English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We use morphological descriptors, Betti numbers and Contour Minkowski Tensor(CMT) on 21cm brightness temperature excursion sets, to study the ionizationand heating history of the intergalactic medium (IGM) during and before theEpoch of Reionization (EoR). The ratio of eigenvalues of the CMT denoted by$\beta$, gives shape information while it's trace gives the contour length ofholes and connected regions. We simulate the matter density, neutral hydrogenfraction, spin temperature and brightness temperature field using the publiclyavailable code 21cmFAST in a redshift range of $z=20.22$ to $z=6$. We study theredshift evolution of three quantities - the Betti number counts$N_{con,hole}$, the characteristic size $r^{ch}_{con,hole}$ and shapeanisotropy parameter $\beta^{ch}_{con,hole}$ of connected regions and holes forthese fields and investigate the different physical origins of their evolution.We make a qualitative comparison of different models of heating and ionizationduring the EoR. We obtain different regimes of morphological evolution ofbrightness temperature, depending upon how the shapes and sizes of connectedregions and holes change with redshift for different astrophysical settingsaffecting the ionization and heating history of the IGM during and before theEoR. We find that the morphology of the brightness temperature field traces themorphology of ionized regions below a certain redshift value depending upon themodel, where $\Delta r^{ch}_{hole}<10 \%$ and $\Delta \beta^{ch}_{hole}<1 \%$relative to the $x_{HI}$ field. This difference decreases with redshift.Therefore, the ionization history of the IGM can be reconstructed using themorphological description of $\delta T_b$ in real space.

Morphology of 21cm brightness temperature during the Epoch of Reioinization using Contour Minkowski Tensor