Five and a half years after our proposal of the existence of Planet Nine, we have finally accomplished what is perhaps the most important task in aiding the search: we now know where to look. We've had a pretty good general idea for years now, but we couldn't really give a full assessment of the range of uncertainties for where in the sky Planet Nine might be, how massive it might be, and how bright it might be. Now we can. You can read all of the details here.

Figuring all of this out sounds somewhat straight forward. Our task is simply to take the observations of all of the distant Kuiper belt objects (KBOs) whose orbits are affected by Planet Nine and use those to determine everything we possibly can. It only took five years.

You can read the full paper for the details, but the five years consisted of a couple of critical steps:

• Understand the physics. Until we had explored all of the various ways that P9 affects objects in the outer solar system, we didn't know which objects were most critical for constraining properties of P9. Many objects are more influenced by Neptune than by P9; if we had included those the signal from P9 would basically be washed out.
• Understand the observations. There has been a lot of talk of observational bias in the population of objects in the outer solar system. Why? Because there is a lot of bias. Without fully characterizing the bias, we would have a difficult time disentangling what we are seeing from just the simple bias.
• Understand how changes to parameters of Planet Nine change the outer solar system. We accomplished this through a huge number of numerical simulations where we placed a bunch of objects in the outer solar system, added the 4 giant planets, and then added different incarnations of Planet Nine, and watched the outer solar system evolve. Every parameters of Planet Nine (almost) has huge impacts on the outer solar system. Which is good, since that means we have leverage to learn about Planet Nine from the outer solar system.
• Figure out a statistical treatment to compare the observations and the simulations. In practice this meant creating a maximum likelihood model combining the simulations, the bias, and the observations of each relevant object.
• Put it all together! Using the maximum likelihood model and what appears to be everyone's favorite statistic technique (MCMC), we now have probability distributions of all of the Planet Nine parameters.

Sorry it took so long.

Here are some fun numbers from the analysis. Planet Nine has a mass of 6.2/+2.2/-1.3 Earth masses, a semimajor axis of 380/+140/-80 AU, and inclination of 16+/-5 degrees, and perihelion of 300/+85/-60 AU. We can turn all of that into a map of where to look in the sky and of how bright and far away Planet Nine would be at any position in the sky (brightness depends on some assumption; you might want to read the detail in the paper).

That plot on top if a full-sky view going from 360 to 0 in Right Ascension. The equator, ecliptic, and +/-15 degrees of the galactic plane are shown, if that helps to orient you. The colors show the probability of find P9 at any point in the sky. The highest probability is near aphelion, around ~60 degrees in RA, pretty close to the galactic plane. Not surprisingly, this is where we have been concentrating with our Subaru search. The bottom two panes show the distance and brightness. The median distance at aphelion is around 500 AU. The median brightness is around 22nd magnitude. There is a lot of room for variation however! At its brightest predicted magnitude, P9 could be found in many ongoing all-sky surveys. At its faintest, it will require dedicated searches with large telescopes.

That plot above is truly the point of the whole paper, but there are two more plots of which I am a big fan so I want to share these also.

As mentioned earlier, there had been a lot of discussion of bias and its effect on what we see in the outer solar system. I am here to tell you bias is real. Also I am here to show you that it doesn't cause the clustering that we see.

Here is a plot that shows a lot of things all at the same time. First, lets concentrate on the green points. Those are 11 real objects in the sky and they show those objects semimajor axis ("a") versus their longitude of perihelion aka the direction their orbits point in space aka "delta varpi". The fact that 10 of those 11 are aligned is the whole reason we are here.

But wait! There is bias. Maybe those are all lined up like that simply because that's where people have looked? Now look at the blue bars. These show, for each object, the probability of the object having been found at all values of longitude of perihelion if the true longitudes of perihelion were distributed uniformly in space. There are two major regions of bias. One is at longitude of perihelion of ~90, and a weaker one is at ~300. These are caused by the DES and OSSOS surveys which both looked in very specific directions and found many objects. But that's not where the cluster is!

Now look at the red in the background. This shows how the green points should be distributed if Planet Nine were out there messing things up. Looks pretty good, no?

OK, one more: