This article has been reviewed according to Science X's editorial process and policies. Editors have highlighted the following attributes while ensuring the content's credibility:

fact-checked

preprint

proofread

Using dark matter distribution to test the cosmological model

Using dark matter distribution to test the cosmological model
The Subaru HSC image. Credit: HSC-SSP project & NAOJ

An international team of astrophysicists and cosmologists at various institutes including the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU) have submitted a set of five papers, measuring a value for the "clumpiness" of the universe's dark matter, known to cosmologists as S8, of 0.76, which aligns with values that other gravitational lensing surveys have found in looking at the relatively recent universe, but it does not align with the value of 0.83 derived from the cosmic microwave background, which dates back to the universe's origins when the universe was about 380,000 years old. Their results were uploaded to the arXiv pre-print server as a set of five papers on April 3.

The gap between these two values is small, but as more and more studies confirm each of the two values, it doesn't appear to be accidental. The possibilities are that there's some as-yet unrecognized error or mistake in one of these two measurements or the standard cosmological model is incomplete in some interesting way.

Dark energy and make up 95% of our we see today, but we understand very little about what they actually are and how they've evolved over the history of the universe. Clumps of dark matter distort the light of distant galaxies through weak gravitational lensing, a phenomenon predicted by Einstein's general theory of relativity.

"This distortion is a really, really small effect. The shape of a single galaxy is distorted by an imperceptible amount. But combining the measurements for millions of galaxies allows one to measure the distortion with quite high precision," said Kavli IPMU Professor Masahiro Takada.

The is defined by only a handful of numbers: the expansion rate of the universe, a measure of how clumpy the dark matter is (S8), the relative contributions of the constituents of the universe (matter, dark matter, and ), the overall density of the universe, and a technical quantity describing how the clumpiness of the universe on large scales relates to that on small scales.

Cosmologists are eager to test this model by constraining these numbers in various ways, such as by observing the fluctuations in the , modeling the expansion history of the universe, or measuring the clumpiness of the universe in the relatively recent past.

A team led by astronomers from Kavli IPMU, the University of Tokyo, Nagoya University, Princeton University, and astronomical communities of Japan and Taiwan, have spent the past year teasing out the secrets of this most elusive material, dark matter, using sophisticated computer simulations and data from the first three years of the Hyper Suprime-Cam survey. The observations from this survey used one of the most powerful astronomical cameras in the world, the Hyper Suprime-Cam (HSC) mounted on the Subaru Telescope on the summit of Maunakea in Hawaii.

Using dark matter distribution to test the cosmological model
The measurement results of S8 parameter from Subaru Hyper Suprime-Cam (HSC) Year 3 data. Here we show the results from the four methods, which are different in the sense that the methods used the different parts of the HSC Year 3 data or combined the HSC Year 3 data with other data. For comparison, "Planck CMB" shows the measurement result of S8 from the cosmic microwave background data from Planck satellite. "Other weak lensing results" show the result from the similar weak lensing measurements based on the US-led Dark Energy Survey (DES) or the Europe-led Kilo-Degree Survey (KiDS) data. Credit: Kavli IPMU

Hiding and uncovering the data

"Scientists are human beings, and they do have preferences. Some would love to really find something fundamentally new, while others might feel comfortable if they find results that look consistent with foreseen results. Scientists have become self-aware enough to know that they will bias themselves, no matter how careful they are, unless they carry out their analysis without allowing themselves to know the results until the end," said Nagoya University Kobayashi-Maskawa Institute for the Origin of Particles and the Universe (KMI) Associate Professor Hironao Miyatake.

To protect the results from such biases, the HSC team hid their results from themselves and their colleagues for months, effectively performing a "blinded analysis." The team even added an extra obfuscating layer: they ran their analyses on three different galactic catalogs, one real and two fake with numerical values offset by random values. The analysis team didn't know which of them was real, so even if someone did accidentally see the values, the team wouldn't know if the results were based on the real catalog or not.

The team spent a year on the blind analysis. On December 3, 2022, the team gathered together on Zoom—one Saturday morning in Japan, Friday evening in Princeton—for the "unblinding." The team unveiled the data, and ran their plots, immediately they saw it was great according to Takada.

"Blinded analysis means you cannot take a peak at the results while running the analysis, which was extremely stressful, but as soon I saw the final result, all of that anxiety flew out of the window," said Kavli IPMU graduate student Sunao Sugiyama.

A huge survey with the world's largest telescope camera

HSC is the largest camera on a telescope of its size in the world. The survey that the research team used covers about 420 square degrees of the sky, about the equivalent of 2,000 full moons. It is not a single contiguous chunk of sky, but split among six different pieces, each about the size of a person's outstretched fist. The 25 million galaxies the researchers surveyed are so distant that instead of seeing these galaxies as they are today, the HSC recorded how they were billions of years ago.

Each of these galaxies glows with the fires of tens of billions of suns, but because they are so far away, they are extremely faint, as much as 25 million times fainter than the faintest stars we can see with the naked eye.

More information: Hironao Miyatake et al, Hyper Suprime-Cam Year 3 Results: Cosmology from Galaxy Clustering and Weak Lensing with HSC and SDSS using the Emulator Based Halo Model. arxiv.org/abs/2304.00704

Surhud More et al, Hyper Suprime-Cam Year 3 Results: Measurements of Clustering of SDSS-BOSS Galaxies, Galaxy-Galaxy Lensing and Cosmic Shear. arxiv.org/abs/2304.00703

Sunao Sugiyama et al, Hyper Suprime-Cam Year 3 Results: Cosmology from Galaxy Clustering and Weak Lensing with HSC and SDSS using the Minimal Bias Model. arxiv.org/abs/2304.00705

Roohi Dalal et al, Hyper Suprime-Cam Year 3 Results: Cosmology from Cosmic Shear Power Spectra. arxiv.org/abs/2304.00701

Xiangchong Li et al, Hyper Suprime-Cam Year 3 Results: Cosmology from Cosmic Shear Two-point Correlation Functions. arxiv.org/abs/2304.00702

Journal information: arXiv

Provided by Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU)

Citation: Using dark matter distribution to test the cosmological model (2023, April 4) retrieved 20 May 2024 from https://phys.org/news/2023-04-dark-cosmological.html
This document is subject to copyright. Apart from any fair dealing for the purpose of private study or research, no part may be reproduced without the written permission. The content is provided for information purposes only.

Explore further

Using the shadows of clusters to measure the universe

58 shares

Feedback to editors