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Red light illuminates telescope.
Photo Courtesy: Dana Hrubes
Scientist Dana Hrubes works on the South Pole Telescope near the primary mirror using a red light to preserve his night vision. Researchers recently used the instrument to detect a long-predicted polarization pattern in the afterglow of the Big Bang called lensed B-modes.

New mode of discovery

South Pole Telescope detects polarization pattern in Big Bang afterglow

Scientists using the South Pole Telescope (SPT) External Non-U.S. government site became the first team to detect a long-predicted polarization pattern in the afterglow of the Big Bang External Non-U.S. government site called lensed B-modes. The detection of this signal is a milestone along the way toward understanding cosmic inflation External U.S. government site, the period of extremely rapid expansion of the universe in the first fraction of a second of its existence.

This measurement, detailed in a recent paper by the SPT collaboration External Non-U.S. government site, is briefly described in articles in Nature and Sky & Telescope External Non-U.S. government site. The University of Chicago External Non-U.S. government site leads the SPT collaboration, which includes a dozen institutions worldwide. John Carlstrom External Non-U.S. government site at the University of Chicago is the principal investigator of the project, which is primarily funded by the National Science Foundation External U.S. government site.

Full moon shines behind telescope.
Photo Credit: Dana Hrubes
The full moon shines behind the South Pole Telescpe.

Located at the geographic South Pole, the SPT is a large millimeter-wavelength telescope designed to observe the cosmic microwave background (CMB) External U.S. government site. The CMB is the light or the afterglow of the “Big Bang” that was released roughly 400,000 years after the birth of the universe — or about 13.7 billion years ago.

This intense visible light — red-shifted or stretched by the expansion of the universe since that time — is detectable today as an extremely weak microwave signal. This signal provides a “snapshot” of the primordial universe and contains a wealth of information concerning both fundamental physics and cosmology, such as the geometry, content, evolution, and even destiny of the universe.

While the South Pole may seem an inhospitable place to most, it provides one of the best sites for achieving the ambitious goals of the SPT project. Since moisture in the atmosphere absorbs microwaves, the thin, cold, dry atmosphere above the South Pole allows the SPT to more easily detect the CMB radiation. The air is so cold that there is very little moisture in it, and at about 9,300 feet elevation, there is much less atmosphere to look through.

SPT, which began observations in 2007, used a very sensitive camera that could measure the extremely small spatial temperature distribution or anisotropy of the CMB at three millimeter-wavelength bands. This first phase, completed in November 2011, had produced the highest resolution, highest sensitivity map of the CMB at that time. [See previous article — Mission complete: South Pole Telescope finishes five-year survey of galaxy clusters.]

The telescope has also discovered hundreds of massive high-redshift galaxy clusters (the most massive gravitationally bound entities in the universe), point sources including high-redshift dusty star-forming galaxies, and dust-obscured active galactic nuclei. [See previous article — Cluster of discoveries: South Pole Telescope finds fastest star-making region in the universe.]

These measurements have allowed the SPT collaboration to understand better the physics of the universe. The high-resolution map of the CMB anisotropy has led to improvements of the CMB power spectrum. The CMB power spectrum is essentially the sound spectrum in the hydrogen-helium plasma of the primordial universe. It is used to quantify a number of properties of the observable universe. 

Telescope focal plane.
Photo Credit: South Pole Telescope website
Focal plane for the South Pole Telescope polarization-sensitive camera.

A catalog of massive galaxy clusters over a range of redshift is allowing us to better constrain cosmological parameters such as the equation of state of dark energy External U.S. government site. The redshift of an observed object indicates when the light that is finally reaching us today was emitted. The higher the redshift of an object, the farther back in time the light was emitted. Therefore, by observing high-redshift objects, we are observing the universe as it was billions of years ago.

Examining objects over a large range of redshifts gives us a look at how gravitationally bound structures evolved over time, helping us to understand better how the mysterious force dubbed dark energy has influenced the expansion history of the universe.

In January 2012, the SPT was equipped with a new polarization-sensitive camera, SPTpol, to add to the capabilities of the telescope.

SPTpol is a dual-frequency polarization-sensitive camera sensitive to two millimeter-wavelength bands that will continue the original SPT science goals, and, in addition, measure the polarization anisotropy of the CMB. Polarization of the CMB light essentially means that the light waves have a preferential rather than random direction of oscillation. 

The polarization signal imprinted on the CMB can be decomposed into what are commonly referred to as “E-mode” (gradient-like) and “B-mode” (curl-like) signals, which are analogous to the “E” and “B” field patterns in electromagnetism.

Measuring the CMB takes extremely sensitive cameras with very low noise to measure variations in the 2.7 degree Kelvin (2.7 degrees above absolute zero) CMB. The temperature anisotropy across the CMB is one part in 100,000, requiring measurements of temperature differences of several hundred-thousandths of a degree. 

Side view of a telescope.
Photo Credit: Dana Hrubes
The South Pole Telescope in 2013 with new receiver, primary mirror shroud and larger ground shield.

The B-mode polarization anisotropy that was first measured with the SPT is 100 times fainter or about one part in 10 million. That means that we are measuring incredibly tiny differences in the 2.7 degree Kelvin CMB. E-mode polarization, essentially created by the fluctuations in density of the hydrogen-helium plasma in the early universe, was first measured with the DASI telescope External Non-U.S. government site at the South Pole in 2002.

B-mode polarization can be created in two ways: B-mode conversion of E-mode polarization by gravitational lensing and direct CMB polarization by inflationary gravity waves.

In mode conversion, E-mode polarized CMB light that has traveled through space for about 13.7 billion years to reach us is gravitationally lensed or distorted into B-mode polarized light as it travels past massive galaxy clusters.

These lensed B-modes can be used to better constrain cosmological parameters, such as the matter distribution in the universe and the masses of neutrinos. This is the B-mode polarization in the CMB that the SPT collaboration was recently the first to detect.

One of the next and even larger goals is to measure the B-mode polarization of the CMB created by gravity waves from the inflationary period  the initial, short-lived exponential expansion or the “bang” in the Big Bang. These are B-modes directly imprinted on the CMB by gravitational waves generated during this theorized inflationary period.

Detection of this primordial B-mode polarization would confirm the theory of inflation, the theory that provides a basis for the hot Big Bang model of the universe.

SF-funded research in this article: John Carlstrom, John Ruhl, Joseph Mohr, William Holzapfel and Nils Halverson, University of Chicago, Award No. 0638937 External U.S. government site; Michael Turner, University of Chicago, Award No. 1125897 External U.S. government site; and John Carlstrom, Albrecht Karle and John Morse, University of Chicago, Award No. 0750083 External U.S. government site.

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Curator: Peter Rejcek, Antarctic Support Contract | NSF Official: Winifred Reuning, Division of Polar Programs