The rate at which the universe is expanding, known as the Hubble constant, is one of the fundamental parameters for understanding the evolution and ultimate fate of the cosmos. However, a persistent difference called the “Hubble Tension” is seen between the value of the constant measured with a wide range of independent distance indicators and its value predicted from the big bang afterglow.
![A large galaxy takes up the entirety of the image. The galaxy has a bright white core, and several large spiral arms extending out from that core, rotating clockwise. The arms are light blue with many pink speckles and clumps littering the arms. The background is also filled with a smattering of white and pink dots.](https://blogs.nasa.gov/webb/wp-content/uploads/sites/326/2023/09/STSCI-J-p23506b-m-2000x1880-1-1024x963.png)
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Credit: NASA, ESA, CSA, and A. Riess (STScI).
NASA’s James Webb Space Telescope provides new capabilities to scrutinize and refine some of the strongest observational evidence for this tension. Nobel Laureate Adam Riess from the Johns Hopkins University and the Space Telescope Science Institute presents his and his colleagues’ recent work using Webb observations to improve the precision of local measurements of the Hubble constant.
“Did you ever struggle to see a sign that was at the edge of your vision? What does it say? What does it mean? Even with the most powerful telescopes, the ‘signs’ astronomers want to read appear so small that we struggle too.
“The sign cosmologists want to read is a cosmic speed limit sign that tells us how fast the universe is expanding — a number called the Hubble constant. Our sign is written into the stars in distant galaxies. The brightnesses of certain stars in those galaxies tell us how far away they are and thus for how much time this light has been traveling to reach us, and the redshifts of the galaxies tell us how much the universe expanded over that time, hence telling us the expansion rate.
![Graphic titled “Uncrowding Cepheids in the Near-Infrared.” Left: Colorful image of a spiral galaxy is labeled “NGC 5584 (Webb NIRCam + Hubble WFC3).” Part of a spiral arm is outlined with a box. Inside the box is a solid red circle. Middle: Set of two diagrams illustrating zoomed-in views of the boxed region. Top diagram shows Hubble pointing toward a large transparent box. Long edge of the base is labeled “depth.” Box contains numerous overlapping, blue-green spheres of different sizes, with a red sphere near the middle. Bottom diagram shows Webb pointing toward an almost identical box. Spheres in this box are significantly smaller and there is less overlap. The red sphere is labeled “Cepheid.” Right: Two square grayscale images. Top is labeled “HST WFC3-IR.” Bottom labeled “JWST NIRCAM.” Pixels in the top image are noticeably larger than those in the bottom image. Black spots in the bottom image are smaller, more distinct, and more numerous. Click View Description for more details.](https://blogs.nasa.gov/webb/wp-content/uploads/sites/326/2023/09/STSCI-H-p23506a-d-2000x1125-1-1024x576.jpg)
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Image Credit: NASA, ESA, A. Riess (STScI), W. Yuan (STScI).
“A particular class of stars, Cepheid variables, has given us the most precise measurements of distance for over a century because these stars are extraordinarily bright: They are supergiant stars, a hundred thousand times the luminosity of the Sun. What’s more, they pulsate (that is, expand and contract in size) over a period of weeks that indicates their relative luminosity. The longer the period, the intrinsically brighter they are. They are the gold standard tool for the purpose of measuring the distances of galaxies a hundred million or more light years away, a crucial step to determine the Hubble constant. Unfortunately, stars in galaxies are crowded together in a small space from our distant vantage point and so we often lack the resolution to separate them from their line-of-sight neighbors.
“A major justification for building the Hubble Space Telescope was to solve this problem. Prior to Hubble’s 1990 launch and its subsequent Cepheid measurements, the expansion rate of the universe was so uncertain astronomers weren’t sure if the universe has been expanding for 10 billion or 20 billion years. That’s because a faster expansion rate will lead to a younger age for the universe, and a slower expansion rate will lead to an older age of the universe. Hubble has better visible-wavelength resolution than any ground-based telescope because it sits above the blurring effects of Earth’s atmosphere. As a result, it can identify individual Cepheid variables in galaxies that are more than a hundred million light-years away and measure the time interval over which they change their brightness.
“However, we also must observe the Cepheids at the near-infrared part of the spectrum to see the light which passes unscathed through intervening dust. (Dust absorbs and scatters blue optical light, making distant objects look faint and fooling us into believing they are farther away than they are). Unfortunately, Hubble’s red-light vision is not as sharp as its blue, so the Cepheid starlight we see there is blended with other stars in its field of view. We can account for the average amount of blending, statistically, the same way a doctor figures out your weight by subtracting the average weight of clothes from the scale reading, but doing so adds noise to the measurements. Some people’s clothes are heavier than others.
“However, sharp infrared vision is one of the James Webb Space Telescope’s superpowers. With its large mirror and sensitive optics, it can readily separate the Cepheid light from neighboring stars with little blending. In the first year of Webb operations with our General Observers program 1685, we collected observations of Cepheids found by Hubble at two steps along what’s known as the cosmic distance ladder. The first step involves observing Cepheids in a galaxy with a known, geometric distance that allows us to calibrate the true luminosity of Cepheids. For our program that galaxy is NGC 4258. The second step is to observe Cepheids in the host galaxies of recent Type Ia supernovae. The combination of the first two steps transfers knowledge of the distance to the supernovae to calibrate their true luminosities. Step three is to observe those supernovae far away where the expansion of the universe is apparent and can be measured by comparing the distances inferred from their brightness and the redshifts of the supernova host galaxies. This sequence of steps is known as the distance ladder.
“We recently got our first Webb measurements from steps one and two which allows us to complete the distance ladder and compare to the previous measurements with Hubble (see figure) Webb’s measurements have dramatically cut the noise in the Cepheid measurements due to the observatory’s resolution at near-infrared wavelengths. This kind of improvement is the stuff astronomers dream of! We observed more than 320 Cepheids across the first two steps. We confirmed that the earlier Hubble Space Telescope measurements were accurate, albeit noisier. We have also observed four more supernova hosts with Webb and we see a similar result for the whole sample.
![Graphs of the luminosity versus period relationship of cepheids in NGC 5584 (top) and NGC 4258 (bottom), as measured by HST (gray data points) and JWST (red data points). Top graph: The y-axis of luminosity ranges from 27 Vega mag at the bottom to 22 Vega mag at the top, labeled in increments of 0.5. The x-axis of Period is on a log scale ranging from ## days on the right to ## days at the far, labeled at 16, 25, 40, 63, and 100. Bottom graph: y-axis ranges from 26 to 20; x-axis ranges from # to 80, labeled at 5, 10, 20, 40, and 80.](https://blogs.nasa.gov/webb/wp-content/uploads/sites/326/2023/09/Graphic-2-1024x1006.png)
Image Credit: NASA, ESA, A. Riess (STScI), and G. Anand (STScI).
“What the results still do not explain is why the universe appears to be expanding so fast! We can predict the expansion rate of the universe by observing its baby picture, the cosmic microwave background, and then employing our best model of how it grows up over time to tell us how fast the universe should be expanding today. The fact that the present measure of the expansion rate significantly exceeds the prediction is a now decade-long problem called “The Hubble Tension.” The most exciting possibility is that the Tension is a clue about something we are missing in our understanding of the cosmos.
“It may indicate the presence of exotic dark energy, exotic dark matter, a revision to our understanding of gravity, or the presence of a unique particle or field. The more mundane explanation would be multiple measurement errors conspiring in the same direction (astronomers have ruled out a single error by using independent steps), so that is why it is so important to redo the measurements with greater fidelity. With Webb confirming the measurements from Hubble, the Webb measurements provide the strongest evidence yet that systematic errors in Hubble’s Cepheid photometry do not play a significant role in the present Hubble Tension. As a result, the more interesting possibilities remain on the table and the mystery of the Tension deepens.”
Editor’s Note: This post highlights data from a paper that was accepted by The Astrophysical Journal.
Author:
- Adam Riess is a Bloomberg Distinguished Professor at the Johns Hopkins University, the Thomas J. Barber Professor in Space Studies at the JHU Krieger School of Arts and Sciences, a distinguished astronomer at the Space Telescope Science Institute, and a recipient of the 2011 Nobel Prize in Physics.