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How heavy is the universe? Conflicting answers hint at new physics.

Gravity arises from the distortion of space-time itself.
(Image: © Shutterstock)

Two entirely different ways of "weighing" the cosmos are producing disparate results. If more precise measurements fail to resolve the discrepancy, physicists may have to revise the standard model of cosmology, our best description of the universe.

"If this really is a glimpse of the standard model breaking down, that would be potentially revolutionary," says astronomer Hendrik Hildebrandt of the Ruhr University Bochum in Germany.

Similar concerns over the correctness of the standard model have been raised over the past few years by two independent calculations of the so-called Hubble constant, or the rate at which the universe is expanding today. Those two measurements also disagreed, creating what has been called the Hubble tension.

The new discrepancy — called the sigma-eight tension — involves measuring the density of matter in the universe and the degree to which it is clumped up, as opposed to being uniformly distributed. The result is encapsulated in a parameter called sigma-eight. To calculate sigma-eight, Hildebrandt and his colleagues turned to an effect called weak gravitational lensing, in which the light from distant galaxies is bent ever so slightly toward our telescopes because of the gravitational pull from matter that lies between the galaxies and Earth.

The resulting distortion is so small that it barely changes the shape of an individual galaxy. But if you take an average of the shapes of tens of thousands of galaxies in a patch of sky, a signal of weak lensing pops out. Presuming that galaxies should be randomly oriented with respect to Earth, their average shape should be nearly circular—without weak lensing, that is. But thanks to the mild distortions from this effect, the average shape instead veers toward the elliptical.

The astronomers used this signal to estimate the amount and distribution of intervening matter (both normal and dark varieties) along the lines of sight to various galaxy-rich regions across a large patch of the sky. In other words, they managed to measure matter's cosmic density.

But doing so precisely requires one more piece of information: the distance to each individual galaxy being studied. Normally, astronomers calculate the distance to another galaxy by finding its spectroscopic redshift—the amount by which the galaxy's light is shifted toward the longer wavelengths of the red side of the spectrum. The greater the redshift, the farther away the object.

Measuring individual spectroscopic redshifts, however, is extremely inefficient when dealing with millions of galaxies. So Hildebrandt's team turned to something called photometric redshift, which involves taking multiple images of the same patch of sky in different wavelengths, spanning the optical and near-infrared ranges. The researchers used those images to estimate the redshift of individual galaxies in each one. "They're not as good as the traditional spectroscopic redshift," Hildebrandt says. "But they're much more efficient in terms of telescope time."

For its entire analysis, the team used high-resolution images of hundreds of square degrees of the sky (the full moon is about half a degree across) in nine wavelength bands—four optical and five near-infrared. These observations of about 15 million galaxies were collected by the European Southern Observatory's Kilo-Degree Survey (KiDS) and VISTA Kilo-Degree Infrared Galaxy Survey (VIKING) using two small telescopes at the organization's Paranal Observatory in Chile.

The VIKING data bolstered the KiDS data set by providing multiple observations of the same region of the sky in near-infrared wavelengths. The greater the distances of a galaxy, the higher the speed at which it is receding from us. This causes more of a galaxy's light to be redshifted into the near-infrared range, so relying solely on optical observations is not enough. Infrared measurements capture a greater amount of the light from such galaxies, leading to better estimates of their photometric redshift.

To ensure that photometric redshifts are as accurate as possible, these observations were calibrated against spectroscopic redshift measurements of a few of the same galaxies made with the more massive eight-meter Very Large Telescope at Paranal and the 10-meter Keck telescopes on Mauna Kea in Hawaii.

Astrophysicist and Nobel laureate Adam Riess of Johns Hopkins University approves of the efforts of the KiDS researchers. "Their latest results use infrared data, which probably does a better job of tracing the mass of the lenses and getting reliable photometric redshifts," he says.

Using the combined data, covering about 350 square degrees of the sky, the astronomers estimated sigma-eight.The value they found conflicts with a sigma-eight figure calculated using the European Space Agency's Planck satellite's observations of the cosmic microwave background (CMB)—the earliest observable light in the universe, which was emitted about 380,000 years after the big bang. Planck mapped the variations in the temperature and polarization of the CMB from point to point in the sky. Cosmologists can employ the map to calculate the sigma-eight value for the early universe. Using the standard model of cosmology (which says that the cosmos is made of about 5 percent ordinary matter, 27 percent dark matter and 68 percent dark energy), they can then extrapolate across more than 13 billion years of cosmic evolution to estimate the present-day value for sigma-eight.

Herein lies the tension. Hildebrandt's weak-lensing study estimates sigma-eight to be about 0.74, whereas the Planck data provides a value of about 0.81. "There is about a 1 percent chance or so that this [tension] is a statistical fluctuation," Hildebrandt says. Statistical fluctuations are random noise in data that can mimic actual signals and can disappear with more data. "This is not something to completely lose sleep over."

Not yet anyway. It is also possible a systematic error lurks in the calculations of one or both of the teams. After the researchers identify any such errors, the discrepancy could go away.

Or it may not do so, which has been the case with the Hubble tension. As astronomical measurements have become more precise, the statistical significance of the Hubble tension has only grown, inflicting sleepless nights on more than a few anxious theorists."Something very similar might happen with our sigma-eight discrepancy," Hildebrandt says. "We don't know."

Riess, who leads one of the teams estimating the Hubble constant using measurements of supernovae in the nearby universe, likens the sigma-eight tension to a "little brother or sister of the Hubble tension." That discrepancy is now considered statistically significant, with less than a one-in-3.5-million chance of being a fluke. The sigma-eight tension, with its one-in-100 chance of being a statistical aberration, is where the Hubble tension was a few years ago. "So [it is] less significant but worth keeping an eye on for a possible connection," Riess says.

If the sigma-eight tension ascends to the same level of statistical relevance as the Hubble tension, the pressure to reevaluate the standard model of cosmology could become too enormous to ignore. At that point, cosmologists may be forced to invoke new physics to bring the Planck estimates in line with the direct measurements of the parameters of the present-day universe. "That will be the exciting alternative," Hildebrandt says.

Potential "new physics" fixes to the standard model could involve changing the amount and nature of dark energy or dark matter—or both—as well as tweaks to how they interact with each other and with normal matter, among other more exotic modifications. "Some theoretical solutions to tinker with the cosmological model to fix the Hubble constant tension make this [sigma-eight tension] worse. Some make it better," Riess says.

Hildebrandt agrees that there is no obvious solution in sight. "If there was a compelling model, maybe people would jump on that bandwagon," he says. "But at the moment, I don't think there is. It's really on us observers to improve the significance [of the sigma-eight tension] or disprove it."

This article was first published at ScientificAmerican.com. © ScientificAmerican.com. All rights reserved Follow Scientific American on Twitter @SciAm and @SciamBlogs. Visit ScientificAmerican.com for the latest in science, health and technology news.

  • Hayseed
    The only thing that has "weight" are stars and planets. And if the modern time-line is close to correct, the majority of mass in the cosmos can not be "weighed".

    Weight come from gravity attraction. If stars have been burning for 13 billion years, most mass now, is isolated charge and has no gravitational attraction.

    Only dipoles and larger structures are affected by gravity.

    How can one measure anything, when we can only see and detect a certain radius(13 billion years) of the whole radius? Surely no one believes that we can see the whole cosmos.

    Making sense of our cosmos will always be iffy. Pick any dark area in space. Look at it closely. The farther you look, the denser it gets.

    Does that make sense? What if gravity decay was very great at the beginning.......then the most density would be on the rim of the cosmos. Out of sight.

    Iffy, iffy, iffy. Astronomy is a guessing game. We can not even determine a base line, to measure the closest star.
    Reply
  • Joshuagenes
    Given that dark energy and gravity are equal in force and dark energy may be a "push force" of gravity which acts in a thinner and more spread out manner... I would say the weight of the universe is zero.
    Reply
  • TorbjornLarsson
    It is below 3 sigma so it isn't even a tension as of yet.
    Reply
  • TorbjornLarsson
    Hayseed said:
    The only thing that has "weight" are stars and planets. And if the modern time-line is close to correct, the majority of mass in the cosmos can not be "weighed".

    Weight come from gravity attraction. If stars have been burning for 13 billion years, most mass now, is isolated charge and has no gravitational attraction.

    Only dipoles and larger structures are affected by gravity.

    How can one measure anything, when we can only see and detect a certain radius(13 billion years) of the whole radius? Surely no one believes that we can see the whole cosmos.

    Making sense of our cosmos will always be iffy. Pick any dark area in space. Look at it closely. The farther you look, the denser it gets.

    Does that make sense? What if gravity decay was very great at the beginning.......then the most density would be on the rim of the cosmos. Out of sight.

    Iffy, iffy, iffy. Astronomy is a guessing game. We can not even determine a base line, to measure the closest star.

    As you yourself point out, the title is a jest about gravity locally affecting mass since the researchers want to quantify how much the density of matter clumps up due to that.

    Many assertions in your comment doesn't square with cosmology, so maybe it is useful to discuss them?

    - Gravity only depends on mass (Newton discovered this), whether from normal or dark matter. Mass has nothing to do with electromagnetic (?) "dipoles" and the amount of mass energy lost in stars due to fusion is something like a percent. Sun will mass approximately the same when it is dead.

    - Clumping is observed on all scales starting from the large structures that you correctly mentions and which clumping is the major component of sigma-eight, but also smaller scales down to stars and planets. The dead Sun will affect sigma-eight about as much as today.

    - Since the universe expands, the observable radius is much larger than the age, and the age is about 14 billion years. The oldest photons, from the cosmic microwave background, that we see have traveled for 14 billion years but their starting point now lies 46 billion years out https://en.wikipedia.org/wiki/Observable_universe ]. The physics and the different measures gets complicated, but this fact is good to know. And the observable radius is, naturally, what we see and can see. We know from cosmic variance (spread in such measures as sigma-eight) that the universe is at least 5 times larger in radius and from its flatness at least 1,000 times larger.

    - We have made sense of "100 %" of the universe, since the current cosmology has less than 0.5 % uncertainty and the current cosmology is complete and self consistent. This is a good description of the latest cosmology and what it means: P1Q8tS-9hYoView: https://www.youtube.com/watch?v=P1Q8tS-9hYo

    - If the last sentence still refer to distances, it may be good to know that we have measured the distance to the closest star system (3 stars) since two centuries back https://en.wikipedia.org/wiki/Alpha_Centauri#Observational_history ]. The method is in fact a key method in the cosmic distance ladder, which was the first way to measure cosmic distances https://en.wikipedia.org/wiki/Cosmic_distance_ladder ].
    Reply