The spring in the Northern Hemisphere brought along the primordial seeds of the Universe. The Planck satellite has completed precise measurements of the fluctuations in the temperature of the Cosmic Microwave Background (CMB), radiation emitted when the Universe was ~380,000 yrs old. How precise? So precise that the error bars on the temperature fluctuations measured are not determined by instrumental noise, but rather by the systematics caused by astrophysical processes. This is to say that the Planck team spent a huge amount of time trying to remove foregrounds from their data: Galactic and extragalactic astrophysical sources that, while interesting by themselves, contaminate CMB measurements by interacting with the CMB photons on their way to us. The angular resolution of the CMB map is roughly 7 arcminutes and the accuracy on the temperature fluctuations measured is of the order of 10-6. The Planck collaboration announced their results on March 21st, presenting their new constraints on cosmological parameters and making data products available to the scientific community. In an upcoming data release in early 2014, the Planck team will provide the full temperature and polarization data. In this post, we summarize two of the papers released by the collaboration on Thursday.Remarkable agreement with ΛCDM, plus a few puzzlesTitle: Planck 2013 results. I. Overview of products and scientific results
Authors: Planck CollaborationThe Planck collaboration’s main goal, first defined in 1995, is to map the temperature fluctuations of the CMB with unprecedented sensitivity, and in turn, determine the cosmological parameters of the Universe with great precision. With roughly 3 times better resolution and 25 times better sensitivity than its predecessor, NASA’s Wilkinson Microwave Anisotropy Probe (WMAP), the Planck collaboration has made substantial progress towards achieving these goals with its first data release. The major cosmological conclusion reached by Planck is that their data agrees remarkably well with the standard, six parameter cosmological model known as ΛCDM (described in terms of the 9-year WMAP results in this astrobite). The Planck team has measured the CMB angular power spectrum, which describes the amplitude of the temperature fluctuations as a function of scale on the sky. Generally, the power spectrum is plotted as a function of multipole number ℓ, where small ℓ corresponds to large scales on the sky. As evidenced by the figure below, the six parameter ΛCDM model not only provides an excellent fit to the Planck spectrum, but also to the 9-year data from WMAP and the smaller scale CMB data from the Atacama Cosmology Telescope and the South Pole Telescope.
While the same ΛCDM model describes the Planck data well overall, there are some significant changes in parameters from previous estimates. In particular, the Planck results indicate about 6% less dark energy, 9% more normal matter, and 18% more dark matter in comparison to previous CMB results. The results also indicate that the expansion of the Universe, characterized by the Hubble constant Ho, is proceeding slightly slower than expected from previous measurements. Perhaps most intriguing, the Planck team confirms the presence of some large scale anomalies in their temperature data, which were first detected with WMAP. No current theoretical models can sufficiently describe the origin of these anomalies, and these findings will surely ignite a flurry of theoretical work. Lastly, the Planck data detects the gravitational lensing of the CMB at extremely high significance and finds strong evidence for the occurrence of inflation. Keep reading to discover Planck’s constraints on the type of initial density fluctuations that led to the structure we see in the Universe today.The Gaussian UniverseTitle: Planck 2013 results. XXIV. Constraints on primordial non-Gaussianity
Author: Planck CollaborationOne of the big question marks in cosmology is whether the primordial density fluctuations are Gaussian. Gaussianity in this context means that the values of the temperature fluctuations can be drawn from a Gaussian distribution. Deviations from Gaussian conditions allow us to constrain models of the physics of the early Universe. We do so by going beyond the power spectrum statistics (the topic of the previous section).Any Gaussian random field can be characterized simply by its two-point correlation (and in Fourier space by its power spectrum). If the primordial perturbations evolve non-linearly or if several inflationary fields interact, the CMB temperature fluctuation field would be non-Gaussian. For a non-Gaussian field, it is insufficient to describe it in terms of its power spectrum. We need to compute, at least, the next order statistics, which in Fourier space is called the bispectrum. The usual approach to parametrizing non-Gaussianity is to do so in terms of a non-linearity parameter, fNL. This parameter captures the amplitude of the bispectrum, which is a function of three wavevectors, k1, k2 and k3. Because the three wavevectors must sum to zero, we can visualize contributions to the bispectrum as triangles of different shapes.The interest in measuring departures from Gaussianity arises because they allow us to set constraints on the mechanism of inflation. Different inflationary models predict different non-Gaussian effects, described not only by the amplitude of the bispectrum, but also by which triangle shapes most contribute to the bispectrum and on which scales they do so. For example, in the limit where k1 << k2 ~ k3, the “squeezed limit”, if significant non-Gaussianity is detected, it would rule out single-field slow-roll inflationary models in favor of multi-field inflation. “Squeezed” non-gaussianity is also predicted in cyclic and ekpyrotic models. One example of inflationary model that peaks in the “equilateral” shape, for which k1 ~ k2 ~ k3, is DBI inflation. The “orthogonal” shape is a feature of generalized single-field models or Galileon inflation. Planck has set the most stringent constraints in non-Gaussianity thus far, finding that their data is consistent with a Gaussian Universe. For the shapes we described above, they obtain the following constraints, paper.