At the beginning of the hot Big Bang, our Universe was nearly uniform, though not entirely. Small variations in density occurred, with some regions being slightly denser or less dense than others.
Gravity and radiation interact with these regions: gravity attracts matter and energy to denser areas, while radiation pushes back. This interplay imprints patterns of temperature fluctuations into the cosmic microwave background (CMB), the leftover radiation from the Big Bang.
The angular size of these temperature fluctuations in the CMB is crucial. These fluctuations follow a specific pattern, where certain regions appear hotter or colder by specific amounts across different distance scales.
In a flat Universe, these scales appear as they are. In contrast, a positively curved Universe would make the scales appear larger, and a negatively curved Universe would make them appear smaller.
From observations, especially from the Planck satellite, scientists have determined with 99.6% certainty that the Universe is flat. This means that if there is any curvature, it would be on a scale at least 250 times larger than the observable Universe, which spans 92 billion light-years in diameter.
Another method of measuring the Universe's flatness is through the angular separation between galaxies that cluster at various epochs. Galaxies tend to cluster around a particular distance, about 500 million light-years apart in the present day. This "enhanced" clustering distance has grown as the Universe expanded. If the Universe were curved, this distance scale would appear distorted.
However, the fact that we observe no such distortion further supports the idea of a flat Universe, with an even greater precision of 99.75%.
If the Universe were a hypersphere (a four-dimensional analogue of a sphere), its radius would have to be at least 400 times larger than what we can observe. This gives us confidence that the Universe is flat, at least on the scales we can measure.
Understanding why the Universe is flat requires looking at cosmic inflation, a theory that explains the rapid expansion of the Universe before the Big Bang. Inflation stretched the Universe to such a large scale that what we observe now appears flat.
However, quantum fluctuations from this period might have left tiny distortions. Current measurements show that any departure from flatness is so small that it is indistinguishable, but future observations could detect deviations at a level between 1-part-in-10,000 and 1-part-in-1,000,000.
Although our current measurements suggest the Universe is flat, upcoming missions and new technologies, such as the Roman Telescope, EUCLID mission, and the Rubin Observatory, aim to measure its curvature with even greater precision. These efforts might eventually reveal that the Universe has a small but significant curvature, offering new insights into cosmic inflation and the origins of the Universe.
While the Universe appears flat today, it’s possible that future discoveries will show otherwise, reminding us that the Universe holds endless possibilities.
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