LOSC-STRAIN, L1=LOSC-STRAIN, V1=LOSC-STRAIN}
data_dict = {H1=data/GW170817/H-H1_LOSC_CLN_16_V1-1187007040-2048.gwf, L1=data/GW170817/L-
L1_LOSC_CLN_16_V1-1187007040-2048.gwf, V1=data/GW170817/V-V1_LOSC_CLN_16_V1-1187007040-2048.gwf}
duration = 128
################################################################################
## Job submission arguments
################################################################################
label = GW170817
outdir = outdir
################################################################################
## Likelihood arguments
################################################################################
distance-marginalization=False
phase-marginalization=False
time-marginalization=False
################################################################################
## Prior arguments
################################################################################
prior-file = GW170817.prior
################################################################################
## Waveform arguments
################################################################################
frequency-domain-source-model = lal_binary_neutron_star
waveform_approximant = IMRPhenomPv2_NRTidalv2
binary-type=BNS
################################################################################
## EOS arguments
################################################################################
with-eos=True
eos-data=./eos/eos_IST_sorted
Neos=9501
eos-weight=./eos/EOS_IST_sorted_weight.dat
The trigger time is the time of the observed event. With regard to detector arguments, one has to specify which detectors should be used. For example, detectors = [H1, L1, V1] stand for LIGO detectors Hanford, Livingston and Virgo. For each detector, the noise power spectral density of gravitational wave detector needs to be provided. Within data_dict, one needs to provide the GW170817 data measured within each detector.
With regard to likelihood arguments, we can specify if want a marginal likelihood that has been integrated over the parameter space, e.g. for distance, phase, or time. The prior file should be tailored to the observed event, in this case GW170817 but also with regard to the GW model that is used for the parameter estimation. The GW model can be specified in waveform_approximant. Here, we use the phenomenological model IMRPhenomPv2_NRTidalv2 for a precessing binary neutron star model.
For inferring the source properties of GW170817, we will sample over a set of EOSs that were computed with Chiral Effective Field Theory. The EOS set 15nsat_cse_natural_R14 was used in the study of Huth et al. and can be downloaded there. In order to make use of the EOS set during the sampling, a pre-routine is required. Within this step, one can include different constraints on the NS EOS such as measurement of NICER or pulsar measurements which is reflected in the EOS_sorted_weight.dat and one needs to sort the EOS files eos_sorted in order to reduce sampling time.
