“Youth is the gift of nature, but age is a work of art.” -Stanislaw Jerzy Lec

Each week at Starts With A Bang, we cover a whole slew of topics on the wonders of the Universe. Throughout, you have the opportunity to send in your questions and suggestions for our weekly Ask Ethan column, and at the end, I pick one to highlight, showcase and answer. This week’s choice won’t just be answered by an Ethan, it was also asked by one: Ethan Barbour, who wants to know about the age of the Universe:

I have an astronomy question, and it is basically this: how many independent ways can we measure the age of the universe?

I’d love to tell you that there are all sorts of different lines of evidence that point to our 13.8 billion year age, similar to how there are so many independent pieces of evidence pointing to dark matter. But in reality, there are only two good ones, and one is better than the other.

Image credit: NASA / GSFC / Dana Berry, via http://svs.gsfc.nasa.gov/cgi-bin/details.cgi?aid=10128.

The “good” one is to think about the fact that our Universe is expanding and cooling today, and to recognize that it was therefore hotter and denser in the past. If we go back, to earlier and earlier times, we’d find that as the volume of the Universe was smaller, all the matter in it was not only closer together, but that the wavelengths of all the individual photons (particles of light) in it were shorter, as the Universe’s expansion has lengthened them to be as long as they are today.

Image credit: Take 27 LTD / Science Photo Library (main); Chaisson & McMillan (inset).

Since a photon’s wavelength defines its energy and temperature, a shorter-wavelength photon is more energetic and higher in temperature. As we go back farther and farther in time, the temperature goes up and up, until at some point, we reach the earliest stages of the hot Big Bang.

This is important: there is an “earliest stage” for the hot Big Bang!

Image credit: wiseGEEK, © 2003–2014 Conjecture Corporation, via http://www.wisegeek.com/what-is-cosmology.htm#; original from Shutterstock / DesignUA.

If we were to extrapolate “infinitely” far back, we’d reach a singularity, where physics breaks down. With our modern understanding of the very early Universe, we know that an inflationary state preceded the hot, dense Big Bang, and that inflationary state was of an indeterminate duration.

So when we speak of “the age of the Universe,” we’re talking about how much time has past since the Universe could first be described by the hot Big Bang until the present day.

Image credit: Bock et al. (2006, astro-ph/0604101); modifications by me.

Under the laws of General Relativity, if you have a Universe like ours, which is:

of uniform density on the largest scales,

which has the same laws and general properties at all locations,

which is the same in all directions, and

in which the Big Bang occurred at all locations everywhere at once,

then there is a unique connection between how old the Universe is and how it’s expanded throughout its history.

Image credit: NASA, ESA, and A. Feild (STScI), via http://www.spacetelescope.org/images/heic0805c/.

In other words, if we can measure how the Universe is expanding today and how it has expanded throughout its entire history, we can know exactly what all the different components are that make it up. We learn this from a whole host of observations, including:

Image credit: ESA/Hubble and NASA, via http://www.spacetelescope.org/images/potw1004a/.

From direct measurements of the brightnesses and distances of objects in the Universe such as stars, galaxies and supernovae, allowing us to construct the cosmic distance ladder.

Image credit: Sloan Digital Sky Survey.

From measurements of large-scale-structure, the clustering of galaxies, and from baryon acoustic oscillations.

Image credit: ESA and the Planck Collaboration.

And from the fluctuations in the cosmic microwave background, a “snapshot” of the Universe when it was a mere 380,000 years old.

You put all of these things together, and you get a Universe that is made up, today, of 68% dark energy, 27% dark matter, 4.9% normal matter, about 0.1% neutrinos, about 0.01% radiation, and pretty much nothing else.

But you throw in how the Universe is expanding today, and we can extrapolate this back in time, and learn the entire expansion history of the Universe, and hence, its age.

Image credit: E. Siegel.

The number we get — most precisely from Planck but augmented from the other sources like supernova measurements, the HST key project and the Sloan Digital Sky Survey — is that the Universe is 13.81 billion years old, with an uncertainty of just 120 million years. This means we’re confident in the age of the Universe to 99.1% accuracy, which is an amazing feat!

Yes , we have a number of different data sets that point to this conclusion, but in reality, it’s all the same method. We’re simply fortunate that there is a consistent picture that they all point towards, but in reality, any one of the constraints themselves is insufficient to say “this is exactly how the Universe is.” Instead, they all offer a variety of possibilities, and it’s only their intersection that tells us where we live.

Image credit: Suzuki et al. (The Supernova Cosmology Project), accepted for publication, Ap.J., 2011., via http://supernova.lbl.gov/Union/.

If the Universe had the same current properties today but were made of 100% normal matter and no dark matter or dark energy, our Universe would be only 10 billion years old. If the Universe were 5% normal matter (with no dark matter or dark energy) and the Hubble constant were 50 km/s/Mpc instead of 70 km/s/Mpc, our Universe would be a whopping 16 billion years old. With the combinations of things we have today, however, we can confidently state 13.81 billion years is the age of the Universe, with a very small uncertainty. It’s an incredible feat of science.

And that’s legitimately one method. It’s the main one, it’s the best one, it’s the most complete one, and it’s got a ton of different pieces of evidence pointing towards it. But there is another, and it’s incredibly useful for checking our results.

It’s the fact that we know how stars live, burn through their fuel, and die. In particular, we know that all stars, when they’re alive and burning through their main fuel (fusing hydrogen into helium), have a specific brightness and color, and remain at that specific brightness and color only for a certain amount of time: until their cores start to run out of fuel.

At that point, the brighter, bluer and higher mass stars begin to “turn off” of the main sequence (the curved line on the color-magnitude diagram, below), evolving into giants and/or supergiants.