In the last decades, telescopes have been able to observe the skies with unprecedented precision and sensitivity.
Our research team on the South Pole Telescope is studying how the Universe evolved and has changed over time. We have just released two years' worth of mapping of the infant universe over 1/25th of the sky.
These observations have sharpened our understanding of the nature of dark energy and the rate at which the universe is expanding.
But more on that later, first we'll look at what we currently understand about the Universe...
It describes the first stage of our universe as a primordial fireball composed of a very hot plasma, much like our Sun.
The Big Bang started around 13.8 billion years ago when a phenomenon known as Cosmic Inflation caused the Universe to expand at a rate faster than the speed of light for a fraction of a second.
As the Universe expanded and cooled after inflation, the ordinary matter (the type we can see and interact with) looked very much like our Sun, a super-heated plasma made up of photons, electrons and ionised (or charged) hydrogen and helium nuclei.
Modern telescopes can detect faint radiation from 400,000 years after the Big Bang, known as the Cosmic Microwave Background (CMB). The CMB is a snapshot of the plasma and conditions at that time, when the plasma's temperature had cooled to about half that of the Sun.
This cooling allowed the plasma to recombine, forming atoms like hydrogen and helium. At the time of the CMB, the Universe was nearly perfectly uniform with only 1 part in 100,000 variations in density across the entire sky.
Our current theory predicts that dark matter collapses to form dense regions that pull in nearby ordinary matter. The gas in these dense regions then cools and collapses to form galaxies and stars we see today.
Together, these stages comprise the current best model of the formation of the cosmos, known as the Lambda-Cold Dark Matter or Lambda-CDM model.
However, in 1998, astronomers measuring the distance to far-away supernovae discovered that the expansion had started to get faster instead of slower.
To explain this, scientists invoked dark energy, an unknown something that, unlike matter, gravitationally repels instead of attracts, pushing the Universe apart almost like 'anti-gravity'. The simplest version of dark energy is Einstein's original idea for a cosmological constant, as a way to balance the action of gravity in his theory of general relativity.
The mysterious dark energy constitutes nearly 70 per cent of the Universe today. And while we can't see dark energy directly, it determines how our Universe is expanding and its eventual fate.
Our international team collected data over two years with the main instrument.
We analysed this data, which covers 1/25th of the sky, to make precise measurements of temperature and polarisation patterns caused by the distribution of matter in the cosmic microwave background of the early Universe.
We combined the maps of the early Universe from the South Pole Telescope with observations of the 3D distribution of galaxies made previously by the Dark Energy Spectroscopic Instrument (DESI) collaboration.
What we saw in the DESI experiments, and now strengthened by our South Pole Telescope observations, is that dark energy is becoming weaker with time, or time-evolving. Dark energy's acceleration of the Universe's expansion may stop far in the future.
Previously, the gold standard for cosmic microwave background measurements was provided by Planck satellite data, taken a decade ago.
The improved measurements from the South Pole Telescope, when combined with the DESI experiment and other CMB datasets, reduce the likelihood of a cosmological constant and increase the preference for time-evolving dark energy models.
The significance further increases when observations of supernovae are added.
To prevent gravitational collapse and allow an eternal static Universe, Einstein added a repelling term to his theory, called a 'Cosmological Constant'. Einstein later retracted this after Edwin Hubble's discovery that the Universe was expanding in 1929.
Three decades after his death, astronomers looking at supernovae discovered the Universe's expansion was accelerating. The simplest explanation for this acceleration was to revive Einstein's cosmological constant as a repelling force.
Until recently, our observations of the Universe could be entirely explained by a cosmological constant.
If the current hints that dark energy is weakening are supported by further research, it will mean that we need to go beyond the cosmological constant, be it a change to the theory of general relativity or to include time-evolving dark energy.
The DESI collaboration is planning an upgraded instrument DESI-2 after the current survey, and eventually wants to build a much more ambitious spectroscopy experiment Spec-S5.
We can look forward to an upgraded receiver being installed on the South Pole Telescope in 2028, as well as future results from the Simons Observatory (beginning survey observations towards the end of this year) and in the 2030s the CMB-S4 experiment.
Sometime along this track, we will hopefully have enough evidence to definitively say if the accelerating expansion of the Universe is truly losing steam.
Research Report:SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field
Related Links
University of Melbourne
Understanding Time and Space
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