Fel yna, Nathan, mae yma'n ymddangos i'ch cyfrifedd yr ERC-draid ymddangos, wrth i'ch ei gael ymddangos i'ch cyfrifedd ymddangos ymddangos ymddangos. Felly mae'r project 5 ymddangos, ac mae gennym nhw i'ch gael i'ch gael i'ch gael i'ch gael i'ch gael. I boQuewch i'n hayf ar gyfer o'r gwahod o'r wych nghylchau'r gweithio. Fy'r gwahod o'r wych yn deall, a yn ychynid. Oes gobeithio, mae gennym eisiau eu gyn bob un o'r gweithio. Felly y maen nhw'n gwisio rwy'n cael ei wneud y bod ni wedi'u cefnwyr yn y rhaid, ac roedd ni'n gobeithio fod wedi eu gwahod gyda sicrhau y wneud yma. sy'n dewis eich cyfeirio y cyfnod. Rwy'n cyfle, yn dda, dweud hynny'n gorfod rhywbeth yna dweud hefyd i'ch mas Ym Mмыnydan, ond Rhaid Ddweud ers Ym Mwynydan yw ddim. Mu'n dwylo dweud, oherwydd rwy'n oed yn gallu nhw'n oeddod i dda i ddatganiadol yn y cwngor, ac mae'n ddweud i gweithio'r tyfu. Rwy'n oedda i ddweud i'r cyfoes. Mae'n meddwl doesion hynny. Rwy'n oeddod i'r cyfeirio mewn i'w ddiwylliant oherwydd Gwethech chi'n cael ei wneud yn eich amser yma. Rydyn ni'n gwneud fyddai'r phwysig fyddai'r cwmwysig ystafell hynny, ac mae'n arwain iawn gwybod ei ddweud yn ei ddweud yn bwysig yn Zotero, ac mae'n gallu gwneud yn gwneud yn y llyfr. Dw i'r ddweud o'r 25 yma, mae'n ddweud'r llai yn y llai, mae'r hynny'n fawr yn ei ddweud yn fawr yn bwysig yn bwysig yn bwysig yn bwysig yn bwysig yn bwysig. I'm happy with that. I'm not going to go back and re-enter everything into Zatira. That's the sort of point I'm going to make. I want everything to be as efficient as possible without me having to go and do huge amounts of manual processing of data. Okay, so I will move on what's, oh gosh, updates ready to install. That's not what I want. Council. Here we go. Okay, so very simple. The project is really quite simple, especially, you know, if you look at it compared to Beyond Boundaries, we've got primary outputs, 10 critical editions of Sanskrit texts on yoga, ranging from about the 11th century to the 19th century. Four monographs and, as I say, umpteen articles, I can't remember. There's probably about 20 journal articles we're going to be producing by the end of it. And our data for producing those primary outputs is, so the primary data categories are scans of manuscripts and published editions. Okay, so we've got one of the project team members that's spent probably most of the last two years in India going round manuscript libraries collecting scans where he can. And also, of course, there are lots of, you know, some of the texts we're working on have been edited in some way, so we try and track down some of the editions that are very obscure, but we track them down and we use scans of those as well. And then the two primary methods in the project proposal are philology, so the editing of these texts and ethnography. So we've got one full-time ethnographer on the project as well. And she spent probably half, you know, already over a year in India searching out traditional yoga practitioners, interviewing them, taking photographs, filming them and so forth. So she produces that ethnographic data. And then a sort of, we didn't flag it up quite so much in the project proposal, but a pretty key part of our work as well, our key source of information, are historical, are historical materials that depict yoga practice. And I'll talk a bit more about all these categories in a minute. Now, where I think, at the moment, the way we store this data is fairly unsystematically, we're not, you know, tagging it with loads of metadata and so forth. I think Daniela is a bit with her ethnographic stuff, but probably not to the degree that would meet the usual requirements at the moment. We've got a shared Google Drive folder and then everything comes down to our personal laptops and then we all back that up on external hard drives and that's it at the moment. But I will talk about the plans for the future now. So yeah, looking at the philological side of the project, the text data processing. So the process of that is we get all the witnesses, we kind of a text, but we start before we've got all the witnesses, which is an ongoing process, and collate those witnesses, those manuscripts. Now, in the project proposal, I did put some fancy stuff in about clodistics. Does anyone know about clodistic called stemmer analysis? But to be honest, since I've looked into it, since the proposal, I've become more and more sceptical about clodistical analysis and I don't think we're going to use it at all. There are various problems with it. Not least, what it is, it's a way of forming a stemmer of a manuscript tradition modelled on genetic analysis, and one of the problems is that you can only fork in two ways. You're going to have a bifocatio, you can't have a trifocatio, and of course, we all know that one manuscript might get copied by more than two scribes, so instantly breaks down there, and it also can't take into account contamination between branches of a stemmer. So this is one of the examples of things where there's a bit of a fashion in indology at the moment, and certain people are really promoting this, but I'm extremely sceptical about it, and I think actually what would be very beneficial would be a project looking at exactly that and seeing whether it is helpful or not, because I don't think anyone's… People don't seem to be questioning it. That seems to be a problem with some of the digital tools available. People just think, oh great, digital humanities is a new digital tool, let's go for it, and I think we need to be a little bit sceptical. Again, for collation, there are tools for collating large bodies of witnesses and so forth, and in fact, when I started my PhD in 1995, I was urged to use this new programme, Collate, that was being developed in Oxford, but again, I think that it actually cost me a lot of time doing that. First of all, you have to read the manuscript, and you have to transcribe it, and then you have to break it up into little chunks that can then be prepared, and I honestly think it probably wasted months of my time doing that, and I wouldn't do that again. Then there's… So, after you've collated your witnesses, there's the editing process. Now, fortunately, well, especially since I've discounted systematic analysis, again, with our texts, we always have contamination, so you can't do rigid mechanical systematic analysis, so the editing really is a… We need to do it. I don't think any digital tools yet have been developed in any way that would be able to perform the editing job on our texts, and then finally, once we've collated and edited, we want to produce the edition for publication. Now, what we're going to do with our project is every edition we're going to produce finally in XML and the TEI encoding that's been developed, especially for the SARIT project. Now, again, in the project proposal, I got all excited and wrote, it seemed like it would be practicable at the time, whereby from the XML SARIT file, you could then process it two ways. You could either go just at the touch of a button that could be converted into Lartec and then a PDF, so book publishing form, or the other way into HTML. I think I've got some pictures for those of you who… Here's an example of a SARIT file. You can't see it, but it's a website. It's got not a huge number of texts yet. I mean, that's one of the problem of these things is there's only a small body of text. Actually, I don't think many endologists are using it as a search tool, but it's very good for presenting a single text, and also we know it's sustainable. It's funding. It's just got a new round of funding from Heidelberg and so forth, so those texts are going to be there for a long time. There's an output file, a PDF produced by Lartec, of a critical edition, and then there are these fancy, very impressive HTML outputs you can get. This was developed by Charles Lee, who's at Cambridge. This is a very nice front-end. You can see at theSaptomIver.org, where you can alter all the parameters of which manuscripts you're looking at and so forth, and it will generate an additional apparatus. This is another one. I was hoping to be able to go live onto the internet, but I don't think I would attempt to do that now. Andrew Ollett developed this one whereby, again, from an XML file, you can wave your mass over these highlighted bits of the edited text, and the variants will pop up by magic. This is what I think we want to do, is we want to make our editions, we want people to read our critical editions, and this seems to be a very good format to encourage people to look at the variants. One of the things we've been talking about yesterday was documenting the process of our research, of working with this data, and whether we need to do that, whether we need to make that available. I was reminded of this a couple of days ago when a friend posted this on Facebook. It's one of Daniel Ingalls's notebooks. He's been going through some Harvard archives, trying to understand how a great scholar Ingalls produced various of his works. I think it would be somewhat hubristic to assume that people might want to do the same with our work. Also, this is something I've thought maybe we could raise in the discussion. I'm not going to go too much further into it, but I don't really see how one would be able to record the process of editing. I'm not sure it's particularly useful. As I say, it's hard enough to get people to read critical editions in the first place, let alone go through the mechanics of how they were made. I will one little aside. There's one moment, I was talking about this a few months ago with some colleagues, when one's editing a text, there's one moment I think would be nice to record. I haven't worked out a way of doing it. You've collated a few manuscripts. A bit of the text doesn't make sense, so you come up with a brilliant emendation, and you record it in your critical edition, then you collate another manuscript, and there it is. Your emendation is now recorded in the manuscript, and you think, yes, I was right. Then there's that sinking feeling when you realise that now, in the addition, you're just going to be recording that witness and not your brilliant emendation anymore. That would be one interesting thing to go back for. There should be some sort of German word for it, I think, for that feeling. Anyway, that is how I move on. Now also with all our data, our primary source of data is manuscript sources, and I know we're meant to make everything available, particularly with this ERC funded project, but the thought of trying to get permission from all Indian libraries to actually make, even once you've got the scans, to then be allowed to put them online and make them publicly available just fills me with absolute horror. I got this email yesterday from Jason, who's one in India at the moment, going around the libraries. Let's just give you a new example. We went to the Sanskrit College's library today only to learn that the uncle of the librarian had died that morning, and the librarian had gone to a village some distance from coach interview with her family. We met the principal and she was very nice. She said the librarian is a custodian of the library, and she's the only one with a key. What can I do? You must come back on Wednesday. Just seeing the manuscripts is often a triumph, and then getting permission to scan them, but getting permission to make them public, I think, that would be a whole another five-year project, probably for each library in itself. That's not something we're considering. I was also relieved to see this. This is also the hot off the press, just two or three days ago. It's not only us. It's not only foreign scholars, even Baba Ramdev, who's tight with the government. He's a Ayurveda yoga guru, stroke businessman entrepreneur. Even he's having trouble getting hold of manuscripts from the government repository in Delhi. This is a problem in our work and pretty insurmountable, I think. It's not getting any easier, put it that way. Okay, so that's the textual data. Now I've got until the hour, haven't I? It's your type. Good. Now I'm going to look at our historical data. I'll give you an example, basically. I'll give you some examples of the stuff we work with and what we might do with the photographs and scans that we have. This is probably the most exciting discovery we've made so far. This was last year. I and Daniela came to this gate on it. I just see one passing note in a Hindi article about it, and there were some, meant to be some statues of some famous yogis at the bottom. But then, and it happened to be on our route, it's this rather obscure little town in Gujarat. Then we noticed when we were looking at the famous yogis here in relief, and then up in here all these yogis doing complex yoga postures. This makes them the oldest such statues by about 300 years. It's a very exciting discovery. We got some rather bad photographs at the time. I don't know if you can tell what's going on, but actually you can from this. We then went back and got some better photographs. That was a whole saga in itself. I went with Mark Singleton as my colleague on the project with Indian photographer. That, again, is worth a book in itself, the story of how we got these photographs. I won't go into it now. But again, I'm wondering, do we need to preserve the story of the different levels? We've got about three or four sets of photographs of this gate getting better and better. Presumably we just want to publish the best ones. Although just go back to this one. I don't know if you can make it. Now it was quite handy having the pigeon on the top. I don't know if you can see it, because at least with that one I can prove I haven't just turned the photograph upside down. It's not someone sitting in lotus posture. Now the other sort of sources, we use one in particular that I've worked with a lot, mughal miniatures of yogis. What we found, particularly with the mughal miniatures, incredibly they're very, what's the word, there's a realist, there's an art historical term, but they really seem to depict real characters and by analysing the insignia and the very fine details in these miniatures, we can kind of, I've used that to map the history of yoga practices and also certain sects of yogis. So here I'm showing this one because of, I've spent much too long looking at the position of earrings in yogis ears and you see here there in the ear lobes and then there was an important shift a couple of hundred years later when the earrings move into the cartelages. Now this is a very sort of specific minor example but what, the point is this is a very useful tool for analysing the history. In fact, Nicety Doward at the back actually his work I think I reference when I'm going on about earrings, but these images are very useful tool but I've got thousands of them on my computer, completely disorganised. Now they also in tandem with ethnographic images, so here's a photograph of a yogi I took at Cumbul Mela in their 2013 and then we can compare that. Actually this is an image from the same album as the previous image I showed, so we know this is a sort of ancient ascetic yoga practice. Meanwhile, the same yogi of today is doing things like this which we have no precedence for and in fact seems to be derived from western modern yoga and tradition. So what I want to do with all these images and it's not written into the project but I've just put in a proposal to the Welcome Institute and hopefully that might come through but I'm determined to make this happen. I've got a part-time PhD student who's all ready to use the other half of her time to input to create a big database of yoga images. So to be something, we're not sure where we're going to host it, that's all depends if we get the funding and so forth, but to that is something I can really see the use of if we tag all these images with metadata, both historical, modern images, we can say lotus position in the 17th century by a female yoga name, we can bring up all the pictures of that and then that would be extremely useful for tracing the history of yoga. So that's what I plan, that's in the dream world what will happen with all the photographic, the image data that we've got as part of the project. And that is it I think, that's all I was going to say about our data. As I said I'm open for throw tomatoes at me rotten eggs, I'm worried that we might be doing something very wrong but we're in the perfect position now, as I said we're two years in, we've amassed a lot of data, I think we're over the hill of manuscript scan acquisitions so now is a good time to be planning for what we're going to do with all that data and how we store it and how we present it and so forth. Okay thank you. I'm going to abuse my prerogative here and ask the question and make comments over the comment. Jeff will tell me that if you have filmed the manuscript it's and it's pre-modern there's no legal issues to share it. It may be extremely rude to the owner of the document legally it's okay but what worries me is that then may jeopardize future scholars going to get the scans of other manuscripts. Then I'll also point out that on Zanodo you can have an embargo period so you could upload all of those and say make this open access in 50 years and now whether or not you believe that will work in terms of what the world will be like for the years from now is not a question but it might be worth thinking about particularly in terms of compliance questions. With the ELC. So it's absolutely the adamant that you have to make all data available publicly available. That's maybe a different discussion but if you did want to make data publicly available without defending people in India you couldn't embargo it with a long environment. And then my question is about your metadata so for instance you have pictures from google books and pictures of the you took in the combi mail and how are you keeping track of like who took this when where what library holds this miniature that I do a picture of? Completely haphazardly to be honest. That's why people send me images all the time. I haven't got time to you know input metadata for all of them. I suppose that my photographs and Daniela's Daniela does give good metadata with you know stores keeps good metadata with her photographs so that's probably a different thing. The ethnographic thing is better but the historical images one can with time and effort track down where they've come from and create that metadata. I don't think it's going to be lost and perhaps not where it was scanned and that kind of thing. But yes that's why I think it'd be great to have this project of an online you know yoga image archive or something. Okay now other people. Yeah you've already asked my metadata question but the second part of my question is about data sharing so you say you have everything in Google Drive and your team and do people work with these other data and how do you know what is what and especially all this precious information that you have and that you haven't recorded anywhere. Well we have. Yeah we do all use it. We can all access I mean all the each so yet there's a folder for every text that we're working on and then all its manuscripts in subfolders and there'll be scans within those so we can all access them quite happily. Daniela's photographs she's the ethnographer they're all available to us and we have files of you know rare books whatever that's it I mean yeah I mean that's it's all I mean I was quite what was the someone mentioned something yesterday I made an overview that looks quite useful because at the moment as I said we've we've got enough work to keep everyone busy individually so we're not sort of at the same time we're not working on the same text. We did try what was that programme Sub-Ether Edit and that was a way of of collaborating you know working on text files at the same time so if everyone's online then everyone can edit the same document but we had lots of problems with that it often didn't work and after all we just gave up and now we're back to the old you know you work on it and then tell me when you're finished and send me an email and I'll work on it um but if this I might have an overleaf and see if that works um I suppose two two questions are one of them is I can understand how it's very I don't wish to be sort of press you on this point in a way that suggests I'm doing something wrong but I can understand why it's very difficult to go back and ask a whole bunch of Indian institutions anything um but there seems to be a due diligence element it doesn't seem like there's a lot of effort involved in saying would you be okay with us uploading this right for public use at the moment where you're in there yes and are making the sense that's true um that kind of due diligence or I'm going to do things with the thing you've given the access to as a result of you maybe I have a due diligence to actually tell you what I'm going to do and make sure you're okay with it well normally you have to often you have to sign something don't you saying that you will give them any publication that you've used it in whether that also says you work reproducer imagine all the things you might do is not necessarily permission um you know I wonder if you have a due diligence to say look this is what we plan to do with it are there any of these things that you might have an issue with right um so I just wonder about that particular yeah kind of I mean yeah we but now you mentioned I'm sort of thinking you could also just sort of after you've got the data then email and ask permission and say because they never respond to emails you can say well I am yes um you can say if you don't respond to this I'll take that yes but yes you're right we should we could just make that part I mean maybe I should say it to Jason look from now on at the point of receipt because you don't want to jeopardise it until you've actually got hold of the things as well they might go oh hang on you know if you ask beforehand and normally they'll have you know normally it's they make you wait for days and you tell them you've got to fly at home and you know that evening and you'll get it at six o'clock just as you've got to get in your taxes in case of grabbing it and running um but yeah I will suggest that to Jason that's a good idea and I just um I was just walking at you I wanted to mention it's there's obviously a lot of variation between libraries and in particular the big chain libraries are well known for being extremely hospitable and helpful and you know they'll put you up for free and feed you and and give you scans for free and I don't know what they I expect their policy they expect they would be fine about uploading the data online as well please yeah I I I wonder we um you and I have talked and it's on your website the connection between um the actual asanas and descriptions and texts and I wonder um it seems to me like that would be obviously given what you said about under the bond and things not something for you to do but it would be wonderful to have um a description in the text which somehow links to a visualization of a particular right you're reading now you put your left leg behind your head and absolutely your pinky I don't know and then there's a picture either historical picture or contemporary picture or both which says look this is this awesome yeah I know we've done that in fact Mark's much more involved than I was in a film we just made a film of the latest the sort of most recent of the text we're editing which has 110 postures is it 112 and we've had you know models in to do those those those poses that's all been filmed they I think some of them have proved impossible even for England's bendiest yogis so we may have to go to Indian school children is looking up in its next next point of call yeah part of the problem is that you really don't know often what's being described the description can be quite quite terse or like streaks and so to put a picture next to it might be a little bit misleading yes we just can't figure out what's going on yeah Mandela I think I mean this is just such an amazing project I mean the content and stuff you're bringing together but I think that one of the most important lesson also for people for funders but also for people that apply is that the amount of work it takes to make this digitally available it's totally underestimated FN right Frederica is just finishing a huge project the crossroads project and because she had it I'm just saying that she had worked in this realm before she she noted knew exactly how to manage her five phd students and postdocs and well yeah but I think and this is something when we see grant so I read a lot of grant applications because they have double heads hats heads is that the amount of work it takes to constantly input the metadata and to manage the materials and systematically file name and to sort them and to order them is so much work that in principle every project should have someone that does this work if you're working on the scale that you are working on right where it's not one person and we know from their data languages documentation project the phd students goes in train qualitatively they start they collect a shitload of data and at day three they forget what they were recording and what they were talking about because they think they can keep it in their minds right and they can't and then they come up to the end of their their three years phd thing they have to submit the documentary corpus to us and they have to finish your dissertation write some articles get a job but I think it's really key to understand that we always think the digital is easy no it's not it's so much work yeah we underestimate this and in the end you know the researchers go into well we can't manage this so we're not going to do this and then my question comes what happens if you get hit by a bus when you walk out the street now with all this material on your google drive google has it yeah great yeah with no metadata there yeah or not will summon it we have to um we have to move on although I will say that when you were talking about how difficult something was that it was faster to do the old fashioned way when I started on my project with Matus he said writing anemlogical dictionary old fashioned way will be much much faster than doing it this way yeah exactly so we will so I saw other benefits in doing it the fancy computer way in terms of methodological explicitness um there also might be things about like whether you're not immediately hit by a bus but I do think that you're you're right to ask kind of what are these computers giving me and if someone tells you it's a new time they're lying uh okay


Okay. So the next feature I would like to talk about is legends and stack charts. So we have been able to show legends in normal column and bar charts, but in 2.4 you can also apply that to stack charts. So I'm going to start from scratch here and I'm going to change the visualization type to stack column, and I'm going to go and select a couple of indicators and click update, and the colors we see here are just the static normal default colors from the color set. So to give this chart a bit more meaning you can go and apply a legend. And to do that you go to options, you now find the legend tab available, and the legend UI is exactly the same so you can decide to go with the predefined legend assigned by the system admin to the indicators, or you can freely choose from a list of legends. So I'm going to apply the ANC coverage to the entire visualization and you can see that you now have legends in stack charts as well. This also applies to stack bar charts. Okay, so I said we have been improving the legend support in 2.4, and that also goes for single values. So as you can see you can apply legends to single values. And we also support icons now. So if there is an icon configured for the indicator in the maintenance app by your admin, you can easily turn them on in data visualizer by going to the options.


Thanks very much Yep, I think I'm on so thanks for the invitation to come and come and talk about about plank and and the cosmology that we've been able to learn from it From its now from its full mission of data. Actually, it's satellite that flew for a few years And our isn't it not on Interesting it definitely looks like it's supposed to be on It's on super Let's try that better Good, okay So I want to show you some of our results our Main data that we're extracting cosmology from the main statistics We're using and what we see is kind of this of the key cosmological results So this is this is drawing on the work of a huge number of people and a huge number of groups a large collaboration of people And some of their logos are pictured here. This is definitely not single-person work. This is this is large large collaboration work Okay, so what I want to show you first is what is our main? What is our main data that we use to talk about things like primordial fluctuations testing inflation testing the contents of the universe and our main data to begin with really our Maps of the microwave background sky and I'm going to show you more or less three of them because it's three that we're currently using for cosmology This is a this is a this is a map that you've perhaps seen more Frequently than the other ones. I'll show you which is the Image of the temperature anisotropy in the microwave background so the temperature of the of the of light at 400,000 years of recombination when the universe transitions to being neutral We're capturing the fluctuations in that light that more or less trace the density fluctuations in space at that time at 400,000 years, and we've now mapped it out. This is an all-sky map unwrapped onto the screen and we've now sort of over the last 20 years we've kind of zoomed in on this on these features with higher and higher fidelity now at High resolution and high sensitivity measured from from plank and these temperature fluctuations the scale here is tends to hundreds of micro Calvin these are fluctuations about the mean temperature Small linear fluctuations that allow us to capture the physics of what's happening after 400,000 years and trace It back from inflation perhaps or whatever mechanism was that put in the initial fluctuations through to the time we capture them So this is the one that you've probably seen more we're now to do our cosmology. We've got new images of the sky And then the second one is the polarization anisotropy of the microwave background So what I'm showing you here. They're not as pretty pictures. There should be prettier pictures coming coming soonish from plank We can measure the temperature of the microwave background We can also measure the polarization of the light you can measure and so what we actually the physical thing We measure our q and u stokes vectors So polarization with this orientation in q and this orientation with u and we can map that over the sky as well as the temperature And that's shown here top and bottom for the q stokes vector and the u stokes vector And we're starting to see and I we're seeing these anisotropies that skirt that that gray the gray plot has got lumps and bumps in it And these anisotropies are tracing the physics of what's going on at recombination as An independent probe the temperature, but it's the same physics what we're what we're seeing The temperature of the C and B traces roughly the density fluctuations in the universe at 400,000 years And the polarization roughly traces the velocity So we have this tightly coupled photon barrier on fluid that evolves after primordial fluctuations are put in And we capture what that what that fluid is doing At 400,000 years both in both in density. It's density in its motion of the of over densities I'm just showing you a zoom in of a little patch of the sky about a hundred square degrees a small region sort of this big Measured from the ground-based telescope called at pole That complements plank by being able to zoom in on in a bit more detail on the polarization And here you can sort of see the fluctuations These are anisotropies in the polarization of these two q and u stokes vectors and It's not coincidence that your eyes will see a shape pattern like this in the top one and this in the bottom one that's the signature of Emote type pattern of polarization, which is the kind of it's a it's the pure if you take a polarization map in Of the sky and you look at it's the divergence part of the map and the curl part The divergence part is the thing that we think traces the motion of the fluid the photon barren fluid and that's what we're seeing in in In the signal here The other part that we could see is a b-mode a curl type polarization That that we haven't yet seen but I'll come back to that Okay, so so we have we get to trace these are We have temperature the cmb we have polarization of the cmb and now we also have this new one Which you'll see increasingly over the next decade Which is the anisotropy in the lensing potential of the cmb? so the micro background comes to us and gets gravitationally distorted by Cosmic structure that lies in between us and when the cmb set off Typically a photon will get deflected by a couple of arc minutes very small amounts of angle on the sky and So we can think of it as you know that the temperature of the cmb we see in some direction of the lens cmb is The unlanded cmb from some original direction Plus the gradient of some deflection field so a distortion a distortion angle It's given by the gradient of some lensing potential And That lensing potential the thing that bends the light is an integral of all the matter lying between us and last scattering And that's useful because being able to probe the integral of everything that's lying between us and last scattering Gives us a handle on things like the geometry of the universe It tells us more about the dark energy about what what that could be and also tells us about the mass of neutrino particles This is kind of an exciting new thing to be able to see and so in the same way as the Cmb temperature anisotropy where you see blue spots The slightly less Lensing in that direction and red spots is like a hot spot. It's more lensing And so you should think of it where you see red The integral of the matter between here and where the cmb set off is higher than over there There's more matter in that direction than over there And this this kind of where we are right now with these lensing maps is Sort of you could think of it maybe like how Kobe was for the cmb temperature As in these these fluctuations you're seeing you're seeing them on large scales They're still a bit noisy But this this lensing map over the next decade should take the next steps should should really kind of Improve in the same way that we've seen that the temperature of the cmb improve But we're already learning things from it One one question I always get asked and then forget to explain so let me just say this now is It's how enough do you figure out what lends the cmb when you just get to measure light that's been lensed a Cartoon of what's what happens to this light is below This is a little snapshot of part of the cmb sky Before and after being distorted by intervening structure that's bending the light around it And it's a very small effect, but something that you can see slightly as though a coherent shifts in the background features Because the light is basically being bent around giant cosmic structures and what we do we actually use the fact that Different Fourier modes of the background signal are not coupled if there's no lensing But bending round a large object couples different Fourier modes together And so we construct an estimator of what did the lensing by looking at pairs of That's of the background temperature at some scale and some different scale length scale And we couple those together and estimate the lensing signal from that I'm not gonna say too much more here because it's maybe It's too You know you don't need to don't need that right now, but it's We appreciate it's not a trivial thing to do and one of the things that we work on a lot right now within plank We then have the collaborations is to is to get this better But this is important because this signal is the signal where you know, we hope when I come back It's in a decade We hope to say we have detected the mass of neutrinos from this and it will come from an improved measurement of this this map So now we'll come back to that Okay, so we have these that's I would say that's kind of our core data are these are these sort of Samples these maps of the temperature polarization and lensing of the of the CMB We then look at their statistics and the statistics we look at are Pretty much the two-point function of those maps because for Gaussian fluctuations, which they do seem to be That captures all of the information in those maps Although we do look for non-Gaussian features, too And so here is the the latest Power spectrum angular power spectrum from plank from this 2015 Data so up here is the is the variance in the map or the power spectrum of the map as a function of angular scale and these are You know tens tens of degrees or more Degree scale here and then sub-degree scale running along here to smaller scales And this is the the angular multiple moment of a spherical harmonic decomposition And so we're in this, you know, we plank is sort of Beautifully measured with very small errors this this the power spectrum now from large scales through to small scales here right down to these these a few arc minute scales and Shows incredible consistency with that red theoretical model That is our model. That's that's the lambda CDM cosmology So we do find a model that fits and it fits very well And you know, this is a flat universe with this handful of parameters that I'll discuss in the next the next slide Where we're seeing we think we're seeing, you know, just simple primordial fluctuations evolved through To recombination in a rather simple universe filled with neutrinos, baryons, photons, cold-up matter and a cosmological constant And the fit is really good I mean so so here down here shows the residuals of this lambda CDM model the red one compared to the data And the error bars are so small that you kind of have to see it on this residual plot and So anything that isn't this kind of simple lambda CDM model would show up as deviations of these data points around that red line Now one thing that your eye, you know goes to straight away is here This sort of dips this lack of power at the largest scales has been seen for a while is still there is a curiosity It's kind of a it's kind of deviant at like two to three sigma, but it's but not not a higher significance It's interesting At smaller scales there are some points that the deviate from the line, but not significantly And actually something that's happened in the last couple of years with improved plank analysis is that the kind of the residuals of this data With respect to the model have just really squeezed in So there's incredibly little wiggle room of anything that's not this model Compared to the data and let me just say just a couple a bit more specifics about what this model is Because what we do is we throw in six numbers Six variables and a handful of assumptions of assumptions about the universe when we're when we're predicting the theories that match the match to the data We assume a flat universe I'll come back to that We've seen flat universe and we can constrain three numbers that describe its contents and the expansion rate of space And we quantify them by a baryon density a cold-up matter density and a peak angle at which we see the CnB acoustic peaks and that maps on to What the contents of the universe are so for example if I tweak around the amount of dark energy the dark matter the cold up matter the Baryons that would change the peak angle. I see the CnB at We have three numbers that describe those And we have two numbers that describe their primordial fluctuations We think they're just Gaussian They're adiabatic So all the different fluids in the universe trace each other at early times they had they follow the same over densities And they are described by a power law With an amplitude and a spectral index and that spectral index differs from one It's not that's one of the big results That's that's consistent that's held up with the with the sort of improved analysis of Planck It's still there right the spectral index is significantly different from one Of that that describes that the fluctuations and those are the kind of probably the five parameters of main interest to this audience We also have an the CnB gets scat when the stars light up the universe the CnB light gets scattered and damped the signal And so the epoch when realization occurred affects our signal And is of great interest to many astrophysicists But perhaps of less interest to this audience That's one of our numbers And we have a bunch of assumptions. We assume the universe is flat We assume that the dark energy is just a cosmological constant. We assume there are three Species of neutrinos. We assume the primordial helium fraction is set by Big Bang Nucleosynthesis that it's 25% of the universe We assume that the total mass of the neutrinos in the universe is is 0.06 eV Which is the minimum mass scale that we get from? Neutrino oscillation experiments We assume there are no tents of fluctuations no cosmic strings and manic fields nothing right all those things are not are not in this this model and this is the model that really fits and And You know we looked for a lot of things that differ from it, and they're just not there And that's really held up even more by looking at these extra maps of the sky the polarization the lensing So here what I'm showing you is The this is now the power spectrum of the emode pattern that sits in the polarization maps If I take my maps of the CnB polarization, and I look for the pure divergence pattern in them And then I compute the two-point function of that Then that's shown here the the power spectrum of that emode signal as a function of Multi-pole again angular scale a large to small scales Here in blue are the data points from Planck and in red this this red curve is not fit to these data points That red curve is just lambda CDM The lambda CDM model that fits the temperature data plotted on the polarization data So the fact that this wasn't even fit to the data, you know says that this model is doing something right It provides a pretty good fit One of the residual worries of then Planck that's being worked on right now Is that if you zoom in and you look at sort of the the difference of the data with respect to the red Lambda CDM model there are there are some more Deviating points than you see in the temperature and We do think there are some residual systematic uncertainties left in the polarization data that kind of the one sigma or so level Probably from some of the temperature signal leaking into the polarization And that's why the main cosmology results are not don't use this polarization yet We sort of looked at it, but really the main results still come from temperature And that's something that you should you should see change in the next year But it's not you know, we're talking about small shifts. We're not talking about something significant We also see the correlation between the temperature and the polarization Down here again red curve not fit to the data It's just the prediction of lambda CDM of the cross correlation between the fluctuations at the temperature and the polarization of the signal Third then the third piece the third piece of that of the data is then the Two-point function the angular correlation the angular power spectrum of that lensing signal the lensing potential This then again shows the power spectrum the two-point function of the lensing signal as a function of multipole Again, these are degree scales in the sky Here the data from plank And again the black curve is just lambda CDM fit from the temperature data. It's not fit to this data And it provides and it fits very well You know, there's kind of this dip here, but it's it's not it's not really significant and this is useful because What this allows us to do so what yeah what this What this measurement allows us to do is do things like as coming back to neutrino mass But also at a more simple level measure the geometry of the universe that the amount The lensing essentially proposes the amount of clustering of cosmic structure at later times in the universe It typically picks up the size of cosmic structures kind of halfway through the universe's history Dominantly it's an integral but that integral peaks kind of halfway through the universe's history So we're picking up most of the signal kind of a kind of seven or eight billion years But it's but it's a broad kernel. It picks up signal from from earlier and from later And if we had a universe that kind of fit the background CMB data But was more geometrically was closed and had less dark energy than the under CDM It would actually produce more lensing because you'd have more clustering in the universe So if you have more clustering happening you boost the lensing signal and you would push that that whole curve up and that's given us these Strong constraints on the curvature of the universe So So here I'm showing you here the the fraction of the universe energy of density in dark energy or cosmological constant here Versus matter density here where the dash curve is a flat universe and anything off that flat curve is a In this direction is a closed universe And it used to be with a CMB you could go all the way down that geometry down to zero dark energy And now you can't because the lensing tell it gives us a lot of new information the lensing prohibits, you know I've asked the closed universe and so Let's just concentrate on that on that blue Contour these are the 95% confidence limits for those two Contents of the universe and you see it's tightly Closed in around the flat the flat line and if I then Expressed it in a in omega k the the curvature of the universe Then just with the CMB I get a 2% is a 95% limits that the maximum deviation from Flatness is 2% just from the CMB Now if I then add in the positions If I look at then galaxies at later times that I look at where the galaxies are This is from the Sloan Digital Sky Survey Galaxies are typically separated by preferentially separated by a particular distance and that's seen here from the Sloan data They're typically separated at this this kind of 120 megaparsecs Where a megaparsec is a typical separation of a galaxy of pairs of galaxies There's this peak separation in that and that and that peak separation Gives us a handle on the expansion rate of the universe at later times And if we throw in that as well, then you get down to a 0.5% constraint on the curvature of the universe. That's that red curve here So really there's any any wiggle room from flatness is is is you know is vanishing If I look at now at the primordial fluctuations This shows our current constraints from both Planck and data including new data from a South Pole Telescopes the bicep to you and Keck array Down here is this is this power is this power the spectral index of fluctuations that I mentioned before where a value of one is scale invariant fluctuations and n less than one is Has less power at smaller scales and is what we would naturally expect from you know many simple models of inflation And this is as I said This is one of the main one of the main results from Planck is that if I just look at that red 95% contour I'll come back to this number in a minute It excludes one at high significance And it zooms in on kind of point nine six point nine seven that that range But now obviously the thing that the thing that's that's certainly of interest is do we see any gravitational waves? So if inflation happens, we would expect to see a background of tensor fluctuate We said expect tensor fluctuations that would source a background of gravitational waves And the strength of those the size that signal will depend on the energy scale of inflation And it's something that obviously we all would like to know If we can see it and what it is because that can that would tell us a huge amount about Both whether inflation happened and it's and its characteristics And so here is this we characterize it by a tensor to scalar ratio that the how big the tensor fluctuations are compared to the scalars and In a given slow roll inflationary model You know every every model will have a have a predicted space point on this NSR plane So here for example would be a Slow roll implant on potential with a Phi squared shape here will be a Phi shape And so here so with just with the plant data We limit this space in the NSR plane to here Where you can just about get this fiasco potential, but a five to the four term is it's gone off that space It's no longer doesn't no longer works and Those just come from meant looking at the temperature anisotropy But what we're really all looking for is is this this specific prediction that gravitational waves will put in a Polarization signal that has a curl part that might look that has this kind of pattern in the polarization and We have not seen that yet a primordial b-mode signal And that's you know We all heard last year that we thought we might have seen this from the bicep to experiment in the South Pole who did see a B-mode signal and would have put if the if the signal was just pure gravitational waves Would have put us up there somewhere a point that's actually inconsistent with blank But there's actually no evidence that it's gravitational waves and everything's pointing to the signal that was seen Just being a mission from our own Milky Way galaxy So that right now By including information from the Planck satellite that tells us more about the signal from the galaxy We've managed to sort of clean up the data from bicep to Clean it up and put actually a new limit on the tensor scalar ratio And that's what's shown here in green down here and That's kind of interesting and then if you and then the blue contour is if you add in the lensing data and external data But it's they're rather similar, but a bit squeezed in this direction but either of these two curves so so bring Bring this five-square potential into kind of then disfavored at more than the 95 percent level I mean they're not then it's not five sigma, but it's um, but it's certainly not preferred by the data and What many of us are doing to move beyond Planck are to try and make it a taxion Kind of in this in this kind of level if the signal is there to be seen or at least push down the limits You know down to here or below Because many you know that's obviously of great interest for constraining inflationary models But the current limit is RF less than point oh nine right now there's no evidence that anything is is That we have any fluctuations that don't just obey this power law Gaussian adiabatic description Okay, and that those constraints have really tightened with all the plant data We can look at the fraction of primordial fluctuations that could be non adiabatic So where the fluids at early times don't follow each other at early times as you might expect if they were imprinted by Inflaton fluctuations decaying to form all the fluids in the universe We can characterize that by some parameter alpha that shows the deviation away from adiabaticity and You know that is restricted to be you know less than a Percent or so on even less so with temperature and even less if we include the polarization data which is It's still Early days for that and there's no evidence for non gas entity the constraints on this FNL parameter That described the deviation of a particular kind of deviation from non gas entity Where zero says their Gaussian is now tightly constrained to be Two and a half or different different types of it for different shapes of non gas entity two and a half plus or minus six and All these other two numbers here that show also a consistent with zero so no evidence of that from the CMB and No evidence that the primordial fluctuations deviate from a power law So any any kind of scale dependence of the spectral index is constrained at the kind of 1% level I can't I can't vary more than that and there's no significant kind of features in the spectrum that could say you have some significant Oscillation or some significant boost at some scale that could be indicative of some more unusual model. We're just not seeing it We've learned a lot about neutrinos With plank and with ground-based experiments. We're able to measure the effective number of species Which for us in cosmology could be neutrinos sorry the effective number of relativistic species that could be neutrinos It could mean other things it could be It could be axions it could be anything that produces a relativistic background We would count as being this these relativistic species and So what we do is we assume it's all neutrinos and we constrain the number of them Okay, so that's it and we allow that to be a continuously variable number. We don't just assume it to be integer values And so I'm showing you here the constraints Well, let me just that we just give you the numbers that we have which is the number of neutrinos species or the effective number of species It's now pretty tightly constrained at three point one plus or minus point three or point two at a one sigma level Depending whether or not we include this is plank data, and this includes galaxy position data And this is this is this is really taken a big and this comes from the fact that if you increase neutrinos You basically sort of imagine you're switching radiation from From photons that are coupled to barion's to neutrinos that are not coupled to barion's The sound waves at the early times propagate differently in those two fluids And so neutrinos additionally damp the power spectrum and slightly shift it could the peak positions So getting a measure of the damping tail from plank And then increasingly with polarization you can squeeze you can really limit how much non photon Radiation you have in the universe and this number used you used to be able to have like ten in the CNB Just like five years ago ten was fine, right? So this the fact that it's you know, even four now looks pretty Disfavored so this this shows that number as a function of barion density And this little if I look at any of these combinations of data for is just just does is really on on the edge Now again, you could have some different Different relativistic Species that could contribute a fraction of an N It could be point two point one ten to the minus five and that's still in there But this is that we are squeezing down on the possibilities there And in the next few years that should Be halved or better that uncertainty from from measuring the CNB even better And we can also look at The primordial helium fraction and that looks that's also now much better constrained with like if I look at neutrino mass There are many effects of neutrinos But just the one I want you to sort of have Carry dominantly at the moment because it's the one where we I hope to make best progress is if you switch coal dark matter If you take some of it and make it to be turn it into neutrinos instead Then the universe that has more massive neutrinos has more suppression of clustering of cosmic structure Because those neutrinos even if they're massive they started off relativistic in the early universe They basically behave like radiation because the universe was so hot so a massive neutrino behave like radiation And then like and then like cold up matter later And the fact that it had this epoch of behaving like radiation it free streamed out and it Doesn't cluster like cold up matter. And so you get less clumping of stuff in the universe and less lensing So you tune up the neutrino mass and you push down the lensing power spectrum And there are other threats too, but this is the the main one to think about and that's given us this measurement of This constraint on the neutrino mass The sum of the neutrino masses that's less than point. This is too many decimal places. I'm sorry I did not choose these number of decimal places point six eight right is a All point seven I take carry point seven right that it should be less than point seven EV at 95 percent confidence and if you add in the Galaxy information, then it's less than point two three or point two EV And this is kind of interesting because this is getting into the regime of you know We're getting we think that there should be a signal at point. Oh six EV or greater We have to be careful because we're doing cosmology and this is all indirect measurements. We're not seeing neutrinos We're just measuring their effects cosmologically So we have to be really careful about whether it could be mimicked by other things that we don't understand yet like dark energy And there are some degeneracies with those but they're not really strong And so this is gonna this is this is where in the next ten years. We're you know, we're hoping cosmologically to actually detect neutrino mass Again with with these caveats of being an indirect detection But I think that's we're in we're in an exciting regime Let me just let me just raise a couple of problems or clues and then I'll then I'll stop I'm saying, you know, I giving maybe the a slightly We see nothing in the plank data and another CNB data that says that we need anything It's not just this simple lambda CDM model. It's kind of a bit freakishly good fit That if I if I were to raise any Problems or clues of where we might see something new something some new physics right now if we look at how Galaxies are lensed around large-scale structure called cosmic shear The current measurements of the size of clustering When this this number kind of quantifies size of clustering Okay, this this green contour doesn't quite overlap with this black one and this black one is the plank one and this green one is kind of the one from Lensing of galaxies. They don't quite overlap I think it's more likely that the gap that the measurements of the lens in galaxies is still in early days and might have systematic uncertainties So I don't say that this is I don't think that this is a huge problem, but it's potentially interesting The the peaks of the CNB are a little bit too smeared out if we introduce this strange parameter that I call a Lensing AL and a lensing should be one if the peaks are all completely as I expect and Actually, if I this is a bit too busy a plot But this blue curve here is the preference from the plank temperature data and it prefers a slightly higher value And so it's that the peaks are slightly more smeared out than I'd expect in just lambda CDM But it's not a physical parameter This is not a physical model but you know if one has a physical model that actually does predict a bit more peak smearing then Then there's some room in the data for that and it's large scales The fact this is dip and power at the largest scales is very interesting and I think we have to look in the polarization data and Just keep it in mind that it's there even though maybe it's not hugely significant Okay, so right now the data from plank the CNB data They demand lambda CDM a bit more and more confidence and so It's got a look like little lambda CDM, even if it's not and in particular if it's not inflation It's got a look a lot like inflation If that was the thing that put in the primordial fluctuations And we're busy searching for gravitational waves And I think the neutrino sector is an area that that holds a lot of promise for the next decade in cosmology And I hope we have a lot of interesting further things to say with the next generation of experiments Thank you great overview A quick question Would you like to comment something about the neutrino mass hierarchy? Yeah, I would yeah, so here so so really we're Realistically for a long time now to come we can only measure the total mass So we just sensitive we're slightly sensitive to the to the hierarchy But mainly we sensitive to total mass and so if it but if the higher if it's inverted Then it will be at least point one two EV will be the total mass sum and we'll get there sooner. Yeah So we could detect an inverted hierarchy I think in five years cosmologically with with the caveats, right? So that that will be interesting and you also mentioned degeneracies with other What is the most dominant source? It's a great question So right now me and my PhD student is actually working on a paper to really push, you know explore kind of as many as possible the If you just want to use the cleanest probes so CMB lensing and the Barry and the galaxy positions then they're most degenerate with with curvature and With the dark energy equation of state So if you allow the dark energy equation of states to vary with kind of a two parameter model doubly not w a then then it then it could it could as much as double the error on the neutrino mass and And And those are those the main ones and but there were kind of then there's this then other data should help break this Generacies again, but those are the two main ones because it's like basically Neutrinos suppress clustering But you can change the expansion rate to look a bit like that that's that's that's why those those are degenerates But they're not completely the same When you say that the quadratic model is disfavored that refers only to single-term potentials, that's right. Yeah, sure. Sure, definitely Yeah, okay You're talking about the time frame. You said that in the next decade, we will know the message and neutrino to another money to Using which experiment? Oh, yeah, it's a good question. So so There's two prongs one is improving the CNB lensing and so for CNB lensing we've got what we call Or an DOE speak stage three CNB experiments These are experiments from the ground that will map half the sky from the ground And that's the advanced act telescope in Chile And the South Pole telescope third generation experiment So both of the ones that have already been doing small-scale CNB They are putting on more detectors and covering more sky and that will get us kind of part the way Then the CNB stage four that is plans, but not fully funded yet Which is the natural extension of all these ground-based experiments, which we're saying we're not going to get a new satellite anytime soon what we can do is use or I say that there are there are Strong proposals for large for smaller satellites to measure the larger scales But to map out the whole sky to get neutrino mass you want to get as much the sky as possible at higher sensitivity And so from a mixture of these ground-based telescopes in Chile the South Pole potentially even Greenland will do that at the same time the measurements of galaxy positions will improve with the Daisy Galaxy clustering survey that's starting in a couple of years that moves on from the stone-digital sky survey So it will be the combination of I think the thing that we can actually make a detection from will be what we call CNB stage four plus The Daisy galaxy clustering survey so, yeah Okay, I'm afraid we have to move on and you can talk to speak it later. Yeah


I'd like to start by looking at how to plan your presentation. And here, I'd like to mention three points, your purpose, your audience, and the setting for the presentation. Before I begin, I should point out that when people advise students about planning presentations, they usually include suggestions about how to select and narrow down a topic. Now, while this is, of course, important, for the purpose of this presentation today, I'm going to assume that this has already been decided either by you or your tutor. So I'll assume that you have chosen the topic, carried out the research, and now you are ready to begin the process of planning a presentation. OK, the first thing that you have to consider in the planning process is the purpose of your presentation. There are two ways of looking at the purpose. The first is the general purpose of the presentation. In other words, do you want to inform, entertain, persuade, and so on? I guess the general purpose of our presentation is to inform or enlighten. As well as thinking about the general purpose of your presentation, you need to think about the specific purpose. And by this, I mean, what you want to accomplish, what you want to achieve, essentially, this involves asking why? Why am I giving these presentations?


The last two things are when you're cleaning it up, instead of throwing it out with liquid on the bottom, mix anything that's remained, like let them sit on top of each other for a while, and mix it up and let that harden and throw it out that way. If I wanted to clean this spreader, just like any resin, I can use solvents to clean this, so an alcohol or like white vinegar works. Don't use a solvent if you get it on your hands, it breaks down and can be absorbed into your hands. So wear gloves, and if it gets on your hands, use soap and water to wash it off. It's a pain, but it will come off eventually, and that's the safest way. So we want to see where you're using your resin for. Upload your images onto the art gallery at arresin.com, or just go there to get inspired by others as well. For answers to all your questions about our resining, just visit the FAQ at arresin.com, and you can buy stuff there too. So we're always making new videos. If you like, you can subscribe, and we'll see you next time.