One of the greatest cosmic mysteries today concerns the expansion of the universe.

During the first billion years of our universe’s history, the rate of expansion of the universe slows and distant galaxies slow into stagnation from our era, as the density of matter and radiation decreases. However, over the past 6 billion years, distant galaxies have been accelerating their stagnation, and the rate of expansion, although it continues to decline, is not heading towards zero. Two different ways of measuring the rate of expansion give conflicting values; The actual rate of expansion remains controversial.
Two main methods each give low error answers, but are not compatible.

Taking us beyond the limits of any previous observatory, including all ground-based telescopes on Earth as well as Hubble, NASA’s JWST has shown us the most distant galaxies ever discovered in the universe. If we adequately map the 3D positions of the observed and measured galaxies, we can create a visual flyby across the universe, as CEERS data from JWST enables us to do here. Measuring the rate of expansion is challenging, as different methods yield different and mutually incompatible results.
By tracing the evolution of an early relic signal, we measure an expansion of 67 km/s/mq.

We can look randomly back into the universe if our telescopes allow it, and the galaxy cluster must reveal a specific distance scale – the acoustic scale – that must evolve with time in a certain way, just as the acoustic “peaks and valleys” in the cosmic microwave background reveal this. Scale too. The evolution of this scale, over time, is an early remnant that reveals a low expansion rate of about 67 km/sec/million blocks.
By starting close and noticing the slack increasing with distance, we measure 73 km/s/m per square metre.

Building the cosmic distance ladder involves moving from our solar system to stars, to nearby galaxies, to distant galaxies. Each ‘step’ carries its own uncertainties, especially the rungs at which the different ‘runs’ of the ladder connect. However, recent improvements in the distance ladder have shown just how strong his results can be.
This discrepancy – the “Hubble tension” – is a recent cosmic mystery.

Recent measurement tensions from the distance ladder (red) with early signal data from the CMB and BAO (blue) shown for contrast. It is plausible that the early sign method is correct and there is a fundamental flaw in the distance ladder; It is plausible that there is a small-scale error biasing the early sign method and the distance scale is correct, or that both groups are correct and some form of new physics (shown above) is the culprit. The idea that there was an early form of dark energy is interesting, but that means there was more dark energy in the early times, and it has (mostly) died out since then.
Many would expect a note error on the “distance ladder” side to be the culprit.

Back in 2001, there were many different sources of error that could bias the best distance-ladder measurements of the Hubble constant, the expansion of the universe, to significantly higher or lower values. Thanks to the diligent and careful work of many, this is no longer possible, since errors have been greatly reduced. New JWST work, not shown here, has reduced errors related to Cepheid and period luminosity errors further than shown here.
We begin by observing Cepheid variable stars within the Milky Way.

Variable star RS Puppis, with its light echoes shining through interstellar clouds. Variable stars come in many varieties. One of them, Cepheid variables, can be measured both within our galaxy and in galaxies up to 50-60 million light-years away. This enables us to extrapolate distances from our galaxy to distant galaxies in the universe. RR Lyrae and AGB branch stars can be used in a similar way.
We infer their exact distances by parallax.

The stars closest to Earth will appear to move cyclically with respect to the more distant stars as the Earth moves through space in orbit around the sun. Before creating the heliocentric model, we were not looking for “shifts” with a baseline of ~300,000,000 km over about 6 months, but rather a baseline of ~12,000 km over one night: the diameter of the Earth as it rotates on its axis. The distances to the stars were so great that the first sight, with a baseline of 300 million km, was not discovered until the 1830s. Today, we measured the parallax of more than a billion stars with the European Space Agency’s Gaia mission.
Then we measure Cepheids in well-measured nearby galaxies.

The top two panels show two nearby, maple-rich galaxies: NGC 4258 (left) and NGC 5584 (right), with JWST’s field of view added over them. Lower panels show JWST renderings, with individually selected Cepheid variants highlighted in each image.
Finally, we measure Type Ia supernovae both inside and outside those galaxies, and relate these cosmic “degrees” together.

As recently as 2019, there were only 19 published galaxies that had distances measured by Cepheid variable stars in which Type Ia supernovae were also observed to occur. We now have distance measurements from individual stars in galaxies that also hosted at least one Type Ia supernova in 42 galaxies, 35 of which have excellent images from Hubble. These 35 galaxies are shown here.
Could the error in Cepheids be biasing our measured expansion rate?

Using the cosmic distance ladder means piecing together different cosmic scales, as one always worries about uncertainty where the different “runs” of the ladder connect. As shown here, we are now down at least three “runs” on that ladder, and the whole set of measurements agree with each other amazingly well.
by Cepheids measured in nearby galaxiesJWST investigates this possibility.

This nearby spiral galaxy, NGC 4258 (also known as Messier 106), is about 20 million light-years away but contains many known Cepheids that are similar to the Cepheids found in the Milky Way. This is an important galaxy for calibrating the cosmic distance scale.
galaxy watch NGC 4258JWST found no optical bias for Algivides.

This image shows many Cepheid variable stars of different periods within the nearby galaxy NGC 4258: an important galaxy for Cepheid calibration and distance. The bottom six rows show the same stars measured by both Hubble (gray labels) and JWST (purple labels) at different wavelengths. The superior resolution in the JWST images reduces previous Hubble errors by large and large amounts while validating and remaining consistent with previous results.
Instead, it confirmed and reinforced previous Hubble Space Telescope findings.

This composite image shows barred spiral galaxy NGC 5584 with bright supernova SN 2007af within it. Nearby galaxies with identifiable Cepheid variable stars that have hosted at least one type Ia supernova within them are incredibly important to the cosmological distance ladder method for measuring the expanding universe.
Cepheids in NGC 5584which she also had A (2007 epoch) a Type Ia supernovaalso revealing no bias.

This graph shows the relationship between the amount of brightness of Cepheid variable stars (y axis) versus their period of change (x axis) in the galaxies NGC 5584 (top) and NGC 4258 (bottom). New JWST data is shown in red, while old Hubble data is shown in grey. The errors and uncertainties of this relationship in both galaxies have been greatly reduced, mainly due to the superior resolution of JWST over that of Hubble.
the Gloss relationship periodthe main calibration tool for Chronology, is now more accurate than ever.

By enabling a better understanding of the Cepheid variables in the nearby galaxies NGC 4258 and NGC 5584, the JWST has reduced the uncertainty in their distances even further. The lowest points on the graph show an estimate of the distance to NGC 5584 from expansion rates inferred from the distance scale (left side) and what is expected from the early remnant method (right side). The mismatch is large and convincing.
Thanks to its superior accuracy, JWST has reduced any uncertainties down to their absolute smallest values.

Standard candles (left) and standard rulers (right) are two different methods that astronomers use to measure the expansion of space at different times/distances in the past. Based on how quantities such as luminosity or angular size change with distance, we can infer the expansion history of the universe. Using the candle method is part of the distance ladder, yielding 73 km/sec/million blocks. The use of a ruler is part of the early indication method, yielding 67 km/s/Mpc. With the new JWST data, the mystery about the expansion rate of the universe has deepened even further.
Mostly Mute Monday tells an astronomical story with pictures and visuals and no more than 200 words.
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