H-alpha subtraction to resolve hydrogen disks

1:10:29about AI being used for LIGO for the gravitational observatory and I told you that when you have these control systems you can eliminate low frequency noise but you're going to inject high frequency noise right this thing is injecting high frequency noise right so that there's going to be some jitter >> of the star there right what you can do is you can capture that response map of a single star that's basically telling you how the instrument and this modal system that we have is responding to that jitter at every single point that the star is at. Okay. So, you've got a response map effectively being like this is what the astronomical jitter

1:11:11>> from the star is. >> Yes. Yes. >> That's from all of the light. >> Yes. >> Then what you do is you look at something called the Halpha emission line. Okay. The Halpha emission line is because of quantum mechanics. Hydrogen has discrete levels. Yes. Right. And whenever the hydrogen atom trans whenever the hydrogen atom goes from the n= 3 to n= 2 energy, it releases this red light that's right at 650 nanome about I think 656 nanome. Okay. So if we look only at that frequency of light, we're going to see the gas cloud >> the the accretion the the disc of

1:11:53hydrogen around the star. >> So what we can do is we can take an image in the Halpha line. >> We can take an image with all the light subtract the two and we'll get a nice >> hydrogen gas cloud >> that is surrounding the star. And so it's like not just that. Okay. We're now able to basically make the stars structure and the gas cloud structure discrete >> using this methodology. >> Yes. Exactly. And we can do it because this is subdiff defraction, right? >> This is we're we're going way inside what rally even thought was possible. >> Yes. Okay. Yes. That Okay. That tracks >> it's pretty cool. And and what they found is with this with this technique,

1:12:34they founded that the the disc was lopsided. >> It's not completely like a plate. It's it's not symmetric. There's like a little bulge to it that they actually saw. And there's a nonzero shift >> in that accretion disc. And that means that now the modelers can go and be like, "Okay, how do we how do we get something like this?" Right? >> What is causing that non-zero shift? >> Exactly. >> Yeah. I mean, I think I think it's really cool. It proves that, you know, you've got this compact. It's cost effective. You just like stick it in the back of the telescope. >> Right. Where the light was coming in. Now, now it goes through this other thing. >> It's It's a bolt-on. It's like a bolt-on. Yeah. Like you don't have to rebuild any of these systems from scratch. You can add this as a as a as

1:13:15an add-on and it just receives the existing feed and then processes. >> Yeah. And then process it in its own way. And there's there's I mean there's so much more that we can do with this. You can put this on a space telescope for example cuz those guys are also limited by rally but maybe not anymore. >> Um and and the last photo that we had photo 19 I just wanted to >> dwell on a little bit. There you can see the gas cloud. You can see the clear Doppler. >> Yes. Red blue shift. >> Red blue shift right between the part that's coming away from us and the part that's coming towards us. The blue is where it's coming from towards us and the red is where it's going away. And that scale bar is one >> micro >> arcsec. >> Arcsec right and I told you before that

1:13:55it used to be 20. Now you've resolved stuff to to that