Can you paint us a picture of how we think this works based on observations in dwarf galaxies? And then as a follow-up, can you tell us what that implies for either Milky Way-like analogs in the early universe or the modern galaxies that we see in our local vicinity today?

Yeah, absolutely.

I think, you know, as I was sort of mentioning earlier, and I think is kind of a common pitfall when people are just thinking about space or any topic in science, really, we tend to think about these things as isolated.

But really, when we're talking about any type of object, it exists within some larger system.

And so the baryon cycle is is what we call the larger system that kind of governs the evolution of normal matter in these galaxies.

And it really doesn't exist in isolation from the star formation we were discussing or the mass we were discussing or the environment we were discussing.

So in the sort of simplest picture of star formation or the baryon cycle and the way that I often start to introduce it, whether I'm talking to students or even giving a talk to other scientists, Really, when we're thinking about star formation, stars in principle want to form as long as gas is sufficiently cold and dense.

It seems like there are some very key wavelengths that you need to look in as far as the information you're, you know, trying to get out of these dwarf galaxies that are that are either forming new stars or that form new stars at some point in the past, or that have their gas distributed a certain way, in motion a certain way, if you want to probe the circumgalactic medium, how important is it to have sort of this pan-wavelength coverage? And are there observatories that you think to yourself, whew, if we built this type of observatory that was good at taking this class of observations in this wavelength range, we could really answer a profound set of questions or solve a profound set of puzzles that basically has you intellectually salivating for that type of data.