Continuing with dark energy for this post. In Post 6, we covered the equation of state (which can be thought of like this: we have two independent equations with two unknowns, so we can make an equation that relates the them. In this particular case, we want to relate energy density and pressure using a parameter that has a unique value for every type of thing in the universe, w.)
We covered in Post 6 that anything that exists in the universe with an equation of state parameter that's more negative than -1/3 could, given prevalence in the universe, cause the universe to accelerate its expansion. You can simplify thinking about this by imagining this as being like having a significant negative pressure.
We left off the end of Post 6 by noting that scientists were aware since Einstein that it was possible to have this "negative pressure" term appear in the Friedmann equations, but until the late 90's, had the expectation that this term would be zero. However, when plotting the magnitude to redshift of a special type of supernova, it quickly became apparent that the data wasn't falling in line with that term (which is called lambda) equaling zero.
So, we have a couple of mysteries up to this point in the series on our hands:
Recall also from earlier posts that the density parameter for radiation (including neutrinos) is negligible, and on the order of 10^(-5).
This would imply that in order to get a universe that appears flat, we would expect everything else in the universe that isn't matter or radiation to have a density parameter of about 0.69. But how can we be sure that lambda comprises all of that: after all, what if there are multiple different kinds of things that we don't know about making it up?
Well, fortunately, we have some ways to measure lambda and its equation of state parameter: the history of the universe's size. If lambda affects the rate of the expansion of the universe, then the scale factor of the universe would actually be different over time than we would expect it to be if we didn't consider lambda! So, what are some possible universes we could have if we had different values of lambda?
[GALLERY=media, 9521]Lambdaplot by Meow Mix posted Jul 7, 2021 at 8:17 PM[/GALLERY]
What we have here are multiple possible universes, each with the known value of the density parameter of matter (at about 0.31), but with different values for lambda. The y-axis is the scale factor of the universe at different points of time. Each different universe produces the universe that we see today (so it is not a coincidence that they all coincide with the red dot that says "now," these values were picked specifically to produce the universe that we see -- at least in terms of the scale factor).
Note that one of these universes didn't have a Big Bang, but instead went through a crunch and a re-expansion (the solid line, with the density parameter of lambda = 1.8, and curvature k = +1)! We can rule this one out by other observations. The alternating dash-dot line with lambda = 1.7289 was far too big for too long (this one is called a "loitering universe"), so it also flies against observations. The regular dashed lines with the green text represents a universe that will eventually experience a Big Crunch, but it is also younger than some of the oldest objects that have been observed.
It seems like the only value of lambda that gives us a universe like the one that we observe and measure, both in the past and the present, is the one where lambda makes up the entire "missing" 0.69 density parameter of the universe.
Let's make a phase space of every possible universe with every possible value for the density parameters of matter and lambda:
[GALLERY=media, 9522]Lambdavsmatter by Meow Mix posted Jul 7, 2021 at 8:43 PM[/GALLERY]
Here, our y-axis is possible values of lambda's density parameter. The x-axis is possible values of matter's density parameter. Since radiation's density parameter is negligible, this phase space represents every possible universe, with some details written in.
For instance, for any universe where lambda is zero (a horizontal line across from the 0 on the y-axis), such a universe is doomed to a Big Crunch as matter's gravity inevitably slows the expansion of the universe and eventually reverses it.
Everything above the dotted line is a positively curved universe, and everything below the dotted line is a negatively curved universe.
If you recall, observationally, we know that the universe is flat: even with the very basic information given in this series, the reader should be able to know that the universe we inhabit falls somewhere on that dotted line (which is where k = 0, curvature is zero).
Understand that prior to the late 90's, the expansion of the universe wasn't thought to be accelerating: it was thought to be constant at most (so, where the dotted line meets the red line) or, more likely, decelerating because gravity would constantly be fighting the expansion (so, anywhere on the dotted line beneath the red line could have represented the universe we live in as far as they knew at the time).
So, let's bring a few things we've talked about over the entirety of this post together on this same plot:
[GALLERY=media, 9523]Concordantcosmology by Meow Mix posted Jul 7, 2021 at 9:40 PM[/GALLERY]
When we plot constraints together, they look like we'd imagined them to, they converge in the same location at their highest confidence levels (the lighter the color, the lower the confidence level); and, most importantly, they happen to converge somewhere that makes sense based on everything else that we've covered in these posts.
What you should get out of this is that this is like finding three clocks running on independent mechanisms agreeing on the same time: it's not a coincidence. It tells us we're on the right track. (This particular mode of constraints is currently called "convergent cosmology.")
So, where do the constraints put us? It looks like our universe is most likely on the k = 0 line as we expected, where the density parameter for matter is around .3 as expected, and where the density parameter for lambda is about .7 as expected.
There is a lot more to this, but as I promised, I have tried to keep this series from becoming too dense or technical for most readers to digest. Thus I will conclude the series with the hope that now you know a little bit more about why cosmologists are able to make a reasonable consensus about the existence of dark matter and dark energy.
----------------------------------------------------------------------------------------------
Addendum: the equation of state of dark energy
We can use similar convergent cosmology constraints to help lock down what dark energy's equation of state might be. Remember, we expected it to be more negative than -1/3 to account for the observation that the universe is accelerating its expansion (as shown by supernovae in the post before this one):
[GALLERY=media, 9524]Eosparamconstraint by Meow Mix posted Jul 7, 2021 at 9:42 PM[/GALLERY]
[GALLERY=media, 9525]Eosparamconstraint2 by Meow Mix posted Jul 7, 2021 at 9:42 PM[/GALLERY]
Not all of the constraints are pretty, but again we at least find constraints that make sense.
Keep in mind that at any time, if the data tells us something that doesn't make sense, then we have a good indicator that something is wrong somewhere with the models and understanding. While we may not have perfect knowledge about the nature of dark matter or dark energy, we have at least correctly inferred their existence and impact on the universe at large.
We covered in Post 6 that anything that exists in the universe with an equation of state parameter that's more negative than -1/3 could, given prevalence in the universe, cause the universe to accelerate its expansion. You can simplify thinking about this by imagining this as being like having a significant negative pressure.
We left off the end of Post 6 by noting that scientists were aware since Einstein that it was possible to have this "negative pressure" term appear in the Friedmann equations, but until the late 90's, had the expectation that this term would be zero. However, when plotting the magnitude to redshift of a special type of supernova, it quickly became apparent that the data wasn't falling in line with that term (which is called lambda) equaling zero.
So, we have a couple of mysteries up to this point in the series on our hands:
- Observations reveal that we can no longer ignore lambda (which can be thought of in a simplified way as a "negative pressure"). However, what is the density parameter of lambda: how much of the universe's energy density comprises this "pressure?" (Covered in this post)
- What is lambda's equation of state parameter: what is the relation between its energy density and its pressure? (Covered in the addendum to this post, at the bottom)
Recall also from earlier posts that the density parameter for radiation (including neutrinos) is negligible, and on the order of 10^(-5).
This would imply that in order to get a universe that appears flat, we would expect everything else in the universe that isn't matter or radiation to have a density parameter of about 0.69. But how can we be sure that lambda comprises all of that: after all, what if there are multiple different kinds of things that we don't know about making it up?
Well, fortunately, we have some ways to measure lambda and its equation of state parameter: the history of the universe's size. If lambda affects the rate of the expansion of the universe, then the scale factor of the universe would actually be different over time than we would expect it to be if we didn't consider lambda! So, what are some possible universes we could have if we had different values of lambda?
[GALLERY=media, 9521]Lambdaplot by Meow Mix posted Jul 7, 2021 at 8:17 PM[/GALLERY]
What we have here are multiple possible universes, each with the known value of the density parameter of matter (at about 0.31), but with different values for lambda. The y-axis is the scale factor of the universe at different points of time. Each different universe produces the universe that we see today (so it is not a coincidence that they all coincide with the red dot that says "now," these values were picked specifically to produce the universe that we see -- at least in terms of the scale factor).
Note that one of these universes didn't have a Big Bang, but instead went through a crunch and a re-expansion (the solid line, with the density parameter of lambda = 1.8, and curvature k = +1)! We can rule this one out by other observations. The alternating dash-dot line with lambda = 1.7289 was far too big for too long (this one is called a "loitering universe"), so it also flies against observations. The regular dashed lines with the green text represents a universe that will eventually experience a Big Crunch, but it is also younger than some of the oldest objects that have been observed.
It seems like the only value of lambda that gives us a universe like the one that we observe and measure, both in the past and the present, is the one where lambda makes up the entire "missing" 0.69 density parameter of the universe.
Let's make a phase space of every possible universe with every possible value for the density parameters of matter and lambda:
[GALLERY=media, 9522]Lambdavsmatter by Meow Mix posted Jul 7, 2021 at 8:43 PM[/GALLERY]
Here, our y-axis is possible values of lambda's density parameter. The x-axis is possible values of matter's density parameter. Since radiation's density parameter is negligible, this phase space represents every possible universe, with some details written in.
For instance, for any universe where lambda is zero (a horizontal line across from the 0 on the y-axis), such a universe is doomed to a Big Crunch as matter's gravity inevitably slows the expansion of the universe and eventually reverses it.
Everything above the dotted line is a positively curved universe, and everything below the dotted line is a negatively curved universe.
If you recall, observationally, we know that the universe is flat: even with the very basic information given in this series, the reader should be able to know that the universe we inhabit falls somewhere on that dotted line (which is where k = 0, curvature is zero).
Understand that prior to the late 90's, the expansion of the universe wasn't thought to be accelerating: it was thought to be constant at most (so, where the dotted line meets the red line) or, more likely, decelerating because gravity would constantly be fighting the expansion (so, anywhere on the dotted line beneath the red line could have represented the universe we live in as far as they knew at the time).
So, let's bring a few things we've talked about over the entirety of this post together on this same plot:
- We get a very accurate measurement of matter's density parameter using galactic clusters, as discussed in the dark matter sections of this series. If it very accurately constrains matter, then we would expect this data, when plotted, to be very vertical with as little thickness as possible (meaning it is saying, "matter's density parameter is between here and here.")
- Baryon acoustic oscillations (also covered in the dark matter section) constrain both lambda and matter density parameters, so we would expect this data, when plotted on this graph, to constrain along the line of curvature since it is very sensitive to the components that go into this.
- We use type 1a supernovae over large ranges of redshifts to give us an understanding of the actual relationship between scale factor vs redshift over time: only certain combinations of density parameters would allow for these observations, so we'd expect this data (when plotted) to cover a range of values of lambda and matter, manifesting diagonally on the plot.
[GALLERY=media, 9523]Concordantcosmology by Meow Mix posted Jul 7, 2021 at 9:40 PM[/GALLERY]
When we plot constraints together, they look like we'd imagined them to, they converge in the same location at their highest confidence levels (the lighter the color, the lower the confidence level); and, most importantly, they happen to converge somewhere that makes sense based on everything else that we've covered in these posts.
What you should get out of this is that this is like finding three clocks running on independent mechanisms agreeing on the same time: it's not a coincidence. It tells us we're on the right track. (This particular mode of constraints is currently called "convergent cosmology.")
So, where do the constraints put us? It looks like our universe is most likely on the k = 0 line as we expected, where the density parameter for matter is around .3 as expected, and where the density parameter for lambda is about .7 as expected.
There is a lot more to this, but as I promised, I have tried to keep this series from becoming too dense or technical for most readers to digest. Thus I will conclude the series with the hope that now you know a little bit more about why cosmologists are able to make a reasonable consensus about the existence of dark matter and dark energy.
----------------------------------------------------------------------------------------------
Addendum: the equation of state of dark energy
We can use similar convergent cosmology constraints to help lock down what dark energy's equation of state might be. Remember, we expected it to be more negative than -1/3 to account for the observation that the universe is accelerating its expansion (as shown by supernovae in the post before this one):
[GALLERY=media, 9524]Eosparamconstraint by Meow Mix posted Jul 7, 2021 at 9:42 PM[/GALLERY]
[GALLERY=media, 9525]Eosparamconstraint2 by Meow Mix posted Jul 7, 2021 at 9:42 PM[/GALLERY]
Not all of the constraints are pretty, but again we at least find constraints that make sense.
Keep in mind that at any time, if the data tells us something that doesn't make sense, then we have a good indicator that something is wrong somewhere with the models and understanding. While we may not have perfect knowledge about the nature of dark matter or dark energy, we have at least correctly inferred their existence and impact on the universe at large.