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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    <subfield code="a">Frank Ohme</subfield>
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    <subfield code="p">Phys. Rev. D</subfield>
    <subfield code="n">064012</subfield>
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    <subfield code="u">Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Callinstr. 38, D-30167 Hannover, Germany and Leibniz Universitat Hannover, D-30167 Hannover, Germany</subfield>
    <subfield code="0">(orcid)0000-0002-3483-7517</subfield>
    <subfield code="a">Krishnendu N. V.</subfield>
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    <subfield code="a">Interplay of spin-precession and higher harmonics in the parameter estimation of binary black holes</subfield>
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    <subfield code="a">Creative Commons Attribution 4.0 International</subfield>
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    <subfield code="a">&lt;p&gt;Welcome to the data release of our recent paper titled &amp;quot;The interplay of spin-precession and higher harmonics in the parameter estimation of binary black holes&amp;quot;.&lt;br&gt;
We provide all the posterior samples used to make different figures/conclusions that went into the &lt;a href="https://arxiv.org/abs/2110.00766"&gt;paper&lt;/a&gt;.&amp;nbsp;&lt;br&gt;
For any clarifications regarding the data structure please write to us at krnava@aei.mpg.de or at frank.ohme@ligo.org&lt;br&gt;
Thank you!&lt;/p&gt;

&lt;p&gt;&lt;strong&gt;Description&lt;/strong&gt;&lt;/p&gt;

&lt;p&gt;We provide a brief description of each folder. &amp;nbsp;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. &amp;nbsp;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.&lt;/p&gt;

&lt;ul&gt;
	&lt;li&gt;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.&lt;/li&gt;
	&lt;li&gt;For example, `chip_1_q1_theta_JN_0` means a highly precessing equal mass binary with face-on orientation.&lt;/li&gt;
	&lt;li&gt;Regarding different types of runs:
	&lt;ul&gt;
		&lt;li&gt;&amp;nbsp;&amp;nbsp;`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.&lt;/li&gt;
		&lt;li&gt;&amp;nbsp;`0noise_fixed_snr30` contains `PhenomPv3HM_inj` and `PhenomPv3_inj`. &amp;nbsp;`PhenomPv3HM_inj` (`PhenomPv3_inj`) is the case where IMRPhenomPv3HM (IMRPhenomPv3) waveform model is used.&amp;nbsp;&amp;nbsp;&lt;/li&gt;
		&lt;li&gt;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. &amp;nbsp;These files contain the posterior distributions on each of the binary parameters.&lt;/li&gt;
		&lt;li&gt;We provide the injection parameters inside each directory, `inj.pkl`.&amp;nbsp;&lt;/li&gt;
	&lt;/ul&gt;
	&lt;/li&gt;
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    <subfield code="a">10.1103/PhysRevD.105.064012</subfield>
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