Any chance you can get density measurements for these planets from radial velocity masses?

That would really nail it down, otherwise it could also be planet engulfment/scattering/mergers etc.

Thanks, that is indeed a more complete one because it includes the directly imaged planets!

Thanks for the pointer, that may be what I will end up doing!

And finally, you can read the entire paper here, soon to be published in ApJ:
arxiv.org/abs/2509.14101

19 /🧵

Solar system-like architectures appear for a small range of initial disk masses around F and G stars, but are not a common feature around K and M stars.

Perhaps we are somewhat special among #exoplanets?

18 /🧵

While the mid mass architecture is most efficient at depositing water directly in the habitable zone:

It's pebble snow!

#exoplanets
17/🧵

The low-mass architectures are quite efficient at creating water-worlds close to the star.

16 /🧵

The architectures are remarkably consistent across stellar mass, with the location and size of planets shifting with snow line and disk mass

15 /🧵

The mid mass architectures form a bimodal distribution:

Giant planet cores at the initial snow line location,

and a second peak with smaller, water-rich #exoplanets in the habitable zone!

14/🧵

And…

13/🧵

Low mass disks from predominantly planetary cores closer in, possible precursors to super-earths or waterworlds.

12/🧵

The main results is there are three growth modes:

High mass disks form exclusively giant planet cores outside the snow line

11/🧵