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·希爾德布蘭特教授為首的波鴻宇宙學(xué)家，對(duì)宇宙中物質(zhì)的密度和結(jié)構(gòu)有了新的見解。幾年前，希爾德布蘭已經(jīng)參與了一個(gè)研究小組，指出了不同群體之間的數(shù)據(jù)差異。物質(zhì)密度和結(jié)構(gòu)的測(cè)定值因測(cè)量方法而異。一項(xiàng)新的分析，包括額外的紅外數(shù)據(jù)，使差異更加突出。它們可能表明這是宇宙學(xué)標(biāo)準(zhǔn)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.

魯爾波鴻大學(xué)的科學(xué)雜志《魯賓》發(fā)表了一篇關(guān)于亨德里克希爾德布蘭特研究的報(bào)告。該研究聯(lián)盟的最新分析稱為千度調(diào)查，于2020年1月發(fā)表在《天文學(xué)和天體物理學(xué)》雜志上。

Two methods for determining the structure of matter

確定物質(zhì)結(jié)構(gòu)的兩種方法

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.

研究小組可以根據(jù)宇宙微波背景來(lái)計(jì)算物質(zhì)的密度和結(jié)構(gòu)，宇宙微波背景是大爆炸后不久發(fā)射的一種輻射，如今仍然可以測(cè)量。這是普朗克研究協(xié)會(huì)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.

千度調(diào)查小組以及其他幾個(gè)小組使用引力透鏡效應(yīng)確定了物質(zhì)的密度和結(jié)構(gòu)：當(dāng)高質(zhì)量物體使光線偏離星系時(shí)，這些星系在一個(gè)不同的位置呈現(xiàn)出扭曲的形狀，而從地球上看它們實(shí)際上是不同的?；谶@些扭曲，宇宙學(xué)家可以推斷出偏轉(zhuǎn)物體的質(zhì)量，從而推斷出宇宙的總質(zhì)量。然而，為了做到這一點(diǎn)，他們需要知道光源、偏轉(zhuǎn)物體和觀察者之間的距離等。研究人員通過(guò)紅移來(lái)確定這些距離，這意味著遙遠(yuǎn)星系的光到達(dá)地球后就轉(zhuǎn)移到了紅色范圍內(nèi)。

New calibration using infrared data

利用紅外數(shù)據(jù)進(jìn)行校準(zhǔn)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，為了確定距離，宇宙學(xué)家拍攝了不同波長(zhǎng)的星系圖像，例如一個(gè)在藍(lán)色范圍內(nèi)，一個(gè)在綠色范圍內(nèi)，一個(gè)在紅色范圍內(nèi);然后他們?cè)趩蝹€(gè)圖像中確定星系的亮度。亨德里克希爾德布蘭特和他的團(tuán)隊(duì)還包括一些來(lái)自紅外范圍的圖像，以便更精確地確定距離。

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."

先前的分析已經(jīng)表明，普朗克財(cái)團(tuán)的微波背景數(shù)據(jù)系統(tǒng)地偏離了引力透鏡效應(yīng)數(shù)據(jù)。根據(jù)數(shù)據(jù)集的不同，這種偏差多少有點(diǎn)明顯;在千度調(diào)查中最為明顯。”我們的數(shù)據(jù)集是唯一一個(gè)基于引力透鏡效應(yīng)并用額外紅外數(shù)據(jù)校準(zhǔn)的數(shù)據(jù)集，”海森堡教授、波鴻RUB觀測(cè)宇宙學(xué)研究小組負(fù)責(zé)人亨德里克·希爾德布蘭特說(shuō)“這可能是與普朗克數(shù)據(jù)偏差較大的原因。”

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.

為了驗(yàn)證這一差異，研究小組使用類似的校準(zhǔn)方法對(duì)另一個(gè)研究聯(lián)盟暗能量調(diào)查的數(shù)據(jù)集進(jìn)行了評(píng)估。因此，這些值與普朗克值的偏差也更大。