 A couple things to say, we have some evaluation form, I want you to give us some feedback on this course, so I'll get it back tomorrow, so yeah, anyway, so I'll distribute it after You're going to have four speakers in this hour, we're just going to describe some of the resources around, available for you to use, so I'm going to talk first, and Dr. Delzana, and Evgeny, and Yu-Yi will show you what's around, okay, and also I'm going to put the run file in a zipped file, the one that I used yesterday in one of the shared folder, I'll tell you later, okay, so first I'd like to show you something that we have at IAEA, we have a lot of stuff at IAEA, we organize meetings, workshops, like this one, and also we host databases and online codes, many things, so this is our home page, you can go to www minus mdiss.aii, yeah, which one should I go, yeah anyway, so this is our main page, and there are a lot of different things, because we do a lot of different things, so our unit was founded in 1976, more than 40 years ago, so main goal of our unit is to provide data, atomic data, molecular data, plasma surface interaction data, any kind of data that is really important for fusion mainly, and also other plasma applications, so we do a lot of meetings as I said, so on the right side there are meeting announcements, so the second one here is the meeting that we are having, nope, it's 2014, so let me show you, this is the one, okay, so this is the meeting page for this particular school, so you go there, there are several things, but also you will find schedules, so I'm going to put the slides and presentations in this web page, and also I'm going to put the abstract here also, it's not there yet, but anyway that's what we're going to do, our web page has a lot of stuff, and we have like databases you can see on top, we have also online computing, the other thing that you might want to consider is actually a lot of activities, if you go to the meeting page, we have meetings every year like eight to nine meetings, and for each meeting, there is a presentation, so let's say if you go to, oops, not this one, let's go to this one, maybe, yeah, then you know there are meeting agenda, and then it also contains the presentation, and we cover a lot of really large areas of fields, so you can find a lot of information there, and the other thing that you may check out is knowledge base, this is wiki style, supposedly it has a lot more information than it does now, but anyway we hope that we can add more stuff, but anyway this was one of the sort of a wiki pages that people who are interested in atomic data, molecular data, plasma surface interface data can come and read stuff, anyway, so let me let me go back to my presentation now, so we have databases, one of the databases numerical database of Aladdin, our unit doesn't collect any data, well we want to collect recommended data, so Aladdin started as a database of recommended data, but unfortunately over the years that sort of idea faded away, so now it's just a collection of data now, but still there are a lot of data were evaluated and recommended, especially the ones from 1980s and so on, so we don't we have some data like 20,000 atomic and molecular data, so this is not a place to get data for your CR modeling, if you want to do collision-radial modeling, you you'd better go to use FAC or RATIP, the codes to generate the data for CR modeling, but this is the data usually people use it for like kinetic codes or radiation hydrodynamic code and they need a few cross sections and that's where they go to find a good data, anyway it has many different data, different types of data, we have heavy particle collisions like charge exchange and so on, and also electron collisions and photon collisions, we also have plasma surface interaction data, reflections, sputtering and penetration and so on, so this is an interface, so Yuri's gonna use this later in this talk, in this hour, so you can see that you know for the heavy particle there are process categories and so on, we have as I said we have plasma surface interaction data, so you see the processes and you find projectile and surface and the chemical compounds of surface, we have bibliographical database which means it's just a literature information, we get spectroscopic data from NIST, NIST also has the bibliographical database for, I mean Yuri's gonna talk about it, but the data we have is the ones only for fusion relevant elements, we used to get traditional data, the bibliographical data from Oak Ridge Lab, but Oak Ridge Lab data center closed about six years ago, so we are sort of trying to get data from this data center and that data center, but after 2010 we are struggling to get bibliographical data, but before 2010 we have pretty much comprehensive bibliographical data sets for spectroscopic and collisional and also plasma surface interaction data, so the way it works is you put the reactant here or there or surface and then you can click you know categories like heavy particle or surface interaction and so on, then it'll come up with the references, references that you have, reference that have the data sets, I'll just show you quickly for example, of course people might think that why don't you go to just Google Scala to find you know like paper that has cross sections, but it doesn't work very well, if you go and say okay I want to get tungsten dielectronic recombination cross section, you go type tungsten dielectronic cross section, you get like millions of millions of data or results, so it's really not good, but if you say you know tungsten here and electron collision and search, then it's going to show you 85 references, if you click on the reactant data it shows the ionization you know in which elements and chart states and so on, so if you're looking for a specific cross section that was published, this database is really really useful. Okay so that was M. Buddha's our bibliographical database, as I said you know the knowledge base was supposed to be the the central place for atomic physicists, plasma physicists, molecule physicists, they can all come to this wiki page and learn from each other, it was supposed to be that way, but well not so yet, but we're working on it, so there we aim to give information about what kind of data is needed for different types of plasma applications, where you can find data, you know data sources, you know online databases, data centers, you know there are many data centers, not many, but there are data centers, national data centers around the world, they maintain their databases and also there are code centers, you know people who make codes and their kind of information was supposed to be in these wiki pages. We have a like database search engine called Gini, so what it does is it goes out to several databases and find information like radiative transition probabilities or electron cross sections, so for example if I want to get transition probabilities of carbon four, we have lengths of one, two, let's make it like 10 to 100, and then if I click this then it's going to go to all this nine, is it nine, yeah nine databases it'll collect all the information from them, it's thinking, it's connecting, it's waiting, okay so now you see that there are results, there's no results from there, okay, okay there is text W3 which is in Russia, they have all these things, all these lines listed and also the one from ChemDB which is in China, they also have some results, so this is one way that you can get data, okay that was Gini and also we maintain online codes and also data that was generated by code, so there are several places like there's electron impact excitation cross sections for any ion and configuration or there is a heavy particle collision code for excitation ionization charge exchange for bare nucleus on hydrogen target and also this is effective ionization recombination rate code generated by Los Alamos code and also we hosted the data that was generated by Los Alamos people using their code on silicon, chlorine and argon and also we have some flight check collision radio code results so you can use flight check online at NIST but if you want to just get chart state distribution or radio loss rate you can just go to this page and also there is electron impact excitation ionization cross section calculated by the atom akm code in Russia, levidive I think and also we have we have generated effect results it's about 30 gigabytes from helium to silicon like silicon atoms, so let's say if you go to the flight check web page at NIST at IAEA you can click on one of these sort of periodic table and then it shows for example if you click on tungsten you get every chart state radio loss rate and also you can get chart state distribution and also ray collisions you can just download it and use it for your work the fact code we generated about it from helium to silicon ions and also we are working on a thing called fly fact project so it uses c-fect data you know that FD made so it's based on SQL format and the Fortran 90 code 95 will calculate the chart state distribution and level population of the c-fect data it's almost there it's been there for a while but and it just I just need to debug it and then put it on the on the web page so it's something to be coming in the future there are other data for example there's a frame counter factors for hydrogen molecules these these numbers are very important for tokamak plasmas and so on so yeah and also we distribute codes so so you can download graph2k from our our web page or from NIST you only need to just click on on the agree I mean people people have a hard time somehow downloading I'll just show you how to do it so you go to graph2k and then you know you go to license agreement you accept then you can download any of those let me just show you what los almos codes data and so this was generated by people in los almos if you go to argon then you can download argon atomic data but if you look at the the configurations these are the configurations that are included in this atomic data so yeah you can use it and for fact data oh yeah for fact actually the source codes are available from github but you can also look at this input guidelines this is what mingu wrote for us so this gives you some tips how to write your input file for fact codes fact data because yeah there are little things that you want to know to make the code work better yeah and then also there are atomic sort of um let me see I can show you some of the input is there any good maybe yeah so this is the um the fact input file in python interface and you can use this also to generate your fact data you know you you set up atoms and then you set up your configuration sets um you have to optimize it structure to get levels level energies and then well there are many other steps yeah this was written by mingu so it's something to check out and you can also get the radiation transition probability and you get um t r is there yeah the the radiation trans um transition radiation okay um let me see I'm trying to find the critical excitation are we still at the transition probability I think we are okay um maybe not okay so here's ci ah yeah yeah yeah yeah right oh yeah r r is the rated recombination oh yeah here it says it's doing ci and r r I guess I missed it somewhere anyway check it out so there are some input file and also there are input file for uta if you want to do the configuration average model um using fact there is a python input file also for z-band split levels for those who are working on tokamaks they want to look at the z-band splitting so you can use this um input file or some some people want to do polarization spectroscopy and here's an input file for polarization and one can actually do the cr model calculations using fact code also so you can use those and um as I said we we um generate all the data already for you so you can just download it and use it for yours okay so we do that um let me see I think that's it oh that was my last slide okay so um again you know IAE has a lot of interesting activities going on and so we had a similar workshop two years ago so this is our school but like two years ago in 2015 we also had a school and workshop and then we had a we have the presentation and lecture notes from that time so you can check it out there also like professor kun that was there also last time yeah so we're gonna have similar lecture notes um presentation available through this web page so check it out okay now we're gonna move on to uh dr delvena and Yuri is going to introduce okay yeah okay so thank you very much for to the organizers so giving you this opportunity I mean whenever there is a workshop in Italy I try to I try to chip in because I'm Italian of course I love to come back to Italy and I've lived for 20 years in England I'm missing good coffee and and good food that I'm sure you have enjoyed during these days so yes this is me in case you've been wondering you know who was this strange person you know going around without without the thing um I thought you might be interested some of you especially in doing some astrophysical work in some resources that some of you might find useful that's my email address this presentation I'll send by email to the organizers so they can be put together with the other ones so you don't have to take notes I have different hearts but the main heart that I have today is about Chianti database which was mainly developed to um to study spectra we started by a group of people about 20 years ago to we were interested in studying solar spectra in this from the extreme ultra valid you see an example here or in the x-rays where plasma are optically thin you have an image of the solar corona which is very typical on the left but optically thin collisionally ionized plasmas are also you know very common in all nebulae supernova remnants intra cluster inter cluster of galaxies and so these plasmas are very very easy to study so as I said this is a group of people that developed the Chianti database I'm one of the members that's the main web address Chianti database maybe if I have a minute I will show you later we provide atomic data but also programs in terms of atomic data they're actually included what we put in we try to find the best atomic data for ions but our atomic data are also included in many other databases the main one that I'm sure the Yuri will talk about later is VAMDC this is a this is a network of about 30 databases worldwide that we put together with some European funding so that's in terms of atomic and molecular databases I think VAMDC is the most comprehensive set of the most comprehensive resource that you can you can think of we do assess the data we publish a referee paper about it and we have details about what we what we think are the best why we think that the various atomic data are the best so the nice thing about astrophysical plasmas that you can forget about all those complications that the previous speakers told talk to you about about radiative transfer of that and opticality in plasma extremely easy the intensity is proportional to the population of the upper level all you need is the traditional probabilities the a values and what we do is in terms of level populations we solve the level populations within an ion taking into account all the population in the populating processes and then separately we we we take into account the charge state distribution at the moment what we do is something very simple we calculated in anization equilibrium using low densities values these are the source of data that we have we have various files or in ASCII one is the energies we have observed and theoretical energies for the ions we have the radiative data and also we have maximum average the ion electron collision strengths and we have the same from protons we also have all the rates to calculate the charge state distribution so we have direct electron impact ionization the electron recombination radiative recombination we have the cross sections and the rates and we provide the programs of people can actually use these rates and and and do and whatever they want to do we improve the NIST wavelengths I mean we start normally from NIST but in some for some of the important ions we actually try to improve the NIST wavelengths and we change the format so we actually publish now the in the latest release which was published recently one year ago we actually published the actual rates as published not some feats as we were used to do before we also have a possibility to include photo excitation in the level population and also non-maxed ion electron distributions but as I said the main limitation is the the fact that we we assume that the plasma is anization equilibrium at the moment so most people what they do they use these programs that we wrote in in IDL for example this is one case you define you take you take an ion in this case oxygen oxygen 5 for plus you define a density range a specific temperature electron temperatures for which you want to calculate the emissivities you calculate the emissivities of all the spectral lines within the ion and then you can take the ratio them and from the simple ratio within lines of the same ion you see that some of these transitions depend from the density in a different way from these ratios then you you can measure directly the electron density in the same thing you can do it with temperature and the other thing which Chianti has been very very popular with a lot of people is that we also provide a simple way to calculate a spectrum in any wavelengths including the continuum and I also developed some python user interfaces which are basically the same kind of thing it will be soon very soon available we have a google group so if you're interested you can sign up to this google group this is the similar in the sense that you can see the emissivity of the spectral lines on again from oxygen 5 as a function of density and or as a function of temperature now very quickly I'm going to put another hat because I'm also a member of a team of atomic physicists they are here is called the APAP UK network and we've been providing basic rates and cross sections for the fusion community through for example ADAS some of you have probably heard about the ADAS atomic database and and also we provide this data to to the Chianti atomic database and for most actually databases around the world the recent in the last few years we worked on all these sequences and my main contribution has been to calculate cross sections for electronic citation so these very difficult coronal iron ions in a sequence of of papers and I'll just show you an example of what it means basically you did these are very large scales including principal quantum numbers up to four and five and they were necessary because I was particularly interested in the soft x-rays this is a this is a spectrum in the soft x-rays and in green you see the atomic data that we had in Chianti before until a few years ago 2012 and we were actually missing most of these lines because these are transitions formed by iron ions from the principal quantum number and equals to four with the new distorted wave data that we work out we calculated it flexible atomic code but even we replaced them with our math is scattering data then we have a much better and complete set of atomic data about this and this large-scale calculation also improved a lot measurements of densities for example this is a plot of the densities obtained from ratios of different lines in the stream of travel at from solemn some solar spectra in version 7 we measure the density of about 10 to the 10 to the 9 or something like that but just changing the atomic data and this was actually a surprise we didn't expect this we actually find using the same observations if I'm much lower densities bringing into agreement basically the observations this is just just an example so that's it a few if you if I have another couple of minutes yes yeah I can show you quickly this is just the web page of our Chianti database and you can find the data the programs you can find the the references and and the details the papers but for me this is what I developed you have you have also of course the user guides for me a very useful thing is to have the direct access to the data files so I'm going to be biased I'm going to choose an ion that I've been working on iron 10 for example iron 9 plus so you see if you you have the links to the actual files these ascii files that I told you about so you can actually directly get the energies and the relative data everything you want and you also had the references to the actual papers and some comments about what is in the database so you have the first file is the energy the second one is the radiative data we have the electron collisional data and the proton collisional data we also have tables of line emissivities and things like that this is the VAMDC portal but I think that Yuri will probably mention it so this is a this is a portal where you can access atomic and molecular data from 30 databases around the world some of the links some of the searches don't work properly but most of them should work this is the the web page of this UK app of network where we've been calculating things corner balance was here during earlier on during the week so he probably taught to you about about these sort of calculations that we've been running with these are matric codes in terms of electron ions scattering if you go there are various links to where you can find the data you can find the codes and for example in terms of atomic data these are matric codes are all in these directories organized by organized by us electronic sequences and finally this is the open edas which I mentioned where also these the data that we calculate they go to and the open edas is quite nice because he has all sorts of all sorts of atomic data you can see all these classes of of data where you can find relative data rates for excitation you also have effective effective rates calculated for unitization and and recombination taking into account density effects all sorts of things so this is another useful resource thank you any quick questions good but anyway as I said I'll I'll send the PDF file so you can all the links to these resources okay so we'll continue from the point left at my lecture I want to show you in a few more details the interface for plasma interactive okay so that's the well you don't see it but it will be published or you can find it easily in the google just write the plasma formulary interactive and you'll find that link Afon's okay okay here you have in the home page of this utility there is a user guide you can download which means just you take get a zip file you unpack and then run index or whatever html it's a javascript utility there is a reference paper with a link and well license in the group of the clients so let's do some interesting more or less realistic calculations let's take 10 to the 14 I am going to to to enter plasma conditions say for tokamak diverter okay I don't know for easy okay so it will be deeterium same temperature same density radiator again talking about deeterium I don't put here a percentage of the radiator because all plasma is homogeneous in this case uh okay and say uh some high uh bilmer line okay and let's put also typical five tesla magnetic field let's see what can we get with very fast calculations or estimates so the most important at least for me as a line shape guy is anything that goes into the energy uh you can get transition energy and natural line widths which is very small of course for hydrogen or deeterium fine structure estimate by the way you have here a kind of documentation which loads Wikipedia directly for time being I will uh and select this option because I don't want it to interfere with this short stock well Doppler and let's switch to centimeters minus one you can use also atomic units and different energies which is not so convenient for for for line broadening but for other stuff in the energy folder it is okay so okay so Doppler estimate of the Zeeman splitting stark and you can get separately contributions if you are ever interested due to the electrons due to ions and uh radiators in which in our case radiators are neutral so there is no uh contribution of course uh you can compare different things if you are if you want to for example let's compare uh Doppler I don't add to favorites uh Zeeman and total stark now you can go to compare and see these uh entities that you selected in a table and you can also sort according to the value and see that the most important for that line for that conditions would be stark which is uh two times larger than Zeeman but they're comparable and also comparable to the Doppler and next thing you likely to to explore is to to see how these values would change if you vary one of the parameters that's very density and I'm going to change it two times in each direction and you see them so as density goes up the of course the Zeeman and the Doppler uh effects remain the same but stark goes up another uh we we we were talking about uh continuum lowering so another entity of interest is minimal energy distance with the distance to the next neighboring level well we can also add it and go back here and you see it's of course orders of magnitude larger which means this line that we were selected a Balmer 8 to 2 will be very far from the continuum lowering but let's see which line we actually can see for this condition the last one let's try to increase it maybe 11 and see okay it's still far from the continuum lowering 12 13 still okay so probably 15 will be the last one yes okay so already for density of 1.5 10 to the 14 particles per cubic centimeter the uh stark broadening will become comparable to the distance to the next level which means that's the last uh line you will see okay and you're welcome to explore all other options here all other entities there is a lot of them uh there are dimensionless like coupling parameters beta for again that's for Takamak people also from atomic uh uh date from atomic physics stuff like oscillator strengths you can get that value for the for the select transition I forgot to mention everything is calculated assuming hydrogenic approximation which you you you must check one uh possibility to check by the way is to go to uh again to the energy and see the fine structure if fine structure is much smaller than the stark broadening that you know you are in the safe region when you can safely use this utility if fine structure becomes larger is larger than the stark then do not use it okay well uh a lot of entities like the in lens it's the by lens and gyro radios again you can add this for comparisons go back here to compare and now you see these entities of the dimension of lens and you can switch back to energy you see them back and uh the cleanse and here also you can plot as a function of density but you can also see how it behaves if you vary magnetic field okay let's uh you can say that about uh two tesla there would be some interest in effect when the by and the by lens and gyro radios becomes comparable well etc you are welcome to explore this utility quite a few resources on the web related to um to atomic physics and and plasma spectroscopy certainly within the next 10 to 15 minutes I will not be able to cover all them at all so um let me let me let me start with simple statement that you already heard a few times if you want to build a collision related model normally it requires a lot of atomic data now you cannot find all the data that is required for a good model in atomic databases uh they're simply it's it's really let's say of course if you if you have kianti kianti is already collision related model with the data with the the same as well as for flagship but if you want to build something uh of of yours almost impossible you have to run cause yourself however what you can find online is the uh data to compare results of some of your calculations again so let's start with the simple thing for instance we want to uh calculate ionization cross section from uh single nice neon and for this I'll be using the uh los alamos interface that you saw we were running for atomic structure okay so I'm going to the same page okay now not one atomic structure can be calculated here but also excitation ionization so here we proceed with cross section calculation um okay so let's speak ionization let's speak configuration mode which means we're not talking about fun structure levels but just about configuration to make everything simple okay now we have to choose the ion and let's take neon one plus single ionized and we go to configuration selection by default the interface offers us two configurations which obviously are the ground configuration for both ions of course neutral neon is 2p6 so single analysis 2p5 double analysis 2p4 and this is exactly what we need in principle it's possible to add more configurations here but let's just restrict ourselves to what we have here all right next step uh the program has calculated the structure parameters and the calculated ionization energy for this configuration to a square 2p5 is approximately 42 electron volts well the good point here is to compare it with the recommended data and if we go to the NIST database a unexpected database with access to ionization energies you'll find that the actually measured value is approximately 41 eb so the difference only one out of 42 which is certainly good and therefore let's continue with calculation now on the next page you can choose different methods and different parameters for your actual calculation so let's say we will have energy units for cross section calculation and threshold units which is reasonably good will put maximum number of 20 energy points to calculate cross section let's say that's probably now there are three methods here to choose from one is the distorted wave method which should work pretty well for for ions then there are two somewhat simplified methods scale hydrogenic and binary encounter method by the way on the entry page there are manuals on all components of the of the of this package so you can read them and check what each of these mean but basically let's pick all three of these and run the code okay so it's running and here's the result scaled hydrogenic binary encounter and distorted wave ionization now okay we have three methods three cross sections how we're doing now to answer this question we can use one of the collision databases that are available and probably this is the best because it's the most comprehensive this is the database developed at the national institute for fusion sciences in in uh japan the address is db sheen or dbs h i n o dot nibs dot ac dot jp it's also not one database but several databases including for instance all parts from the ia alady and differential cross sections from our molecules ion abundance tables for different types of calculation but at this point let's just try to find where ionization cross sections are so we enter the database and it offers us quite a number of actual numerical databases certainly we picking up the ionization and here we we will be looking for a singly ionized neon so the element will be neon initial ionization state will be one let's just go ahead with with this choice and we're looking for cross sections okay here what it finds 13 records for single ionization one electron comes two electrons go out two records for double ionizations one electron comes three electrons go out so of course we pick single ionization because this is what we calculated these two options give uh bibliographic information but we actually want numerical data so we select this option ask to display and this is the result of what it found in in in the database all these papers we want graphical display to look at at the data now the automatic modes for to scale x and y axis may not be very convenient a priority so let's pick linear for y logarithmic for x and let's see what we got here okay it's a little bit small but nonetheless you can see that there's a lot of data now the legend here has letters e or t at the end and of course it means experiment of theory so and of course you can see that there are uncertainties given here for experimental data these green open circles this is some theory going up but let's say that we accept that at the peak of cross section which is approximately at 200 electron volts the cross section here is slightly over 3 10 to the minus 17 here's the scale okay how are we doing for our las almas calculation uh the scaled hydrogenic ionization has peak at 1.9 electron volts and you remember actually we have it at 200 oh excuse me this is x value let's let's quickly recalculate so we will we will ask for the output in electron volts yeah that that would be too little so it would be about 80 100 okay now the the units are correct so energy in the peak is reached at approximately 93 electron volts actual peak experimental is at 200 so it's way off the value the actual value of cross section 5.6 10 to the minus 17 slightly above them 3.2 or whatever it might be so not not too good now binary encounter reaches the peak value of 8.2 10 to the minus 17 which is way above the measured value at slightly higher energy which is 110 ev approximately but the distorted wave ionization results reaches the peak at 170 200 between 170 200 ev with a value of slightly below 4 10 to the minus 17 and remember this was the simplest calculation we just took two configurations in random so it seems that the distorted wave ionization result is probably the best now let's find out what we have at IEA and for this we go to the IEA MDs data Aladdin database which can be reached again through all this stuff that he showed you we are talking about electron collisions we're talking about ionization we're picking up reactant one which is neon we start with neon plus one and then we try to find all available data for this science so there are four sets of data let's speak second and third we go to numerical data here's the tables of data and here the plots okay now one set of results goes practically to where we to what we calculated was Los Alamos here the other one goes way below now the difference is that this ionization is of the 2p electron but this red one actually is from the 2p electron and I didn't point it out but that explains the difference in cross-section now why we agree so well with this black curve well that cross-section was also calculated with Los Alamos code which is which means that Los Alamos code works generally pretty well now let me then say just a few words about kind of data that we have at NIST in addition to the atomic spectro database there is a big program on production of physical reference data and you can find not only atomic spectroscopy data but molecular spectroscopy physical constant the periodic table here is practically the same as this one that please don't forget to pick it up except that online we already have new names for the four elements here from 113 to 118 now for atomic spectroscopy data in addition to atomic specter database we also have few others but I would like to emphasize as strongly as possible the importance of bibliographic databases the data that come to the atomic specter database first are evaluated by scientists and unfortunately we don't have as many people working on this as we would like therefore although data can be produced calculated it takes long on time actually to reach atomic specter database and this is what Julia was talking about today they take data from NIST but this data may be really old simply because we don't have enough resources to update it however the data that propagates to the bibliographical database so better say bibliographic references to the data is updated almost daily so for instance if we go to the atomic energy levels and spectra bibliographic databases and we display the search form as you see it was last updated two days ago so we actually have semi-automatic system that downloads papers analyzes and then scientists spent not not too much time basically confirming what this automatic system found and what what it has so if we are talking about for instance something like singly ionized neon you see it finds 231 references and some of them are from 2015-14 and this is kind of data that hopefully does reach atomic specter database but not immediately and finally Julia also mentioned that you mentioned the virtual atomic and molecular data center this is kind of organization that now it's a consortium that tries to develop methods to retrieve data simultaneously from various databases quite powerful and a lot will be developed in the future okay let me stop at this point and we will continue we'll start at 225 at the at the computer room