Light and the Age of the Universe - The Discovery and Analysis of the CMB

Discovery of the Cosmic Microwave Background

The Comic Microwave Background was discovered pretty much by accident by Arno Penzias and Robert Wilson who were working for Bell Laboratories, looking for signals from radio waves reflected from balloons. In the course of their experiments, they had to eliminate all noise sources such as radio broadcasts, and even a "white dielectric substance" left on the inside of the detector horn by a family of pigeons who had taken nest there. Once they had got rid of and accounted for every bit of noise they could, they noticed that there was a constant microwave hiss, from every direction, day and night - they had discovered the Cosmic Microwave Background.

The antenna where they made this discovery is now a national monument in the US:

They still did not know what they had found however, but when a friend of theirs told them about a still unpublished paper by Jim Peebles talking about the possibility of finding a signal like theirs, and what it would mean, they began to realise the significance of their discovery. The papers by Peebles and his colleagues, and the paper published by Penzias and Wilson were published together in Astrophysical Journal Letters. Penzias and Wilson won the 1978 Nobel Prize for their work.

The Cosmic Background Explorer

It was thought from early on after the discovery, that there would be small anisotropies (differences depending on direction) in the CMB, but ground based measurements were not good enough to measure them. It was not until the COsmic Background Explorer (COBE) was launched in 1989 that these anisotropies were first observed.

These fluctuations were very small, just one part in 10,000 of the average temperature. The resolution was still relatively low however, and so there was still much detail to be found. One additional important piece of evidence however came out of this - the match between the theoretically predicted Black Body curve based on the Big Bang model, and the experimental curve. The two matched precisely:

These results earned another Nobel Prize, but this time for the principal investigators on the COBE project; George Smoot and John Mather. The CMB wasn't the only thing that COBE was analysing however, and there were other important experiments and discoveries made. A good outline of the COBE satellite's other results can be found here.

The Wilkinson Microwave Anisotropy Probe (WMAP)

The next satellite to look at the CMB was WMAP. This time dedicated to the analysis of the CMB. After the success of COBE, WMAP was designed to not only view the CMB at higher resolution and sensitivity, but also to look at other features of the CMB such as polarization in order to give a better understanding of the early universe. There are a number of interesting results from WMAP, which will continue to operate until (currently) September 2010, and more details can be found here.

A brief summary of some of the WMAP results

• The universe is 13.73 billion years old (the most accurate figure we have))
• The universe is very flat (Euclidean)
• Around 23% of the universe is dark matter.
• The anisotropies appear to be random (though there are some hints of deviations from simple randomness which could give further clues into the early nature of the universe)

The Future Exploration of the CMB

This article has provided only a brief outline of the discovery and analysis of the Cosmic Microwave background. There are a number of features that have not been discussed, such as doppler shift, polarization and so on, and there is still much work to be done in understanding the details of the CMB. Although WMAP only has a few months of life left, the European Planck observatory, which started to take measurements in 2009, and is expected to begin to release results in 2012.

Light and the Age of the Universe - the Cosmic Microwave Background

Our main window to understanding the universe is light and the electromagnetic spectrum. Trapped here on earth, there is very little of the universe that we can actually touch and test with our own hands, but light provides an amazing tool. The Cosmic Microwave Background is perhaps on of the best methods we have of finding the age of the universe.

All objects that are in thermal equilibrium - that is, the matter and EM radiation in the objects are the same temperature - have what is known as a black body spectrum - EM radiation with properties that are a function of the temperature of that object only. That spectrum might be modified a little but atomic absorption and emission lines, but the fundamental black body spectrum will remain. The spectrum looks like the curves on this graph:

Each curve represents a black body emitter with a particular temperature, shown in Kelvin (roughly the temperature in degrees plus 273, where 0 is absolute zero). The Sun, indeed all stars have a black body spectrum. In the case of the sun, the surface, and black body temperature is about 6000K, so it looks not so dissimilar from the 5000K curve. You can see that the black body spectrum continues beyond the visible - indeed the IR part is what is responsible for heat from the sun. The earth has a black body spectrum of about 278K (5.5 Celsius), which peaks in the infra red.

So what does this have to do with the age of the universe? Well when the universe was a mere 400,000 years old, about 13.7 billion years ago, everything was very much closer together, though space was expanding rapidly, and so the universe was much hotter than it is now, so hot in fact that there were no atoms, there was just a sea or plasma of hydrogen and helium nuclei (and a bit of lithium) electrons, Electromagnetic radiation and other subatomic particles (earlier than this there weren't even nuclei, but that's earlier than we are interested in here). The universe was still too hot for the electrons to bind to the nuclei, and so photons were constantly being absorbed and re-emitted by the various charged particles that were around, and the universe was in a state of equilibrium between matter and radiation. This means there was a black body spectrum. Eventually, as the universe expanded electrons no longer had enough energy to constantly escape binding to the nuclei, and they finally bound, becoming hydrogen and helium atoms. There was still substantial interaction between matter and radiation, particularly in the form of scattering, such as Compton Scattering and Thompson Scattering. The universe continued to cool as it expanded further, and eventually cooled down to a temperature of about 4000K at which the scattering dropped off. The radiation at this point became decoupled from the matter in the universe, as the universe became transparent, though the shape of the spectrum remained imprinted on the light that passed on, and continued traveling through the universe.

In the intervening billions of years, space itself continued to stretch. Imagine drawing a wave on a balloon, and blowing up the balloon. You will see the wavelength becomes longer and longer. The same effect occurs to the radiation, but now the the very space of the universe is expanding, so photons that initially had a short wavelength, over time were stretched out so the wavelength was longer and longer, so long in fact, that the BB spectrum which peaked at 4000K now peaks at a temperature of just 2.725K - barely above absolute zero.

This temperature is the same in all directions, though there are tiny fluctuations, which resulted from small changes to the very uniform distribution of matter and energy in the early universe as we can see in the (Wilkinson Microwave Anisotropy Probe ) WMAP satellite image below. It is these tiny imperfections that seeded the collapse of the primordial matter into the stars and galaxies of the universe today.

By knowing the rate at which the universe is expanding, which we can measure from the red shift of other features of the universe such as distant stars, galaxies and quasars, and these initial temperatures (which we know from looking at hydrogen and helium in the lab) we can then deduce the age of the universe (in much the same way as we can determine how long a cup of water has been standing on a table for if we know it was boiling when it was put there)...

...13.7 billion years old.

Quickfire Question: How do incandescent (filament) bulbs work?

We are all familiar with incandescent bulbs, which have been until relatively recently been the most popular sort of bulb.

A voltage is placed across a metal filament held in an inert gas like argon, neon or nitrogen, in order to stop the gas from reacting with the filament and allowing the bulb to live longer. The filament has a high resistance to the current flowing through it, and this heats the filament, causing the atoms in the filament to vibrate. As the atoms vibrate, they then radiate energy in the form of light.

An important point that can be made here, is that all vibrating atoms and molecules will radiate somewhere on the electromagnetic spectrum. The hotter they are, the faster they vibrate, and thus the higher the energy (and frequency) the photons are that they emit.

A problem with this sort of lamp, is that they are very inefficient. Because the light is generated by heating, large amounts of energy is lost in unwanted heat. Also as the filament is heated, it slowly evaporates over time and eventually breaks, leading to a relatively short lifetime. It is mainly for these reasons that there is a move to using energy saving bulbs, which both have a longer life, and also produce the same amount of light for less energy input.

Quickfire Question: Why are street lamps amber?

We are familiar with the colour of many street lamps, the amber glow of the sodium vapour:

But how do these lamps work, why are they the colour that they are, and why do we use them?

(1) How do Sodium Lamps Work

Inside the tube, there is a small amount of sodium metal, with a little neon and argon gas in there. A voltage is applied across the tube, and this excites the outer electrons in the neon and argon gas warming the sodium and also being responsible for the faint red glow that you can see before the light turns on fully. Eventually the sodium vaporizes and due to the voltage, its outer electrons too are excited. When those electrons spontaneously drop back into their ground state, they emit light at a very particular wavelength - the amber light that we see.

(2) Why are Sodium Lamps that colour?

Only one electron is excited by the electrical discharge, and only with enough energy to jump up one energy level, so when they drop back to the ground state they can only emit a very pure colour of light. The wavelength of sodium light is 589.3nm. (actually there is a little more going on, meaning there are two lines very close to one another at 589.0 and 589.6nm). This is known as monochromatic light, and it is also the reason it is hard to pick out any colour of objects lit by a sodium lamp alone.

(3) Why do we use sodium lamps?

There are a number of reasons, and I will outline a few: Sodium lamps are very efficient, because most of the energy is turned straight into light, unlike incandescent filament lamps, which turn a lot of the energy into heat. That wavelength is also pretty close to the optimal response of the human eye:

This graph (called the scotopic response curve) shows how the eye responds (side axis) to different wavelengths of light (on the bottom axis). We can see the sodium lamp is pretty close to the middle. That means that a lower level of light is needed to see things clearly.

They also use no mercury or dangerous metals, and so are easily disposed of, keeping the cost down even further.

The Science of Optics: Polarization of light, Water, Insects and 3D Cinema.

As mentioned earlier, light is a transverse wave, but as it is in 3D space (rather than on a surface like water) it can oscillate in any direction perpendicular to the direction of motion. The particular polarization depends on the relationship between the electric and magnetic field, but the simplest polarization is linear polarization - the light oscillates in a flat plane. When interacting with materials, it is often useful to be able to determine the relationship of the polarization to the material or angle of reflection. Here we will consider reflection from a mirror.

The light travels in the direction of the black line, and bounces off the mirror (the grey shape) - so the light takes a path that stays in the plane of the blue shape. The blue wave oscillates perpendicularly to the blue shape and is known as perpendicular or s-polarization. The red wave oscillates in the plane of the blue shape and is known as parallel or p-polarization. The light can also oscillate in any direction perpendicular to the direction of travel, and so some component of the light can be perpendicular, and some can be parallel.

This is very important in reflections, because different amounts of the perpendicular and parallel components can be reflected from a surface. The light that reflects from water at a shallow angle for example is almost all p-polarized light. That means if we take a polarizing sheet or polarized glasses (remember it has to be linear polarization - 3D glasses from cinemas are usually circularly polarized, so this won't work) and hold them in front of the reflection, we can cut out almost all of the reflected light and see into the water.

This image shows two photos of a puddle - one without a polarizer and one with a polarizer. The polarizer removes all of the light reflected from the surface, and so the reflection of the building disappears.

Interestingly, when locusts are swarming, they avoid areas of ground where there are large amounts of horizontally polarized light, because that means the light is reflected from water, meaning they avoid lakes and only land where there is food. You can read more about that here.

Some scattered light is also polarized, particularly light that is Rayleigh scattered. Rayleigh scattering occurs when the object that the light scatters from is very much smaller than the wavelength of light. Rayleigh scattering is stronger for shorter (bluer) wavelengths of light than for longer (redder) wavelengths. A good example of this is the scattering of sunlight that makes the sky blue.

As sunlight passes through the atmosphere, more of the blue light is scattered than the longer wavelengths, and so the sky appears blue. Just like the reflection from the water, this light is also partially polarized (though not totally, because of multiple reflections that can mess the polarizations up a bit). The polarization of the sky is in a direction that is tangental to a circle drawn around the sun.

As a result of this, insects which can detect the polarization of the light can tell where the sun is in the sky, even on cloudy days, and without being able to see the sun or shadows. Since this polarization follows the sun as it moves through the sky, this allows insects like bees to find the same patch of flowers even as the day goes on.

Circular Polarization and 3D Cinemas

So far I have described linear polarization, but light can also be circularly polarized. If we imagine some light traveling in the x direction, oscillating at an angle between the y and z direction, we can project its components in the y and z direction like this:

As we can see, they are in phase. This means they are doing the same thing i.e. they are both maximum at the same time, zero at the same time and minimum at the same time. But what happens if they are out of phase?

When we add them together, we can see that the electric field now rotates around the x-direction. This is known as circularly polarized light. The light can either spin clockwise as it moves, or counter-clockwise. Just like with the linear polarizer, we can have polarizers that let through only one circular polarization of light and block the other, and this is the technique that some 3D cinemas use - One lens blocks light that is clockwise polarized, and one lens blocks light that is counterclockwise polarized. This means that different images can be sent to each eye, and then your brain can make a 3D image from these.

Circular polarization is used rather than linear polarization, because if one image was projected using horizontally polarized light, and the other using vertically polarized light, the glasses would have to be perfectly oriented all the time, or you could keep picking up a bit of the wrong image in your eyes, making you see a double image (like you see if you take the glasses off). Circularly polarized light is not affected in this way. Note that only some 3D cinemas use this technique - others have switching glasses, that very rapidly block and unblock the eye, allowing your eye to see alternate images.

Optics and Life: Strange Sight - The world in Ultra Violet

We are all familiar with rainbows, showing us the full spectrum of colour that we can see- red, orange, yellow, green, blue, indogo and violet, but the electromagnetic spectrum continues beyond both sides of the rainbow. Red is the longer wavelength (around 600nm), and longer we have infra-red (which is pretty much responsible for the radiated heat you feel from a fire or the Sun), microwaves and the longest - radio waves. Beyond violet we have ultra violet (UV), x-rays and gamma rays.

As you can see, the actual bit of the electromagnetic spectrum that we can see is very narrow. What would it be like if we could see beyond our limited range?

Well as a matter of fact, many organisms can. Indeed it is often an essential part of their lives. Pollinating insects such as bees can see into the Ultra Violet, and it is for visibility to bees that flowers have co-evolved their colours (along with the insects ability to discern them). But you might ask - if bees can see into the UV, then what do flowers look like to them? Well often they are very different indeed, here are a few examples:

This is the common dandlion - on the left is the normal visible light image, and on the right is the UV image. This is colour shifted so we can see it, but nevertheless shows us that there is a strong two tone image, with the bright part in the middle of the flower, telling the bees where the nectar is.

This one is an evening primrose. Again yellow to us, but the insects can see lines, almost like landing strips on the runway, pointing to the pollen and nectar in the center.

UV photography does require special equipment. Firstly, you need to be able to cut out the visible light using filters, and then you need detectors that are capable of imaging the UV light, and you also need lenses that can focus the light. More information can be found here:

http://photographyoftheinvisibleworld.blogspot.com/

Other organisms can see into the Infra-red. This is particularly useful, because water does not absorb infra red light so easily as other wavelengths, and so the fish can see further.

Some can even see different polarizations of light - again many bees and insects. This is particularly useful, as it allows them to see what direction they are going in, and possibly even see predators underwater.

Lasers

We are all pretty familiar with lasers these days, from laser pens to the sorts of lasers that evil masterminds use to cut British Secret agents in half (an example here being James Bond and Goldfinger), but what are they exactly?

Laser is actually an acronym, and it stands for Light Amplification by Stimulated Emission of Radiation. let's go through the terms. Light... well we know about that. Amplification - makes things brighter - easy so far. Radiation - another word for the electromagnetic spectrum, which includes light, so again, no problem. But what about Stimulated Emission? what does that mean? To explain this, I will start off with spontaneous emission in atoms. This also works with molecules as well, but atoms are a little easier to explain.

Normally atoms rest in their ground state, all the electrons in the atom are as low as they can be. The energy levels in atoms are limited, so if we imagine them as shelves, only two electrons can go on the bottom shelf, eight on the next, eighteen on the next and so on, with as many electrons in the atom as there are protons. Now when an atom becomes excited either by being heated or when it absorbs a photon, one or more of these electrons can jump into a higher shell (I will refer the difference in energy between the lower and upper level as the energy gap) . Left on its own, the atom may only stay in this state for a limited length of time, after which the electron will then drop down again to the ground state, emitting a photon along the way. The energy of the photon is the same as the energy gap. The important thing here though, is that length of time - it is only an average and is quite random. The electron spontaneously decays to the ground state, without any influence, and the emission of the photon in this case is called spontaneous emission.

Now imagine that we have our atom in its excited state, just like before, only this time, the atom is hit by some electromagnetic radiation of the same energy as this energy gap. This can jiggle the atom and force the electron to decay back to its ground state, so now we have two photons which can then go on to hit a couple more excited atoms, and we have four photons and so on. This kind of forced decay of electrons into their ground state is called stimulated emission. The stimulated emission is usually seeded by some spontaneous emission occurring in the laser.

There are limits to this of course; for one we need to have lots of excited atoms, and once we run out of excited atoms then we can't have any more stimulated emission. To get the excited atoms in the first place we have to dump lots of energy into the lasing material, and we do this in a technique known as pumping. There are lots of ways to pump a laser, but they all amount to pretty much the same thing - dumping lots of energy into the laser material, so that when photons pass through the cavity, they can stimulate the emission of more photons. The lasing medium itself has to be something that we can excite relatively easily, and there are lots of different materials such as ruby, special glasses (like Yttrium Aluminium Garnet), dye lasers and even gas lasers like Helium Neon (HeNe) lasers and Argon Ion lasers. Probably the most familiar sorts of lasers to us now are semiconductor lasers, used everywhere from DVD players to laser pointers.

A special feature of this light is that it is coherent. If we remember the previous post about the wave properties of light, coherent means that all the photons of one frequency are oscillating in step with one another. That means they always constructively interfere. This is unlike light from a normal fluorescent or incandescent bulb, which emits incoherent light (by spontaneous emission). It is this coherence that makes lasers so powerful, and why you have to be extremely careful when using a 4W laser like an Argon Ion laser (you have to wear special glasses and even stray reflections can burn your skin), even though the actual energy it emits is far less than a 60W bulb..

Laser Cavities

To make the laser more useful and to form a stronger pulse or beam, we can take our laser pump material and stick mirrors on the ends. One of the mirrors reflects all the light, and one of them reflects almost all of the light - usually something like 99%. Now the light can bounce backwards and forwards in the cavity. These mirrors are often specially shaped to make the beam as stable as possible. You do have to be careful here though, as if the amount of energy in the cavity gets too high - the light gets too bright - then you can start to get odd effects happening in the cavity such as self focussing, which can easily blow a hole in the lasing material. For glasses of course this will break the laser and the pump material will need replacing, and this presents a problem for high powered lasers.

Hopefully this has given you an idea about the basics of lasers. I haven't delved into any of the mathematics here, but you may be unsuprised to know that Einstein was a pivotal figure here once again, as he determined that stimulated emission had to occur.