Minkowski Tensors in Two Dimensions: Probing the Morphology and Isotropy of the Matter and Galaxy Density Fields

作者：Appleby Stephen; Chingangbam Pravabati; Park Changbom; Hong Sungwook E; Kim Juhan; Ganesan Vidhya

来源：Astrophysical Journal, 2018, 858(2): 87.

DOI：10.3847/1538-4357/aabb53

<jats:title>Abstract</jats:title>
<jats:p>We apply the Minkowski tensor statistics to two-dimensional slices of the three-dimensional matter density field. The Minkowski tensors are a set of functions that are sensitive to directionally dependent signals in the data and, furthermore, can be used to quantify the mean shape of density fields. We begin by reviewing the definition of Minkowski tensors and introducing a method of calculating them from a discretely sampled field. Focusing on the statistic <jats:inline-formula>
<jats:tex-math>
<?CDATA ${W}_{2}^{1,1}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaabb53ieqn1.gif" xlink:type="simple" />
</jats:inline-formula>—a 2 × 2 matrix—we calculate its value for both the entire excursion set and individual connected regions and holes within the set. To study the morphology of structures within the excursion set, we calculate the eigenvalues <jats:italic>λ</jats:italic>
<jats:sub>1</jats:sub>, <jats:italic>λ</jats:italic>
<jats:sub>2</jats:sub> for the matrix <jats:inline-formula>
<jats:tex-math>
<?CDATA ${W}_{2}^{1,1}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaabb53ieqn2.gif" xlink:type="simple" />
</jats:inline-formula> of each distinct connected region and hole and measure their mean shape using the ratio <jats:inline-formula>
<jats:tex-math>
<?CDATA $\beta \equiv \langle {\lambda }_{2}/{\lambda }_{1}\rangle $?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaabb53ieqn3.gif" xlink:type="simple" />
</jats:inline-formula>. We compare both <jats:inline-formula>
<jats:tex-math>
<?CDATA ${W}_{2}^{1,1}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaabb53ieqn4.gif" xlink:type="simple" />
</jats:inline-formula> and <jats:italic>β</jats:italic> for a Gaussian field and a smoothed density field generated from the latest Horizon Run 4 cosmological simulation to study the effect of gravitational collapse on these functions. The global statistic <jats:inline-formula>
<jats:tex-math>
<?CDATA ${W}_{2}^{1,1}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaabb53ieqn5.gif" xlink:type="simple" />
</jats:inline-formula> is essentially independent of gravitational collapse, as the process maintains statistical isotropy. However, <jats:italic>β</jats:italic> is modified significantly, with overdensities becoming relatively more circular compared to underdensities at low redshifts. When applying the statistics to a redshift-space distorted density field, the matrix <jats:inline-formula>
<jats:tex-math>
<?CDATA ${W}_{2}^{1,1}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaabb53ieqn6.gif" xlink:type="simple" />
</jats:inline-formula> is no longer proportional to the identity matrix, and measurements of its diagonal elements can be used to probe the large-scale velocity field.</jats:p>

• 出版日期2018-5-10