sexta-feira, 21 de março de 2008

A New Day in Precision Cosmology

A Sky & Telescope Special Online Feature
March 11, 2008
by Alan MacRobert

All-sky map of microwave background
Tiny temperature irregularities in the cosmic microwave background are plotted on this map of the whole sky. This is the new the 5-year WMAP data. The average temperature is 2.725 kelvins (degrees above absolute zero; equivalent to –270° C or –455° F). The colors represent very slight deviations from this temperature, as in a weather map. Red regions are warmer and blue regions are colder by only about 0.0002 degree. Click image for larger view.
NASA / WMAP Science Team
Ask what's the greatest scientific triumph of our lifetime, and somewhere near the top of the list would be the establishment of "precision cosmology." In just the last decade or so, astronomers working in a remarkable specialty have determined — with high accuracy — such things as the date of the Big Bang, the amount and makeup of all the matter and energy in the universe, the large-scale shape of space, and how cosmic structure (galaxy clusters, galaxies, stars) grew and evolved from the very beginning to now, and why.
Along the way, researchers have confirmed some key predictions of the "inflationary universe" theory of how the Big Bang itself erupted from a much larger, underlying pre-existence, which could be producing inconceivable numbers of other, separate big-bang universes all the time.
This has become possible not by conventional astronomy, but by analyzing the cosmic microwave background radiation that covers the entire sky. This weak radio glow is literally the white light emitted by the still-white-hot universe as it stood just 380,000 years after the Big Bang. The light has been redshifted down into the microwave part of the spectrum (by a factor of 1,091) by the expansion of space since that time.

The temperature fluctuations sorted by size
This "power spectrum" shows how strong the temperature irregularities in the microwave background are (vertical axis) depending on their angular sizes on the sky (horizontal axis). Very large structures are on the left, and smaller angles are on the right. The strongest variations appear about 1° wide on the sky, the large first peak in the graph. This means that there was a preferred length for the cosmic-sized acoustic waves (pressure waves) in the dense early universe. The exact positions and sizes of the first, second, and third acoustic peaks tell about various conditions prevailing in the early universe. Dots with error bars are WMAP observations. The red line shows the values predicted by one particular theoretical cosmic model. Click image for larger view.
NASA / WMAP Science Team
Dozens of experiments have mapped tiny, telltale irregularities in the microwave background; these projects have worked at various scales and have pointed at different parts of the sky. But the most important instrument now doing this work is the orbiting Wilkinson Microwave Anisotropy Probe (WMAP). It is mapping the background radiation's temperature and polarization across the entire celestial sphere, and at a wide variety of angular scales: from large (many degrees wide, constellation-size) to nearly as small as the resolution of the human eye.
As time goes on, WMAP has continued to sharpen its picture.
Its first-year data release, in 2003, set milestones in precision cosmology -- among other things, pinning the age of the universe to 13.7 billion years with an uncertainty of just a couple percent, and confirming the existence of the recently discovered "dark energy" that is making the expansion of the universe speed up.
The three-year data release, in 2006, confirmed that the first results were on target, refined the numbers, and put new constraints on how cosmic inflation could have worked during the first 10–32 second or so of the Big Bang. The story of how such things can be found from mere maps of the microwave background (such as the new one pictured at top) is told in the May issue of Sky & Telescope, now at the printer.
The New Big Picture
Just after we sent that issue to press, WMAP's science team released the much-awaited five-year data set, along with their conclusions about what it tells. Once again, the additional data (and better long-term calibration of the instruments) refines the picture significantly — and, as a result, yields new conclusions.
The following results combine the new WMAP data with other recent astronomical clues:
  • The universe is 13.73 ± 0.12 billion years old. That's an uncertainty of only 0.9% now (at the 68-percent confidence level). Astronomy books in your public library probably say the universe is "between 10 and 20" billion years old.

  • The Hubble constant, the rate of the universe's expansion today, is 70.1 ± 1.3 kilometers per second per megaparsec. Books in your library probably say it's "between 50 and 100."
    These refinements affect everything else. For instance:

    Everything in the universe, now and long ago. The top chart shows the constituents today. The bottom one shows the composition just 380,000 years after the Big Bang, when the universe became transparent and the microwave background radiation broke free. The relative composition changed greatly as the universe expanded. Dark matter and baryonic matter ("atoms") just thinned out as the space they were in widened, like ordinary gases. But photons and neutrinos also lose energy in expanding space, so their energy density decreased faster than the matter. They're an insignificant portion now.

    Meanwhile, the proportion of dark energy increased directly with the increasing volume of space — indicating that it is something about spacetime itself, rather than being some substance that exists in space.

    NASA / WMAP Science Team

  • The sum total of everything in the universe consists of the following: matter made of atoms ("baryonic matter") 4.6% ± 0.15%, nonbaryonic dark matter 23% ± 1%, dark energy 72% ± 1.5%. We know almost nothing about what the dark matter and dark energy are, but we do know quite well now how much of each is out there.

  • All this matter and energy adds up, within just 1% uncertainty, to exactly enough to make space "flat," as inflationary-universe theories predict. That is, empty space on the largest cosmic scales is just like the ordinary space right around you: having no overall curvature or weird geometry. This also implies that space extends infinitely far beyond our visible horizon, equally in all directions, as best we can tell.

  • The behavior of the mysterious dark energy is becoming clearer. Its "equation of state," a parameter known as w, equals –1 to a precision of 6%. That's the best determination of it yet. This implies that dark energy is not something that spreads out as space expands, the way particles in space would, but is something inherent to spacetime itself — so that one cubic centimeter of space always contains the same amount of it no matter how greatly space has expanded. This matches Albert Einstein's idea of a "cosmological constant" from the 1920s (referred to by the Greek letter Lambda, Λ) and argues against the dark energy being a sort of physical substance that has been proposed, dubbed "quintessence."
    This also means that the universe's stars, planets, and atoms will not all be torn apart in the coming billions of years by a runaway increase in cosmic acceleration, a situation called the Big Rip.

  • In the first instants of the Big Bang, microscopic quantum fluctuations — little, random irregularities that got inflated to become the seeds of cosmic structure today — indeed seem to have been random at all scales, as inflation predicts — rather than being shaped or directed by some additional process. However, there are several hints of something else going on right at the current edge of uncertainty.

    Cosmic history, from beginning to now
    Cosmic history symbolized. The far left depicts the Big Bang, the earliest moment we can yet probe, when an extremely brief moment of "inflation" produced a burst of exponential growth in the universe. (Size is symbolized by vertical extent here.) For the next several billion years, the expansion of the universe gradually slowed as the matter in the universe pulled on itself via gravity. More recently, the expansion has begun to speed up — as the repulsive effect of dark energy has come to dominate over the pull of gravity as matter thins out. Today's microwave background (green surface at left) broke free 380,000 years after inflation, when the stuff of the universe first thinned and cooled enough to become transparent. This radiation has traversed the universe mostly unimpeded since then. The conditions of very early times are imprinted on this radiation. It also forms a backlight for later developments of the universe. Click image for larger view.
    NASA / WMAP Science Team

  • Some versions of cosmic inflation itself are now eliminated. Others have gained new support. (For you cosmo-geeks in the know: the "scalar spectral index" seems to be clearly tilted, with a value around 0.96 instead of 1.0.) "The new WMAP data rule out many mainstream ideas that seek to describe the growth burst in the early universe," explains WMAP principal investigator Charles Bennett (Johns Hopkins University). "It is astonishing that bold predictions of events in the first moments of the universe now can be confronted with solid measurements."

  • WMAP also finds concrete evidence for a "cosmic neutrino background" filling space. The neutrinos (weak, extremely low-mass particles) came from nuclear reactions in the dense matter that filled the universe in the Big Bang's first few minutes. By the time of the visible microwave background, 380,000 years later, neutrinos still amounted to 10% of all matter and energy in the universe, compared to their vanishingly small proportion today.
    In addition, the three types of neutrinos that exist have masses that can add up to no more that 0.61 electron volt, agreeing with laboratory experiments.

  • The cosmic "dark ages" — the era between when the Big Bang cooled and the first stars formed (an era when the universe became so cold that molecular-hydrogen snowflakes may have formed) — began ending around cosmic age 400 million years (redshift 11). This change is known as the "reionization era." The date fits in with evidence that's been coming from more normal astronomical methods. (Reionization apparently was, however, a drawn-out affair, happening by fits and starts in different places.)
    The five-year WMAP results have been issued in seven scientific papers submitted to the Astrophysical Journal.
    Also, NASA has put out a popular summary .
    "We are living in an extraordinary time," says Gary Hinshaw (NASA/Goddard Space Flight Center). "Ours is the first generation in human history to make such detailed and far-reaching measurements of our universe."
    Posted by:
    Lucimary Vargas
    Além Paraíba-MG-Brasil

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