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How was the polarization experimentally measured in the BICEP2 experiments and why did they look specifically at B-modes? Why is it implying the existence of gravitational waves and the need to quantize gravity? Moreover, why is it implying inflation as a unique option?

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Could you edit your post to ask one specific question please? The others you can post separately, although check our existing BICEP2 questions to make sure they're not duplicates. –  David Z Mar 18 at 0:41
    
The problem is that they are all connected and I prefer to get a coherent answer which connects between them. I already checked for duplicates but found none. –  Yair Mar 18 at 1:33
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Hm... well, a good rule of thumb, especially in this case, is that you should be able to ask your core question in the post title, and the question body should be an elaboration of that. "Some questions on BICEP2 experiments" is frankly a bad title, which makes it seem like you have an assortment of unrelated questions. If you can put your main question in the title, and expand on the question body to show how these other things are related to it, this would probably be a much better question. If you can't adequately summarize your question in the title field, it may be too broad. –  David Z Mar 18 at 2:13

2 Answers 2

I can answer partially to your questions.

How do we measure polarisation ?

They measured the so-called $Q$ and $U$ Stokes parameters. There are four Stokes parameters : $I$, $Q$, $U$, and $V$. $I$ is the intensity, that we already know a lot about (temperature), then $Q$ and $U$ are linear polarization along axis that are tilted with an angle of 45° with respect to each other, and V describe the circular polarization. There is no physical phenomena to create circular polarisation in the CMB, that is why we ignore it and only consider $Q$ and $U$ (maybe $V$ is still measured for calibration or whatever but it is near zero). Wikipedia

Why do we look specifically at $B$ modes ?

The $Q$ and $U$ parameters can be easy to measure experimentally, but are not very handy on a theoretical point of vue since they depend on the system of coordinates that you use. What is more interesting is the $E$ and $B$ modes of the polarisation. Given a $Q$ and $U$ map, you can decompose the polarisation into $E$ and $B$ modes (it can be a tricky problem however when you have a lot of pixels or some borders).

The $E$ modes are often referred as the "gradient" part of the polarisation, while the $B$ mode are the "curl". The thing is that $B$ modes can only be created with tensorial perturbation (i.e. gravitational waves), and not scalar perturbation (temperature).

Last, I don't think observing $B$ modes has for only implication that the inflation is the only possible theory. You can always find other fancy theories that would produce the same signal. But those are generally more complicated and less convincing in general. This is why people consider that observing $B$ modes is a solid hint for inflation.

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Thanks for your clarifications! –  Yair Mar 18 at 2:27

Here is the link to the paper.

This is a detector at the south pole with a telescope focusing the cosmic background radiation (CMB), on a focal plane equipped with incident energy sensitive detectors, the signal going to a data acquisition system. All the system is kept at 4 kelvin because the incident CMB is very very low frequency: a black body radiation system of temperature 2.7 kelvin.

It seems that the detectors in the focal plane are paired

Changes in the power incident on this island were detected using a transition edge sensor (TES). There was an 8x8 array of pixels on each tile, and four such tiles were combined to form the complete focal plane unit. There were thus, in principle, 256 dual-polarization pixels in the focal plane for a total of 512 detectors,

. . .

The focal plane was cooled to 270 mK by a closed cycle three-stage sorption refrigerator.

In section 4.1

In the next step the sum and difference of each detector pair is taken, the pair-sum being ultimately used to form maps of temperature anisotropy, and the pair-difference to measure polarization. Each half-scan is then subjected to a third order polynomial filtering.

This says that it is the relative difference between adjacent temperature detectors that will give the information on polarization. These transition edge detectors use superconductivity to attain the sensitivity to polarization.

From the FAQ of the experiment

What is B-mode polarization and how is it generated by inflation?

Measuring the polarization of the Cosmic Microwave Background at different points on the sky determines a direction and polarized intensity (the polarized intensity of the CMB is less than 1/1,000,000 its total brightness). This can be visualized as a map of little line segments at every spot on the sky, the patterns of which we analyze. B-mode polarization is essentially the swirly part of that pattern (known mathematically as the ‘curl’). For the density fluctuations that generate most of the polarization of the CMB this part of the primordial pattern is exactly zero.

[This is because density flows in the early universe go into or out of dense regions, and the polarization lines up with these flows in a way that doesn't swirl, producing only so-called E-mode polarization. To generate a B-mode pattern in the early universe you need gravitational waves.]

Inflation magnifies quantum fluctuations, which exist even in vacuum. The quantum fluctuations in the inflation field itself (“inflaton”) become the density fluctuations seen in the CMB and at much later times in galaxy distributions. During inflation, the quantum fluctuations in gravity (“graviton”) become long wavelength gravitational waves that produced the B-mode we see.

This is exciting because it is a first detection of an imprint of the graviton. To have gravitons, gravity must be quantized. What the result tells us is that the approximate field theoretical models used for the first instances after the Big Bang, which assume quantization of gravity are on the right path, which means gravity has to be quantized.

This observation excludes models that do not have this high intensity gravitational fields that the Big Bang standard cosmology has. I suppose theorists with different theories will be scrambling to fit the data.

In this blog post a good discussion of the results is given by prof. Liam McAllister.

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"During inflation, the quantum fluctuations in gravity (“graviton”) become long wavelength gravitational waves that produced the B-mode we see." Does that mean that quantum gravitational waves were created during inflation, and put to large scales because of inflation ? Therefore, the gravitational waves were still present when the CMB was released, imprinting the polarisation ? I was confused by that. Does that also mean that primordial gravity waves are still existing today, but we can't see them because they have waayyy to small amplitude ? –  Bagheera Mar 19 at 15:49

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