 Okay everyone, how are you doing today? Welcome to our 45th webinar of the Latin American webinars on physics Today, we are very pleased to have Viviana Gamaldi Viviana is currently at the Escuela Internacionales Superiori di Studi avanzati or CISA. She's currently a postdoc Viviana got her PhD degree from la Universidad Complutense de Madrid and and she is Really amazing guest today because she's won a Award at Premio Extraternario Doctorado from the University of Madrid and Today she's going to tell us about dwarf irregular galaxies dark matter and gamma rays The title of her talk is prospects for dark matter detection in dwarf irregular galaxies with gamma rays and without further Me anything else to say I want to introduce you have Viviana. Thanks for joining us And I'm gonna just give you the space to you want to say hi and then just You can start giving us and telling us about your your talk today. Thank you so much, Viviana Okay, thank you Alejandro. Thank you also for this invitation to put this a web seminar to give this to give this web seminar so I will start to share my Desperate, okay, so Again, thank you today as you said I will Speak about this new prospect for dark matter detection in dwarf irregular galaxies with the gamma rays This work is a collaboration with the Katerina Karukas and Paolo Salucci, and it was recently submitted to J. Ka so as first I Would like to start with the motivation for this work and as first this work comes from the the request to explore new sources for new sources for Dark matter detection. In fact so far there were a lot of hints for gamma rays, signals that could be explained as a dark matter, but In general, we don't have so far the Conclusive detection of dark matter particle. So in particular dwarf irregular galaxies are Dark matter dominated objects with huge alos, and this is why they are good candidates for dark matter in direct searches and Also, they are rotational and supported objects. So these allow us to Determine with a currency the Density the dark matter density distribution profile in in this object. So This is the outline of the talk so as first I would like to introduce the concept of Universal rotation cure of galaxies then I will do just a brief summary about the way in which we do dark matter research with gamma rays and Then I will focus on the astrophysical factor and the background in in this object in particular I will show as the angular resolution of gamma ray telescope is a very important characteristic in this case and then I will also show the sky map of The distribution of this object in the sky Finally, I will focus on the possibility to make an extended source analysis for this sample of dwarf irregular galaxies and in particularly in particular I will focus on One galaxy or our sample that is the WLM galaxy So in the end, I will just draw the conclusion of this work. So about the concept of University in the rotation for this concept in particular our fears that The velocity you can can you see the pointer, right? I suppose that so the velocity rotation in In okay, thank you The velocity Rotation in these structures Follow the concept of universality is not just a function of the radius But also of the luminosity of the object and of the optical radius So in this paper by per six solution Saluchi and the same they analyze a sample of more of them one thousand galaxies in for a red with a red shift less than one and in this range of magnitude and They found that this velocity rotation When normalized with respect to the optical radius assume very similar Behavior for different galaxy and in particularly that The normalization of this cool was a function of their luminosity So when we struck this concept We can find that the in general the bar matter fraction the aloe Central density of the matter aloe the core radius are all function Inverse function of the limit of the luminosity of the of the galaxy so In this paper in the previous paper by Caruchas and Saluchi, they try to extract this concept of universality to This new kind of galaxy that are the Dwarf irregular galaxy because the previous work was performed for Well, the sun the sun and spiral galaxy. So in this case they have a simple of 56 galaxies in these rings of magnitude and When they plot the velocity cool with respect to the radius they found that these Velocity rotation cure are very different among them However, after a double normalization with respect to the optical radius and with respect to the velocity at the optical radius They found that these rotational cure Became very similar among them So They starting from this simple of 56 galaxy. They construct this synthetic rotation cure That is given by these black points so, um, I don't want to enter in the detail of the construction of this cure in Here so the details can be found in in this publication. So what we Are interested in in in this case is to fit this cure with some Darmachter density profile they perform this fit and We can see here the results of this fit In particular, we have that the solid line are for the buffer profile Then we are some dashed line for the Navarro-Franklin wire profile and this dotted lashing line is For the dc-14 that stay for decincio decincio decincio 14 Okay, so in particular for each profile the red line represents the contribution for the disc from the disc The blue is the contribution from the gas the brown is the yellow and the pink is the total fit So here is visible that the buckle profile is able to fit very well this synthetic cure While the Navarro-Franklin wire pays to do that in in the inner part And also here in the outer part while this Decincio 14 also works fine, but basically this is a Profile with the five free parameters with respect to the bucket profile that just have two free parameters So the bucket profile definitely represents a good description A description is enough in this case to describe this cure So about the way in which we do the Darmatendaris with the gamma rays in As usual we have that the gamma reflux at the detector the differential gamma reflux at the detector is given by a product of By the product of a particle-physic path and this astrophysical path astrophysical path so the particle-physic path is a function of the mass of the Darmatendaris particle of the annihilation cross-section and of these differential gamma reflux that is the Gamma rays that are produced in each Darmatendaris annihilation or decay event So this part can be considered the same In all the astrophysical sources, so in dorsferoid galaxies for example, or the galactic center About the astrophysical factor again as usual it is the integration along the line of size of the Darmatendaris distribution in the source So here we have this square Because we are considering the annihilation event and this is the back-up profile that we use to fit the rotation curious So here I will show A sample of our sample. So there are no called the physics galaxy here. This is more visible This is just to show you that the distances are in general this Than tens of megaparsecs. This is the error on the distances the optical radius the scale radius The central density of the Darmatendaris distribution The mass of the halo Numeria radio the inclination of each structure the mass of the disk and this is the morphological classification for each galaxy so As you can see here The virial radar is sometimes much more bigger than the optical radius, and I will show this fact in in this live in particular we Found that the virial radius is in sometimes 20 times bigger than the optical radius. So when we Transform these dependence as An angular dimension of the sky the of the structure that of course depend on the distance of the galaxy set We found that the the optical dimension these galaxies Is very little while the dimension of the virial halo is a bit The big difference about this true angle is that the optical angles in general Is Cannot be resolved with gamma ray telescopes while the virial dimension can be Considered as an extended source So We calculate the astrophysical factor for All the galaxy of our sample and we plot heat with respect to the angular dimension of the of the halo As a reference, we also plot Three the astrophysical factor for a three dwarf spheroidal galaxy that is the term tracheal seven one and seven two And what we want to show here is as first that While the spheroidal galaxy are in general Analyzed as point-like sources sources because of the angular dimension Uh, again our same polo galaxy Call me sometimes analyze as extended source Second a second, uh, we have that the error bars on the astrophysical factor Here are lower than the Then the error bars in the case of the spheroidal galaxy not in all the case Of course, there is a good estimation of the astrophysical factor But for the same but for example in the case of seven one, there is a huge error bar that sometimes Cover all the range of values of any dwarf irregular galaxy so About the astrophysical background the difference with the Edward spheroidal galaxy is That here we have a star for me region. So we expect a background also in gamma rays In particular, we have that gamma rays could be produced but can be produced by supernova remnants also with nebulas and other kind of A sort of point like sources So the production of gamma rays in the star for me region depends on the star formation range of the region itself There are some studies about Uh, the relation between the gamma reproduction depending on the star for me the star formation rate The most of these studied are performed for well-designed spiral galaxy. However, we can assume this estimation as Like an upper limit for our cases Here for example, there is an A work this we can find some of this estimation in this reference Um, then we expect a sort of diffuse emission of gamma rays from interstellar matter In particular gamma rays can be produced by pion decay bestralum and inverse compound And in this uh reference by martin. We can find an estimation again of the gamma rays produced by these Uh effects And in general we can find that we expect a luminosity of Almost 10 to 56 hertz per second at minus one While in general for example the sensitivity of the oak experiment that is a night altitude water sharing of telescope is expected to be around 10 to minus 12 So in principle all these sources could be detected by any, uh telescope But, uh Okay, this is just in principle because as I saw as I showed before The most of the time the optical region is not resolved by the gamma rays telescope. So, uh They are not detected as gamma ray sources And in this in this case we can suppose to perform A First up in the first approximation a point like, uh analysis Okay, uh, I sorry. I forgot to say that gamma rays couldn't be generated also by active galactic nuclei But this component is not observed in regular galaxy. So we can totally neglect this contribution So, um the The kind of analysis that we, uh proposing these works is In order to Get a better estimation of this background on the general the gamma reflux produced just from the darmatter component The prospect darmatter component, uh, we suggest to mask these star forming region at least in that sources that are In which the optical region can be resolved by the telescope So in this case, uh Masking the source the optical region we can perform a kind of a standard source uh analysis Uh, of course in this case the astrophysical factor, uh, should be Redefined and we should subtract the masked part to the total astrophysical factor So, uh, okay here we have A comparison of the angular dimension of each source with respect to the angular resolution of each instrument So, uh, we have here the simple our, uh, sorry The simple of our galaxies And here their optical or their, um, angular dimension so the Violet points stay for the angular dimension on the optical region of each source the Green point are for the scale dimension related to with the bucket profile and the blue points are, uh The the angular dimension for the full virial Halon Again as comparison we show the dimension of the records at true and cv1 Here the best angular resolution is given by this, um, red dotted line That is the angular resolution expected for the sharing of telescope array cta um Then we have these Blue line That is the angular resolution for the case telescope for the hook telescope and it is also The best case for the angular resolution of Fermilac. The worst case is given by this yellow line because this is because the angular resolution for Fermilac is very independent dependent on the The the energy so we show this band as It's an estimation So here we should notice that in general All these sources again are font like for the most of Telescope and in principle in principle they um They are not resolved by any of these Of these devices. Okay. Some of them can be resolved for example by has hope or for the next cta In general the in their video radio radios they Can be resolved and they can be also Analyzed as a standing source um And not to do here is that maybe This the gamma ray the gamma ray emission from the optical region of this course the of this source is called a contribution to this Isotropic gamma ray background that has been found by Fermilac and Is not totally understood so far So about the sky map Of these sources. I just show here some of these sources for us. This is in The galaxy center. So this is the ic10 galaxy very close to the galaxy plane and this is the wlm galaxy It means very high Here for example the Green line represents the Field of view of the oak telescope. So this means that This line and this line are the border lines. So all this region is visible by oak um Then for example, we have the hess That is this blue line and these other blue lines. So this region is visible by hess And then we consider the yellow line. So all this region has been visible by magic or the cta north Telescope and we suppose that the complementary part should be visible with the cta south So, um These are the characteristics of all these uh telescope that we consider A quick show here the sensitivity for each telescope. So this green line is fermilac This yellow line is cta. The blue line is hess and the violet line is We perform the standard key square square analysis this is The gamma ray Flux that we expect for the armature annihilation of the key events This is the solid angle the omega the effective area the exposition time and this is the background so as a background As i will show you we Consider two different casing one case in this this background is zero And another case in which this background is given by the sensitivity of this Of each device Okay, so because we are interested in the analysis of the extended sources Um, actually there are not so much publication about this kind of analysis um We found in particular this one in which the others compare the Sensitivity for the standard sources. In fact, we have here the source extension and the integrated flux In this range of energy between 10 and 100 gb And the others compare as i said the sensitivity of the fermilac Telescope and the next cta. So in this range of energy We use so these You know sensitivities And we calculate the spectic flux for thermo matter particle of 100 gb and one tv For each one of the sources of the galaxy in our sample Because of the way in which this sensitivity are calculated We need to integrate just on this range of energy So we found that the flux that we found is several order of a magnitude lower than the sensitivity of these instruments in this In this energy range Um Okay, uh, then uh, we choose a Galaxy the best candidate candidate in our sample. This is now. This is a wlm galaxy We choose the galaxy this galaxy because it has the third highest value of the astrophysical factor The sample and in a huge alloy of almost three degrees It is on the sky view of both the haze hawk cta and fermilac telescope because of its high longitude we can assume that The background is zero for this source And then we have that the rotation cure for this source is well reproduced by The bucket profile that we found for the The Feet of the synthetic rotation So again, we perform this kind of Five sigma analysis, but in this case for extended sources This means that the the our our background need to be Defined again and We found that an approximation to get the background for the standard source is this one. So We use this approximation to get these five sigma estimation Okay And this is what we get so We have that the We perform two kind of different analysis as I said, this is the case for The b-channel and we have that for example in the case of zero background and a request of five sigma Signal on zero background for fermilac to we get this green line If we ask for a five sigma detection on the sensitivity of the fermilac of the The sensitivity of the fermilac instrument In the sense of extended source we find this biode line And this is this and we perform the same kind of analysis for all the Telescope so this black line this dotted National the black line is for cta with zero background And the same kind of live in red is for The background for the standard source Then we have this yellow dotted line that is oak with zero background and the blue one is oak with background and Finally The last one is this one Uh, that is has zero background and s with the background. So if you compare These results for example with Some analysis insist that were performed by the fermilac collaboration Uh, we get for example the the upper limit for the induce to d'ostroidal galaxy That are located here Should impeachable be confirmed by the analysis of these double and uh galaxy Of course, there are some differences in the analysis because they ask they get just a 2.5 sigma So we ask for a five sigma that this means that It should request for a two sigma detection should Results in some uh more constraining limits and But also these This point is obtaining for six years of formation while our our estimation is for 10 years Then we also compare This plot with the galactic center ss and these are two different estimation obtaining for the to cannot three galaxy one is from These people and the other one is again from the fermilac Collaboration so the difference here is the muscle is a matter particle if I remember one is for 100 and the other one is for 66 6 gb the matter particle Okay, we also perform the state analysis for all The galaxy in our sample in this case. We just showed the case for fermi and cpa because uh, they are able to cover all the sky map and again, these are the results for zero background and For an extended background for the fermilac experiment and for the next cta again as a comparison we showed the case for The state of analogy obtained by the fermilac collaboration and they obtained these dot and dash the brown land Again, again, there is a request for choosing one request to choose sigma detection versus our five sigma request and so maybe Our results are not really competitive with these results for dorsal and galaxy but We want to underline that this is just a primary estimation and It could be very interesting to Determine the results with the real data so I won't skip to the conclusion of the work So in principle the astrophysical fact of the irregular galaxy is comparable with the selection on the spheroidal galaxy, so this Makes that the booster both irregular galaxy are good candidates for darmat and research searches In particular We have that we could perform two kind of different analysis for these sourcing ones is the Point like analysis and in people in principle we already get some first preliminary results retrieval by the work collaboration and a second we suggests to Mask the star for me region of this galaxy in order to perform the analysis as extended source in particular this analysis This case of analysis or in particular the detection of Some gamma ray signal from an extended source. It could represent a smoking gun for darmatter detection This is because a kind of the detection of this kind Could be could be not associated with astrophysic so The Misunderstanding in the signal should be lower Finally, we also have that this kind of those irregular galaxy the number of these galaxy That have been studying in the rotational theories and crisis. They are now like 500 object so this is very good for future state analysis and So we hope that this could be Um, it's a gesture also for make a new kind of data analysis and for next observation with the both the current and Next generation of gamma ray telescopes. So I think that That's cool. So thank you for your attention and there are any questions Thank you so much Evianna. Very interesting talk. Um, we have some questions from The the youtube interface and then I will I'm going to ask that question first for you and then I will open the question Here for the people that are present here. So I guess the first question That it's it's been asked by Fernando Rossi Torres is in your chi-square analysis Uh, where are how did you take into account the systematic uncertainties? Where are they? Um in the chi-square analysis of the cloud No, I just I'm So in this plot you mean Yeah, I'm guessing that's the plot. Yeah Okay, we just make a kind of Roof analysis. So we just take these sensitivities here And we assume that they are the background in our analysis so, um These sensitivities are in principle already a request for a five sigma detection um With 10 even so We perform this two kind of analysis with zero background and no zero background because Um In order to to have in some sense an upper limit and the low and the lower limit And we expect that the the real case is somewhere between these Uh, these lines so In this in some way these upper lower limit take Taking into account the uncertainties on the Kind of an analysis that we perform Okay, thank you. Yeah, let's see Uh, um All right Okay, so anybody here would like to ask a question. I have a couple but I can't wait for for everyone I have a question All right, Nicolas. Thank you. Yes Thanks again for the super nice talk. I have a I think a um very nice question But I was wondering what's the difference between like an irregular dwarf with respect to a like normal say, spheroidal dwarf Okay, the first difference is um In the dynamics in fact, as I said that these are Rotational supported object while in dwarf with spheroidal galaxy. Uh, we have dispersion velocities or There is not a rotation in the star so This is the reason To take in account this galaxy because these allow us to get an ideal currency in the rotation proof But in the other case the astrophysical factor is Determined with different reasons and a second the second difference is About the astrophysics because The druster of the galaxy in general are assumed to have Zero background While in this case, this is not possible. So we need to apply this kind of mask and I suppose this is these are the main differences and the third big difference is in In their dimension because dwarf spheroidal galaxy are in general assumed to be to have to to be point like Sources while in this case, we have a huge area. So extended sources Okay, see, thanks Thank you so much. Uh, hold on one second. Yeah, I think Fernando you answered Fernando's question Thank you very much. Uh, who else would like to uh, ask another question This is Oscar. I have a question All right, thank you Oscar. How you doing? Oh, brilliant. Thanks. So, uh, thanks Diana for this for this very nice talk I just wanted for you to expand to return one of your Remarks you made the end of the of your talk. So you mentioned that As mocking gone signal so as mocking gone for uh, for dark matter detection will be So the detection of extended gamma rays in one of these rotation is supported dwarfs and so So I was just thinking that So if in the star formation region You are launching Young pool source Then you could in principle also populate the the rotation is supported dwarf and then perhaps major an extended gamma ray signal from one of these Irregular dwarf galaxies. So I just wanted for you to comment on that So, uh, if I want to understand you say that this this pulsar in the star forming region called affect the background in the standard Is it right? What do you mean? Yeah, so so yeah, so and yeah Yeah, I'm just saying that uh, so In the star formation region you you're going to have Young pulsars these young pulsars are going to have a certain kick velocity And then basically they are going to launch it from the nucleus of the dwarf And they perhaps are going to populate the dwarf galaxy and so You can measure an unresolved population of your of young pulsars And then you can get an extended signal from a dwarf galaxy or or or That's that's what I intuitively will say How you can get an extended signal Okay, of course, of course we have to make the strong hypothesis that the gamma ray background is strongly related to the optical region so that there are no I mean if there is a pulsar in the halo It's very difficult to detect. I mean, it's not it's not resolved. It's part as I say maybe of the isotropic Gamma ray background that we can find in the sky so Of course, there is there is this strong hypothesis on the localization of the background and okay, maybe you Another another possibility could be some Pulsar or some kind of astrophysics that can be in the middle between the observer and the galaxy This is another possibility but a we suppose that It could be localized in some way and and must or Subtracted to the analysis um I won't just underline a think about these Smoking gun for a standing sources. Actually, we just or just extended something that was claimed by linden and rupert. I mean to fendom wrong In which they analyze if I don't wrong a substructure in the galaxy and they explain very well while this The determination of gamma dark matter signal in a standing source and could be a smoking gas in in this sense Right. Yeah, I understand that in the context of our doors for the just because they you're supposed to be They are supposed to have very poor So they are supposed to have very old stellar populations And so maybe they are you expect to have very few pulsars, but then in these rotationally So in these regular dark galaxies them, uh, yeah, I just I just think that it's Maybe more likely that you're going to happen result population of young pulsars. And so perhaps that So, yeah, I'm just saying that perhaps that A statement doesn't apply for this case. That's Okay, thanks. Thank you Thank you. Oscar for your question. Can anybody else like to ask another question? Yeah, I have a question. I mean kind of the beginners of all very nice your talk but I guess it's it's related also with the question that Oscar did But it's really how it's Is strong how it change your results if you change the size of the masking I mean because in in the beginning you are saying you're just marking the part that is related with the optical distribution of matter So what happened if you extend a little bit you make a little bit larger the mask in order to be more conservative in your In the analysis You make a little bit smaller Okay, that's also to say that the optical region is not uh, it's uh, like a determination. No, it's uh A parameter that uh taking account not strictly the optical region, but it is a big uh a little larger than that However, uh The astrophysical factor is calculated simply in this way So in principle you can also apply a mask equal to the angular resolution of the instrument for example to a region that is not resolved so So all the the point is just to recalculate this halo this, uh, sorry this astrophysical factor for the halo so in this way and you can get an estimation of of your new astrophysical factor and As a consequence if it is uh, it could be represent a good analysis or not Okay So in principle your curves with this should be a little bit Upper more. I would say I mean if there is nothing special in the Um, yes, I can your excretion curve your constraint should be a little bit higher If if the mask is bigger in some sense because you are reducing more that matter or Yes, this is the point. I want to show you the Stable is not there in In the slide, but this is for example the astrophysical factor for the optical region Yeah, is that from the paper for the virial region? So That is the paper Okay, so I can watch it there so another question that was very I mean because your analysis is kind of As you said in some part of your talk that there are not So many similar analysis done before so do you know if it is If you think about also to apply this metal for the search of in x-ray of X-ray lines or Since all similar a similar study with war for another type of target. I've been done Recently for this 3.5 kV line, maybe Is for example applied to the galaxy center, no there are these So you must for example the Black hole region and you perform some analysis of the ring around the black hole So the kind of analysis can of course this is in gamma rays, of course So this kind of analysis is applied So far in other words for x-rays I Don't have so much experience in x-rays analysis or radio and so on So I really don't know very well how x-ray experiment works I suppose that if you are able to apply a mask you can do that Of course in x-rays you have a bigger A better angle a resolution so You can see the masking would be a little easier. Yeah, I mean I mean because I was surprised by the large amount of Dwarf irregular galaxies that there are there are much more than the standard dwarf galaxies, no Yes, I mean the plot that you're showing now you can see that the number is much much larger than the Yes, this is a new catalogue that Was published From I don't remember the actual. I'm sorry, but you can find it in the in the paper And so there is an increasing they are still working on The catalogue and on the on to the their mind the rotational curve of these galaxies So the number is in crisis. However, maybe if Kate is there and She wants to add something on that. Can you hear me? Yes. Yeah, okay. No, I just wanted to say that yes, that's true that there are much more dwarf regulars than dwarf ferroidals But the problem is that they're farther so the distance to them is Typically larger than the distance to any dwarf ferroidal So maybe the problem also also for dwarf ferroidal is just the limit of the detection. So they're They are less bright. So it's harder to detect them farther So maybe they're they have the same amount as dwarf regulars, but just dwarf regulars start forming. So They're bright galaxies. This might be the reason why they are more So you mean it's just uh, kind of it's easier to detect because of the start forming galaxy Well, I mean the start forming region Yeah, it's just the the bias that of the limit of the of the instrument that is Ah, that's nice. So but but you don't I mean by doing the stacking you should earn something. I mean you can get an improved the sensitivity Yeah, from the j factor you can see that they are not as high for example as dwarf ferroidals, but they're more Let's say better that their mind the error bars in the j factor is smaller Just because of the dynamics they have better dynamics. So you can estimate the dark matter parameters much better Than in dwarf ferroidals this here you gain but then in the distance you lose Because they're farther. So but maybe if you you detect them You know large amount and then you stack then you you can gain something Yeah, if you have 500 objects, I guess you Yeah, so but all day that because Yeah, the Vienna set that is a kind of recent catalog this one Yeah, it was a it's not a recent catalog because they started the the name of the author is Karachansev And the catalog started to be like, uh, I don't remember from 2000 something But they renew it very frequently. So it gets more and more galaxies So you can find I was kind of my Trying to guess more what is the the rate of grow of new of this catalog is exactly at the start Yeah, I think it's it's quite large. I mean the volume that is uh, this catalog is limited is 11 megaparsec So all these 500 galaxies are within 11 megaparsec. And yeah, I think it's uh, it's growing pretty fast Yeah, but these measurements are pretty for example with balls or something like that or because With balls or something like that they are from time to time popping up new And Yeah, I think it's uh, I think it's x-ray And x-ray, I have because they're forming a like yeah, yeah, yeah Ah, okay, that's good. I think you can do both x-ray and optical them Ah, yeah, that's great So, yeah, I don't I have one more question if the host allows me. Yeah. Yeah, roberto. Thank you So if I have we have more complicated questions than I do So The last question for viviana in your analysis you use the bb channel I mean bb bar channel for the animation of that water But did you also consider the case of a monochromatic emission gamma lines? No, I didn't Okay, but it should be improved or not. Oh, I mean, what is your feeling about that? It should be as competitive as the Be your tau with respect with the already Of the bounds of fermio or whatever Or you think that you lose too much with this method This is could be a for example good In the paper we are just we also suggest to perform a kind of state analysis in different point of the halo So maybe if you have a line This could be a good point in that sense. So In the sense that you should enhance the line With the analysis in different point of the halo. So if this line is six, maybe It could be it could give a Good answer Okay I just have a quick question. So so basically before you can do any analysis on This gamma ray lines on this gamma rays. You have to basically choose what sort of Dark matter profile you need to use, correct? Yes, the backup profile Okay, and then how do you how do you choose that and how do you know? I mean Do you have anything to test it against to test that profile and that that? To test that profile against something so that you know that's sort of like the right dark matter profile that Might be there in the first place. Oh, yeah, because you're trying to match those Gravitational curves, right? Yes, is that how you do it? Yes, this is the work by Kate basically and paolo, yes, perfect um, okay I don't think we have anything else right now on the No, yeah, hold on one second robert. Sorry, nicolas. Let me just see if there's something here online Oh, here's let me can I go with one question from the audience outside of here really quickly? Do you mind? Okay, and then we'll go to nicolas and then we'll call it a day Uh, so fernando say is asking the production of gamma rays happens directly From the dark matter annihilation or for example dark matter annihilates into neutrinos And a weak correction produces also gamma rays. So basically the do do that's a weak correction produce gamma rays as well Yes, we we just uh perform the basic analysis of gamma rays that annihilate directly in the channel. So But the channel of tau and so on We didn't perform the case. We didn't analyze the case of dark matter that annihilates in neutrinos and subsequent Emission, but of course it could be done and Uh, I'm not sure about the the results in somewhere in some in some way The results are proportional with the results that are obtained in in in different Analysis, I mean if you perform this different kind of analysis for a door You can find some pro some proportional results I mean The difference here is in the standard analysis and in in the kind of source, but There are no Bigger difference in the kind to perform the the analysis of dark matter in the resources Okay, so it will be a very weak very small correction. You mean? Yeah, okay Uh, and then the last one how is within 11 mega park sex. There are 10 to the fifth dir r so the sort so I don't get this question but Anyway, let me just let me just figure it out really for you the question, but let's go with nicolas and then Yes, so so you work on the with the barcode profile But I had the impression that this profile was intentional or maybe at least not favored by emboli simulation Is that correct? Okay. See this point is this very discussed But in this case for the rotational cure Uh We are pretty sure that These kind of tools are well described this kind of profile that maybe in other cases. This is it is not the better profile But in this case as you can see from from here This okay, so again, I can show you some more information So with the hypothesis of universal universality We get that in some cases we we have Better description description of the rotation tool and some other cases it Doesn't work very well Maybe again it can ask better to this question But the point is that there could be some Um Uncertainty in the inclination for example of the estimation the inclination of the galaxy or in the This parameter see that they use to make the analysis Um the concentration Uh, however, as you can see in the inner part the The rotation q are well described So this is why the bucket profile is a good good description in this case Okay Well, thank you viviana. I think we've asked you a lot of questions. Um, if I have one very short Okay, look at him. Yeah, yeah, because Another one for me now in the case of a decaying dark matter Viviana did you include that case because in principle the the profile when you go to the video radius It would be more much stronger. I don't know because usually they started I mean usually this diffuse signal from dark matter in the case of decaying dark matter is Is stronger with respect to annihilating case when you go to larger distance, I would respect in the center of the of the aloe We didn't analyze the decay Dark matter case See it could be something interesting to do But again, I suppose that the You can see some pro can get some proportionality in the with what you get from the analysis from other sources so Less constraining I suppose But dark matter decay into into what into something lighter than itself More so you know next to next to lightest dark matter candidate or something. No, I understood that Yeah, I mean the standard decaying that much I can in the same, uh, this should be the the same Case but the only difference will be this square here that could be Surprised for the Direct proportionality and the same here in the square order the matter party I'm not sure about the That's how I I didn't calculate the astrophysical factor for the key dark matter. So I don't know exactly, but I could respect Yeah, so now you can have another paper to Thank you Okay, thank you very much everyone for your questions. Thank you Evianna for that great talk You're welcome. Uh, so in two weeks we have our 46 uh episode and in A couple of months, maybe we're gonna have our 50th episode and that's like, uh, I guess a special thing So stay tuned And uh, thank you and I hope to see you all next time Thank you very much, uh for for coming today Bye