It’s one of the big cosmology debates: The universe is expanding, but how fast exactly? Two available measurements yield different results. Leiden physicist David Harvey adapted an independent third measurement method using the light warping properties of galaxies predicted by Einstein. He published his findings in the Monthly Notices of the Royal Astronomical Society.
We’ve known for almost a century about the expansion of the universe. Astronomers noted that the light from faraway galaxies have a lower wavelength than galaxies close by. The light waves seem stretched, or redshifted, which means that those far galaxies are moving away.
This expansion rate, called the Hubble constant, can be measured. Certain supernovas, or exploding stars, have a well-understood brightness; this makes it possible to estimate their distance from Earth and relate that distance to their redshift or speed. For every megaparsec of distance (a parsec is 3.3 light-years), the speed that galaxies recede from us, increases with 73 kilometers per second.
However, increasingly accurate measurements of the cosmic microwave background, a remnant of light in the very early universe, yielded a different Hubble constant: about 67 kilometers per second.
How can that be? Why the difference? Could this difference tell us anything new about the universe and physics? “This,” says Leiden physicist David Harvey, “is why a third measurement, independent from the other two, has come into view: gravitational lenses.”
Albert Einstein’s theory of general relativity predicts that a concentration of mass, such as a galaxy, can bend the path of light, much like a lens does. When a galaxy is in front of a bright light source, the light is bent around it and can reach Earth via different routes, providing two, and sometimes even four, images of the same source.
In 1964, the Norwegian astrophysicist Sjur Refsdal had an “a-ha” moment: When the lensing galaxy is a bit off-center, one route is longer than the other. That means that the light takes longer by that path. So when there is a variation of the brightness of the quasar, this blip will be visible in one image before the other. The difference could be days, or even weeks or months.
This timing difference, Refsdal showed, can also be used to pin down distances to the quasar and the lens. Comparing these with the redshift of the quasars gives you an independent measurement of the Hubble constant.
A research collaboration under the HoliCOW project used six of these lenses to narrow down the Hubble constant to about 73. However, there are complications: apart from the distance difference, the mass of the foreground galaxy also exerts a delaying effect, depending on the exact mass distribution. “You have to model that distribution, but a lot of unknowns remain,” says Harvey. Uncertainties like this limit the accuracy of this technique.
Imaging the whole sky
This could change when a new telescope sees first light in Chile in 2021. The Vera Rubin Observatory is dedicated to imaging the whole sky every few nights, and is expected to image thousands of double quasars, offering a chance to narrow down the Hubble constant even further.
Harvey says, “The problem is that modeling all those foreground galaxies individually is impossible computationally.” So instead, Harvey designed a method to calculate the average effect of a full distribution of up to 1,000 lenses.
“In that case, individual quirks of the gravitational lenses are not that important, and you don’t have to do simulations for all the lenses. You just have to make sure that you model the entire population,” says Harvey.
“In the paper, I show that with this approach, the error in the Hubble constant thresholds at 2% when you approach thousands of quasars.”
This error margin will allow a meaningful comparison between the several Hubble constant candidates, and could help in understanding the discrepancy. “And if you want to go below 2%, you have to improve your model by doing better simulations. My guess is that this would be possible.”
More information: David Harvey, A 4 percent measurement of H0 using the cumulative distribution of strong lensing time delays in doubly imaged quasars. Monthly Notices of the Royal Astronomical Society (2020). DOI: 10.1093/mnras/staa2522
Citation: Gravitational lenses measure universe expansion (2020, November 17) retrieved 17 November 2020 from https://phys.org/news/2020-11-gravitational-lenses-universe-expansion.html
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