宇宙的重量

宇宙的重量

Bochum cosmologists headed by Professor Hendrik Hildebrandt have gained new insights into the density and structure of matter in the universe. Several years ago, Hildebrandt had already been involved in a research consortium that had pointed out discrepancies in the data between different groups. The values determined for matter density and structure differed depending on the measurement method. A new analysis, which included additional infrared data, made the differences stand out even more. They could indicate that this is the flaw in the Standard Model of Cosmology.

以亨德里克·希尔德布兰特教授为首的波鸿宇宙学家，对宇宙中物质的密度和结构有了新的见解。几年前，希尔德布兰已经参与了一个研究小组，指出了不同群体之间的数据差异。物质密度和结构的测定值因测量方法而异。一项新的分析，包括额外的红外数据，使差异更加突出。它们可能表明这是宇宙学标准模型的缺陷。

Rubin, the science magazine of Ruhr-Universität Bochum, has published a report on Hendrik Hildebrandt's research. The latest analysis of the research consortium, called Kilo-Degree Survey, was published in the journal Astronomy and Astrophysics in January 2020.

鲁尔波鸿大学的科学杂志《鲁宾》发表了一篇关于亨德里克希尔德布兰特研究的报告。该研究联盟的最新分析称为千度调查，于2020年1月发表在《天文学和天体物理学》杂志上。

Two methods for determining the structure of matter

确定物质结构的两种方法

Research teams can calculate the density and structure of matter based on the cosmic microwave background, a radiation that was emitted shortly after the Big Bang and can still be measured today. This is the method used by the Planck Research Consortium.

研究小组可以根据宇宙微波背景来计算物质的密度和结构，宇宙微波背景是大爆炸后不久发射的一种辐射，如今仍然可以测量。这是普朗克研究协会使用的方法。

The Kilo-Degree Survey team, as well as several other groups, determined the density and structure of matter using the gravitational lensing effect: as high-mass objects deflect light from galaxies, these galaxies appear in a distorted form in a different location than they actually are when viewed from Earth. Based on these distortions, cosmologists can deduce the mass of the deflecting objects and thus the total mass of the universe. In order to do so, however, they need to know the distances between the light source, the deflecting object and the observer, among other things. The researchers determine these distances with the help of redshift, which means that the light of distant galaxies arrives on Earth shifted into the red range.

千度调查小组以及其他几个小组使用引力透镜效应确定了物质的密度和结构：当高质量物体使光线偏离星系时，这些星系在一个不同的位置呈现出扭曲的形状，而从地球上看它们实际上是不同的。基于这些扭曲，宇宙学家可以推断出偏转物体的质量，从而推断出宇宙的总质量。然而，为了做到这一点，他们需要知道光源、偏转物体和观察者之间的距离等。研究人员通过红移来确定这些距离，这意味着遥远星系的光到达地球后就转移到了红色范围内。

New calibration using infrared data

利用红外数据进行校准的新方法

To determine distances, cosmologists therefore take images of galaxies at different wavelengths, for example one in the blue, one in the green and one in the red range; they then determine the brightness of the galaxies in the individual images. Hendrik Hildebrandt and his team also include several images from the infrared range in order to determine the distance more precisely.

因此，为了确定距离，宇宙学家拍摄了不同波长的星系图像，例如一个在蓝色范围内，一个在绿色范围内，一个在红色范围内;然后他们在单个图像中确定星系的亮度。亨德里克希尔德布兰特和他的团队还包括一些来自红外范围的图像，以便更精确地确定距离。

Previous analyses had already shown that the microwave background data from the Planck Consortium systematically deviate from the gravitational lensing effect data. Depending on the data set, the deviation was more or less pronounced; it was most pronounced in the Kilo-Degree Survey. "Our data set is the only one based on the gravitational lensing effect and calibrated with additional infrared data," says Hendrik Hildebrandt, Heisenberg professor and head of the RUB research group Observational Cosmology in Bochum. "This could be the reason for the greater deviation from the Planck data."

先前的分析已经表明，普朗克财团的微波背景数据系统地偏离了引力透镜效应数据。根据数据集的不同，这种偏差多少有点明显;在千度调查中最为明显。”我们的数据集是唯一一个基于引力透镜效应并用额外红外数据校准的数据集，”海森堡教授、波鸿RUB观测宇宙学研究小组负责人亨德里克·希尔德布兰特说“这可能是与普朗克数据偏差较大的原因。”

To verify this discrepancy, the group evaluated the data set of another research consortium, the Dark Energy Survey, using a similar calibration. As a result, these values also deviated even more strongly from the Planck values.

为了验证这一差异，研究小组使用类似的校准方法对另一个研究联盟暗能量调查的数据集进行了评估。因此，这些值与普朗克值的偏差也更大。