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

Kapahtia, Akanksha; Chingangbam, Pravabati; Appleby, Stephen

doi:10.1088/1475-7516/2019/09/053

Cited by 37 publications

(28 citation statements)

References 70 publications

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“…stephen.appleby@apctp.org Minkowski tensors Beisbart et al (2001b,a); ; Chingangbam et al (2017); Kapahtia et al (2019); Appleby et al (2018a,b); Kapahtia et al (2018); Joby et al (2019), Betti numbers Park et al (2013); Feldbrugge et al (2019); Pranav et al (2019aPranav et al ( ,b, 2017; Shivshankar et al (2015); van de Weygaert et al (2011) and multi-scale analyses of the cosmic web Sousbie et al (2011); Codis et al (2018); Kraljic et al (2020). Previous application of the Minkowski functionals to various modern data sets can be found in (Park et al 2001;Hikage et al 2002Hikage et al , 2003James et al 2009;Gott et al 2009;Choi et al 2010b;Zhang et al 2010;Petri et al 2013;Blake et al 2014;Wiegand et al 2014;Parihar et al 2014;Wang et al 2015;Wiegand & Eisenstein 2017;Buchert et al 2017;Sullivan et al 2019;Hikage et al 2001;Gott et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Cosmological Parameter Estimation from the Two-dimensional Genus Topology: Measuring the Shape of the Matter Power Spectrum

Appleby

Park

Hong

et al. 2020

ApJ

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We measure the genus of the galaxy distribution in two-dimensional slices of the SDSS-III BOSS catalog to constrain the cosmological parameters governing the expansion history of the Universe. The BOSS catalogs are divided into twelve concentric shells over the redshift range 0.25 < z < 0.6 and we repeatedly measure the genus from the two-dimensional galaxy density fields, each time varying the cosmological parameters used to infer the distance-redshift relation to the shells. We also indirectly reconstruct the two-dimensional genus amplitude using the three-dimensional genus measured from SDSS Main Galaxy Sample with galaxies at low redshift z < 0.12. We combine the low-and highredshift measurements, finding the cosmological model which minimizes the redshift evolution of the genus amplitude, using the fact that this quantity should be conserved. Being a distance measure, the test is sensitive to the matter density parameter (Ω m) and equation of state of dark energy (w de). We find a constraint of w de = −1.05 +0.13 −0.12 , Ω m = 0.303 ± 0.036 after combining the high-and low-redshift measurements and combining with Planck CMB data. Higher redshift data and combining data sets at low redshift will allow for stronger constraints.

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Section: Introductionmentioning

confidence: 99%

Cosmological Parameter Estimation from the Two-dimensional Genus Topology: Measuring the Shape of the Matter Power Spectrum

Appleby

Park

Hong

et al. 2020

ApJ

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“…There are a number of complementary methods which deal with the signal in real space and have been employed directly on the simulated tomographic images to probe the morphology of the 21-cm field and its evolution during the EoR through the analysis of topology and geometry of this field. Among them, the widely used methods are the Minkowski Functionals (MFs) (Friedrich et al 2011;Hong et al 2014;Yoshiura et al 2017;Bag et al 2018Bag et al , 2019 which have been used to track the reionization history, the Minkowski tensors (Kapahtia et al 2019) which are the generalized tensorial form of MFs and can encapsulate the direction information. These are also methods based on percolation theory (Iliev et al 2006;Iliev et al 2014;Furlanetto & Oh 2016;Bag et al 2018Bag et al , 2019, granulometry (Kakiichi et al 2017) and persistence theory (Elbers & van de Weygaert 2019) which have been used for the theoretical study of the topological phases of H regions during EoR.…”

Section: Introductionmentioning

confidence: 99%

Distinguishing reionization models using the largest cluster statistics of the 21-cm maps

Aadarsh¹,

Bag²,

Majumdar³

et al. 2022

Preprint

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The evolution of topology and morphology of ionized or neutral hydrogen during different stages of the Epoch of Reionization (EoR) have the potential to provide us a great amount of information about the properties of the ionizing sources during this era. We compare a variety of reionization source models in terms of the geometrical properties of the ionized regions. We show that the percolation transition in the ionized hydrogen, as studied by tracing the evolution of the Largest Cluster Statistics (LCS), is a robust statistic that can distinguish the fundamentally different scenarios -inside-out and outside-in reionization. Particularly, the global neutral fraction at the onset of percolation is significantly higher for the inside-out scenario as compared to that for the outside-in reionization. In complementary to percolation analysis, we explore the shape and morphology of the ionized regions as they evolve in different reionization models in terms of the Shapefinders (SFs) that are ratios of the Minkowski functionals (MFs). The shape distribution can readily discern the reionization scenario with extreme non-uniform recombination in the IGM, such as the clumping model. In the rest of the reionization models, the largest ionized region abruptly grows only in terms of its third SF -'length' -during percolation while the first two SFs -'thickness' and 'breadth' -remain stable. Thus the ionized hydrogen in these scenarios becomes highly filamentary near percolation and exhibit a 'characteristic cross-section' that varies among the source models. Therefore, the geometrical studies based on SFs, together with the percolation analysis can shed light on the reionization sources.

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“…They have a long and venerable history within cosmology, both theoretical and computational, as well as observational, starting with the genus of isodensity excursion sets (Gott et al 1990;Park & Gott 1991;Mecke et al 1994;Schmalzing & Gorski 1998;Melott et al 1989;Park et al 1992Park et al , 2001Zunckel et al 2011). Often referred to merely as summary statistics in cosmological literature, they emerge from topo-geometrical description of space and manifolds, and together with the homology characteristics encoded in the Betti numbers (Park et al 2013;Feldbrugge et al 2019;Pranav et al 2019aPranav et al ,b, 2017Shivshankar et al 2015;van de Weygaert et al 2011), and its hierarchical extension persistent homology (Edelsbrunner & Harer 2010;Pranav et al 2017), as well as the Minkowski tensors (Beisbart et al 2001b,a;Ganesan & Chingangbam 2017;Chingangbam et al 2017a,b;Kapahtia et al 2019;Appleby et al 2018a,b;Kapahtia et al 2018;Joby et al 2019;Wilding et al 2020;Chingangbam et al 2021), present a high-level description of the topo-geometrical properties of the fields of interest in cosmology. Extracting information from these statistics remains an open and challenging program (Park et al 2001;Hikage et al 2002Hikage et al , 2003Park et al 2005;James et al 2009;Sheth et al 2003;Sheth & Sahni 2005;Gott et al 2009;Choi et al 2010;…”

Section: Introductionmentioning

confidence: 99%

Minkowski Functionals of SDSS-III BOSS : Hints of Possible Anisotropy in the Density Field?

Appleby,

Park,

Pranav

et al. 2021

Preprint

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We present measurements of the Minkowski functionals extracted from the SDSS-III BOSS catalogs. After defining the Minkowski functionals, we describe how an unbiased reconstruction of these statistics can be obtained from a field with masked regions and survey boundaries, validating our methodology with Gaussian random fields and mock galaxy snapshot data. From the BOSS galaxy data we generate a set of four density fields in three dimensions corresponding to the northern and southern skies of LOWZ and CMASS catalogs, smoothing over large scales such that the field is perturbatively non-Gaussian. We extract the Minkowski functionals from each data set separately, and measure their shapes and amplitudes by fitting a Hermite polynomial expansion. For the shape parameter of the Minkowski functional curves a 0 , that is related to the bispectrum of the field, we find that the LOWZ-South data presents a systematically lower value of a 0 = −0.080 ± 0.040 than its northern sky counterpart a 0 = 0.032 ± 0.024. Although the significance of this discrepancy is low, it potentially indicates some systematics in the data or that the matter density field exhibits anisotropy at low redshift. By assuming a standard isotropic flat ΛCDM cosmology, the amplitudes of Minkowski functionals from the combination of northern and southern sky data give the constraints Ω c h 2 n s = 0.110 ± 0.006 and 0.111 ± 0.008 for CMASS and LOWZ, respectively, which is in agreement with the Planck ΛCDM best-fit Ω c h 2 n s = 0.116 ± 0.001.

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

Cited by 37 publications

References 70 publications

Cosmological Parameter Estimation from the Two-dimensional Genus Topology: Measuring the Shape of the Matter Power Spectrum

Cosmological Parameter Estimation from the Two-dimensional Genus Topology: Measuring the Shape of the Matter Power Spectrum

Distinguishing reionization models using the largest cluster statistics of the 21-cm maps

Minkowski Functionals of SDSS-III BOSS : Hints of Possible Anisotropy in the Density Field?

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