 Okay, so we've got another lightning talk on the Pictor telescope a free to use and open source radio telescope Okay, thank you very much. Hello everyone. My name is a post loss In this lightning talk, I will present to you a picture which is a free to use an open source radio telescope that allows Anyone from all around the world to observe the radio sky for free So let's start a little introduction So this is our galaxy. I think most of you have already seen this image, maybe But how did we take this image? Well, of course, we didn't send a spaceship there. That's a bit too far but So how did we compose it? Well, we synthesized it. This is an artist conception Mostly using radio astronomy So, you know, if you if you've seen the the galaxy at night the Milky Way band You may not really be able to tell if we even live in a spiral galaxy So today we'll try to prove this to you with a live observation So let's start with the electromagnetic spectrum. I think you've all seen this sketch So in the middle part, we have the visible spectrum. This is a spectrum that we see with our own eyes This is where most astronomy takes place in and of course, we have some invisible Wavelengths like x-rays gamma rays infrared ultraviolet microwaves and of course radio, which I will focus on today So now under certain conditions had a Neutral hydrogen atom can emit radiation a photon with a wavelength of 21 centimeters. It's called the spin flip transition Which is responsible for the productions of the obvious waves and as you know, our galaxy is full of hunt full of hydrogen So we can detect the these fire alarms. You see, this is an all-sky map and in the center. We have the Milky Way Hence why it's so bright and at 420 megahertz. This is this corresponds to wavelength of 21 centimeters So we wanted to build a radio telescope that can detect this very very faint radiation and make it available to everyone To use online for free without any registration advertisements or anything like that so we began planning some We've gone with some simulations for the antenna. This is a fit home simulation using electromagnetic solvers This is a simulated radiation pattern and after that we decided to build the the antenna and got it measured in the lab This is the telecommunication system laboratory of the Department of Digital Systems of the University of Peru's We got the graphs and everything. This is S11 of the monopole for those familiar with RF systems And of course women we measured the entire feed home Which made it made the monopole a bit more wide band So let's look at some stats It's a it's it's got it's a parabolic antenna with a diameter of 1.5 meters So it's a large dish it can operate from from 1300 to 700 megahertz So if anyone doesn't want to observe the hydrogen line, he can look at a different frequency They have far beam width. This is like the field of view. It's about nine degrees and Most importantly, it's got a filtered LNA very low noise amplifier with a point five DB noise figure And of course, it's fully open source So anyone can take the code and build his own so this is what the telescope looks like and its current form and This is this is basically the the data acquisition flow graph Digital signal processing. It's based on polyphase filter banks spectrometer This is new radio many of you know this and You can find the full documentation here on Made a separate documentation just for this flow graph So how does it work a single end of the feedhorn gets amplified filter and then amplified This is a two-stage low noise amplifier and runs through a three meter low low loss cock the coaxial cable Then runs through a far out the cage to reduce as pure as emissions to the telescope Which is undesired runs through by ST and as they are and of course the Raspberry Pi So let's why don't we make an observation? So to make an observation a user simply Simply goes to picture telescope.com And you can scroll down. I've got the github here and everything check some Information out and I've also written a PDF in English. You can take a look at that. It has some introductory radio astronomy information So maybe that's something you're interested in for beginner users, for example So we have here some a form. It tells you where the telescope is pointing to Right now it's in Zenith so direct overhead so it allows us to for example put an observation name like Like force is an example Sender frequency we wanted we want to observe the hydrogen line. So 40 and 20 megahertz sounds reasonable Bond width you can go up to 3.2 megahertz, but 2.4 is usually sufficient Then we have the number of channels. This is the FFT size 2048 is usually fine It's more than enough And you have the number of pin which basically determines the integration time for FFT sample This won't really affect your signal to noise ratio. It's usually for interference mitigation and other kinds of things so duration let's just put 20 seconds and input our email address So if we hit Let's run this again So we said false them Okay, 20 second duration and our email address right, let's Enter, okay So now the observation is running and the telescope just picks up this This observation. Let's actually look into this in more detail So what happens is the user Loads observation page checks the server checks if the if there is an observation running And if not it permits the user to submit an observation with his desired parameters So then the telescope awaits the observation request checks if it has already been run And if not then it runs the observation does some digital signal processing including RFI mitigation, etc. And then sends the The data to the observer via email. So the user can just go into his email and check the observation data So I think we should have received the observation now Let's give it a second It usually takes maybe a minute or two for the email to arrive. Okay, there we go So we have here the the observation parameters that we entered Bond with sample rate number of channels and everything Now over here we have the graphs so that the telescope data So we have four graphs in total. This is the average spectrum. This is the calibrated spectrum so this is what the SDR receives and You can see a very faint peak there, but you also see some three hams So this this is called the bandpass shape and it's due to the it's like an SDR artifact So if we calibrate that it becomes flat and we can see the hydrogen line a lot more clear so What would we see here in this in this peak? This is the hydrogen line this corresponds to a unique spiral arm in our galaxy Specifically, this is the the sickness arm. So our whole spiral arm of the solar system And we have two more graphs The waterfall which basically shows you the entire data. It's just not very easy to see hence why you have some more graphs And of course power versus time Okay, so if we go back to the presentation Okay, so this is another example of observation taken at an even better time. You can see three three peaks here So it's each of those peaks corresponds to a different spiral arm in our galaxy So with just an observation with this you can get such data in like 60 seconds, for example You have proven you have detected three unique spiral arms of the galaxy So you've proven that the Milky Way is indeed like we do in Italy We do indeed live in a spiral galaxy. It's not very easy to prove using optical measurements So let's look at the Let's look at some statistics So picture has been used From 360 plus unique users from all around the world We have 2.3 thousand observations on the archive Imagine our goal was to hit a hundred unique users in a year and In less than a year in just a few months. We reached so many users, which is great And these users include students, teachers, educators, professors, amateurs and even professional astronomers So some future plans We have a lot of plans for the future regarding radio astronomy One of them is the development of a similar educational instrument for for pulsar education and may be be part of research As part of the pulsar monitoring network, which will be dedicated for for glitch research Pulsar glitch is basically an open issue in no one problem in science because What it means is the pulsar pulsar is a neutron star It presents a sudden a sudden Decrease a sudden change in the in the in the spin period So we're looking to research more into that and Of course, we have Lyronet, which is which will be a global network of open-source radio telescopes This include some small and large dishes the largest one right now is 18 meters in the amateurs It's a huge huge dish and we have some many many more and This this network will be for research and education as well So we have plenty of plans for that and last but not least We'd like to thank a libero space foundation for their support and the support with the stickers and also helping us build another Antenna that will also be part of Laronet. So Yeah, thank you very much and of course feel free to take any stickers you want from over there and I'll be happy to take some questions Okay, so the question is what's the cost of designing the such telescope? Yes, so it depends on the diameter of course and what back and you will use and what are front end So maybe you you want to go with some even lower noise amplifiers some better filters Larger dish, you know Maybe you want to make it more wideband So there's a lot of options You can design a telescope like picture for you know a few hundred bucks maybe less We just designed a new one called nano RT nano radio telescope, which looks like an optical telescope. It's very very small This this costed under a hundred so there's a lot of possibilities and if anyone wants to To build a radio telescope they can really do this. I mean I've written all the software for you So you don't have to go through this work as well Any more questions? Yes So the telescope basically points constantly to the neath so you can use students can use something like like a Plantarium virtual plantarium software like a stararium to to see what the telescope is pointing to so The the elevation sometimes changes for example on requests Like if a student which is to observe the moon or the Sun for example, then they tell us can you can you please shift it to a certain elevation and They they often perform drift scan observation So they don't have in the case of the moon and the Sun You don't have to observe at 14 20 megahertz because you're not looking to observe the hydrogen line We're looking to observe something much closer so in the case of of a Sun or a lunar lunar drift scan observation you what you're looking for is the power versus time In this case you should see the power being mostly flat and slowly rising Forming a Gaussian curve and then you know going straight like so you basically see a peak when the When the Sun or moon enters your your field of view of the beam of the telescope any any more questions? Okay, thank you very much. Thank you