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            <title xml:lang="en">Measuring the growth of matter fluctuations with third-order galaxy correlations</title>
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                <forename type="first">Kai</forename>
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                <forename type="first">Julien</forename>
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                <forename type="first">Francisco J.</forename>
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                <forename>Christian</forename>
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              <date type="whenSubmitted">2016-03-14 17:25:39</date>
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            <idno type="halRefHtml">&lt;i&gt;Monthly Notices of the Royal Astronomical Society&lt;/i&gt;, 2015, 447 (2), pp.1724-1745. &lt;a target="_blank" href="https://dx.doi.org/10.1093/mnras/stu2492"&gt;&amp;#x27E8;10.1093/mnras/stu2492&amp;#x27E9;&lt;/a&gt;</idno>
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            <idno type="stamp" n="UNIV-TLN">Université de Toulon</idno>
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            <idno type="stamp" n="UNIV-AMU">Aix Marseille Université</idno>
            <idno type="stamp" n="CPT">Centre de Physique Théorique</idno>
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                <title xml:lang="en">Measuring the growth of matter fluctuations with third-order galaxy correlations</title>
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                    <forename type="first">Enrique</forename>
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                    <forename type="first">Martin</forename>
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                    <forename type="first">Pablo</forename>
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                    <forename type="first">Francisco J.</forename>
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              <p>Measurements of the linear growth factor $D$ at different redshifts $z$ are key to distinguish among cosmological models. One can estimate the derivative $dD(z)/d\ln(1+z)$ from redshift space measurements of the 3D anisotropic galaxy two-point correlation $\xi(z)$, but the degeneracy of its transverse (or projected) component with galaxy bias $b$, i.e. $\xi_{\perp}(z) \propto\ D^2(z) b^2(z)$, introduces large errors in the growth measurement. Here we present a comparison between two methods which break this degeneracy by combining second- and third-order statistics. One uses the shape of the reduced three-point correlation and the other a combination of third-order one- and two-point cumulants. These methods use the fact that, for Gaussian initial conditions and scales larger than $20$ $h^{-1}$Mpc, the reduced third-order matter correlations are independent of redshift (and therefore of the growth factor) while the third-order galaxy correlations depend on $b$. We use matter and halo catalogs from the MICE-GC simulation to test how well we can recover $b(z)$ and therefore $D(z)$ with these methods in 3D real space. We also present a new approach, which enables us to measure $D$ directly from the redshift evolution of second- and third-order galaxy correlations without the need of modelling matter correlations. For haloes with masses lower than $10^{14}$ $h^{-1}$M$_\odot$, we find $10%$ deviations between the different estimates of $D$, which are comparable to current observational errors. At higher masses we find larger differences that can probably be attributed to the breakdown of the bias model and non-Poissonian shot noise.</p>
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