Journal article Open Access

Interplay of spin-precession and higher harmonics in the parameter estimation of binary black holes

Krishnendu N. V.; Frank Ohme


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  <dc:creator>Krishnendu N. V.</dc:creator>
  <dc:creator>Frank Ohme</dc:creator>
  <dc:date>2022-03-07</dc:date>
  <dc:description>Welcome to the data release of our recent paper titled "The interplay of spin-precession and higher harmonics in the parameter estimation of binary black holes".
We provide all the posterior samples used to make different figures/conclusions that went into the paper. 
For any clarifications regarding the data structure please write to us at krnava@aei.mpg.de or at frank.ohme@ligo.org
Thank you!

Description

We provide a brief description of each folder.  As we discuss in detail in the papers, we study the measurability of spin-induced orbital precession in generic binary systems, employing two waveform models IMRPhenomPv3HM and IMRPhenomPv3. The parameters are estimated using the gravitational-wave data analysis toolkit parallel Bilby.  Our injections are assuming the binary produced fixed signal-to-noise ratio in the three detector network consisting of two LIGO and one Virgo detector at their design sensitivities.


	General convention followed for directory naming: `chi_1` highly precessing system and `chi_2` slowly precessing system. `q1`, `q3` and `q7` correspond to three different mass ratios considered (maps to inverse mass ratios, 1/q=1, 3, 7) at a fixed total mass 40Msun. Finally, `theta_JN_0` represents a face-on system and `theta_JN_piby2` represents an edge-on binary.
	For example, `chip_1_q1_theta_JN_0` means a highly precessing equal mass binary with face-on orientation.
	Regarding different types of runs:
	
		  `0noise_fixed_snr30` contains injections at a fixed signal-to-noise ratio of 30 and `0noise_fixed_snr30` contains injections at a fixed signal-to-noise ratio of 60.
		 `0noise_fixed_snr30` contains `PhenomPv3HM_inj` and `PhenomPv3_inj`.  `PhenomPv3HM_inj` (`PhenomPv3_inj`) is the case where IMRPhenomPv3HM (IMRPhenomPv3) waveform model is used.  
		Data files, `PhenomPv3HM_pesummary.dat` means IMRPhenomPv3HM is employed as the recovery model and `PhenomPv3_pesummary.dat ` means IMRPhenomPv3 is employed as the recovery model.  These files contain the posterior distributions on each of the binary parameters.
		We provide the injection parameters inside each directory, `inj.pkl`. 
	
	
</dc:description>
  <dc:identifier>https://zenodo.org/record/6337692</dc:identifier>
  <dc:identifier>10.1103/PhysRevD.105.064012</dc:identifier>
  <dc:identifier>oai:zenodo.org:6337692</dc:identifier>
  <dc:language>eng</dc:language>
  <dc:rights>info:eu-repo/semantics/openAccess</dc:rights>
  <dc:rights>https://creativecommons.org/licenses/by/4.0/legalcode</dc:rights>
  <dc:source>Phys. Rev. D 105(064012)</dc:source>
  <dc:subject>Gravitational waves, binary black holes</dc:subject>
  <dc:title>Interplay of spin-precession and higher harmonics in the parameter estimation of binary black holes</dc:title>
  <dc:type>info:eu-repo/semantics/article</dc:type>
  <dc:type>publication-article</dc:type>
</oai_dc:dc>
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