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See current, upcoming and recent past observations scientists are making with the Webb Space Telescope. Use the &quot;Observation Details + &quot; button (right side of the window) to view each observation&#x27;s science focus areas, instruments used and more. Note that the sky map showing the target’s ...

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Telescope

telescope

Authors:
(1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland;
(2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction 2 Some open questions 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 3.6 Future gamma-ray telescopes PBHs have a range of potentially interesting direct gamma ray signals associated with Hawking evaporation. These include the 511 keV gamma-ray line, produced by electron-positron pair-annihilation, where positrons originate from black hole evaporation. The INTEGRAL detection of the Large Magellanic Cloud provides one of the strongest bounds attainable with present observations, and should be greatly improved upon by future MeV gamma-ray telescopes such as GECCO [60], as well as AMEGO [61] and ASTROGRAM [62], among others [63]. Exploding PBHs, the late-time limit of Hawking evaporation for small PBHs, provide intriguing candidates for future very high energy gamma ray telescopes that may address transient phenomena, that pertain especially to the new frontier of PBHs of ultralralow masses. Such gamma ray experiments include HAWC (100 GeV -50 TeV) and CTA (20 GeV-300 TeV) [66] at TeV scales, and at PeV-scale photon energies LHAASO [67] and SWGO [68]. Such searches will be closely coordinated with multimessenger projects spanning next generation underground gravitational wave telescopes (EINSTEIN (ET), COSMIC EXPLORER (CE)) and FRB observatories (CHORD) [69]. This paper is available on arxiv under CC BY 4.0 DEED license. Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Authors: Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction Abstract and 1 Introduction 2 Some open questions 2 Some open questions 2.1 What is the abundance of PBHs? 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3 The PBH Roadmap 3.1 High redshift mergers 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 4 Conclusions and References 3.6 Future gamma-ray telescopes PBHs have a range of potentially interesting direct gamma ray signals associated with Hawking evaporation. These include the 511 keV gamma-ray line, produced by electron-positron pair-annihilation, where positrons originate from black hole evaporation. The INTEGRAL detection of the Large Magellanic Cloud provides one of the strongest bounds attainable with present observations, and should be greatly improved upon by future MeV gamma-ray telescopes such as GECCO [60], as well as AMEGO [61] and ASTROGRAM [62], among others [63]. Exploding PBHs, the late-time limit of Hawking evaporation for small PBHs, provide intriguing candidates for future very high energy gamma ray telescopes that may address transient phenomena, that pertain especially to the new frontier of PBHs of ultralralow masses. Such gamma ray experiments include HAWC (100 GeV -50 TeV) and CTA (20 GeV-300 TeV) [66] at TeV scales, and at PeV-scale photon energies LHAASO [67] and SWGO [68]. Such searches will be closely coordinated with multimessenger projects spanning next generation underground gravitational wave telescopes (EINSTEIN (ET), COSMIC EXPLORER (CE)) and FRB observatories (CHORD) [69]. This paper is available on arxiv under CC BY 4.0 DEED license. This paper is available on arxiv under CC BY 4.0 DEED license. available on arxiv

PBH Eccentricity, PBH Spin and Future Gamma-Ray Telescopes

How it Works by Archibald Williams is part of the HackerNoon Books Series. You can jump to any chapter in this book . THE MICROSCOPE, THE TELESCOPE, AND THE MAGIC-LANTERN. here Chapter XIII. THE MICROSCOPE, THE TELESCOPE, AND THE MAGIC-LANTERN. The simple microscope—Use of the simple microscope in the telescope—The terrestrial telescope—The Galilean telescope—The prismatic telescope—The reflecting telescope—The parabolic mirror—The compound microscope—The magic-lantern—The bioscope—The plane mirror. IN Fig. 119 is represented an eye looking at a vase, three inches high, situated at a, a foot away. If we were to place another vase, b, six inches high, at a distance of two feet; or c, nine inches high, at three feet; or d, a foot high, at four feet, the image on the retina would in every case be of the same size as that cast by a. We can therefore lay down the rule that . the apparent size of an object depends on the angle that it subtends at the eye To see a thing more plainly, we go nearer to it; and if it be very small, we hold it close to the eye. There is, however, a limit to the nearness to which it can be brought with advantage. The normal eye is unable to adapt its focus to an object less than about ten inches away, termed the "least distance of distinct vision." THE SIMPLE MICROSCOPE. A magnifying glass comes in useful when we want to examine an object very closely. The glass is a lens of short focus, held at a distance somewhat less than its principal focal length, f ( ), from the object. The rays from the head and tip of the pin which enter the eye are denoted by continuous lines. As they are deflected by the glass the eye gets the that a much longer pin is situated a considerable distance behind the real object in the plane in which the refracted rays would meet if produced backwards (shown by the dotted lines). The effect of the glass, practically, is to remove it (the object) to beyond the least distance of distinct vision, and at the same time to retain undiminished the angle it subtends at the eye, or, what amounts to the same thing, the actual size of the image formed on the retina. It follows, therefore, that if a lens be of such short focus that it allows us to see an object clearly at a distance of two inches—that is, one-fifth of the least distance of distinct vision—we shall get an image on the retina five times larger in diameter than would be possible without the lens. see Fig. 120 impression The two simple diagrams (Figs. 121 and 122) show why the image to be magnified should be nearer to the lens than the principal focus, f. We have already seen (Fig. 109) that rays coming from a point in the principal focal plane emerge as a parallel pencil. These the eye can bring to a focus, because it normally has a curvature for focussing parallel rays. But, owing to the power of "accommodation," it can also focus rays (Fig. 121), the eye lens thickening the necessary amount, and we therefore put our magnifying glass a bit nearer than f to get full advantage of proximity. If we had the object the principal focus, as in Fig. 122, the rays from it would converge, and these could not be gathered to a sharp point by the eye lens, as it cannot more than is required for focussing parallel rays. diverging outside flatten USE OF THE SIMPLE MICROSCOPE IN THE TELESCOPE. Let us now turn to Fig. 123. At a is a distant object, say, a hundred yards away. b is a double convex lens, which has a focal length of twenty inches. We may suppose that it is a lens in a camera. An inverted image of the object is cast by the lens at c. If the eye were placed at c, it would distinguish nothing. But if withdrawn to d, the least distance of distinct vision, behind c, the image is seen clearly. That the image really is at c is proved by letting down the focussing screen, which at once catches it. Now, as the focus of the lens is twice , the image will be twice as large as the object would appear if viewed directly without the lens. We may put this into a very simple formula:— d In Fig. 124 we have interposed between the eye and the object a small magnifying glass of 2½-inch focus, so that the eye can now clearly see the image when one-quarter away from it. b already magnifies the image twice; the eye-piece again magnifies it four times; so that the total magnification is 2 × 4 = 8 times. This result is arrived at quickly by dividing the focus of b (which corresponds to the object-glass of a telescope) by the focus of the eye-piece, thus:— d The ordinary astronomical telescope has a very long focus object-glass at one end of the tube, and a very short focus eye-piece at the other. To see an object clearly one merely has to push in or pull out the eye-piece until its focus exactly corresponds with that of the object-glass. THE TERRESTRIAL TELESCOPE. An astronomical telescope inverts images. This inversion is inconvenient for other purposes. So the terrestrial telescope (such as is commonly used by sailors) has an eye-piece compounded of four convex lenses which erect as well as magnify the image. Fig. 125 shows the simplest form of compound erecting eye-piece. THE GALILEAN TELESCOPE. A third form of telescope is that invented by the great Italian astronomer, Galileo, in 1609. Its principle is shown in Fig. 126. The rays transmitted by the object-glass are caught, coming to a focus, on a concave lens which separates them so that they appear to meet in the paths of convergence denoted by the dotted lines. The image is erect. Opera-glasses are constructed on the Galilean principle. before THE PRISMATIC TELESCOPE. In order to be able to use a long-focus object-glass without a long focussing-tube, a system of glass reflecting prisms is sometimes employed, as in Fig. 127. A ray passing through the object-glass is reflected from one posterior surface of prism a on to the other posterior surface, and by it out through the front on to a second prism arranged at right angles to it, which passes the ray on to the compound eye-piece. The distance between object-glass and eye-piece is thus practically trebled. The best-known prismatic telescopes are the Zeiss field-glasses. THE REFLECTING TELESCOPE. We must not omit reference to the telescope, so largely used by astronomers. The front end of the telescope is open, there being no object-glass. Rays from the object fall on a parabolic mirror situated in the rear end of the tube. This reflects them forwards to a focus. In the Newtonian reflector a plane mirror or prism is situated in the axis of the tube, at the focus, to reflect the rays through an eye-piece projecting through the side of the tube. Herschel's form of reflector has the mirror set at an angle to the axis, so that the rays are reflected direct into an eye-piece pointing through the side of the tube towards the mirror. reflecting THE PARABOLIC MIRROR. This mirror (Fig. 128) is of such a shape that all rays parallel to the axis are reflected to a common point. In the marine searchlight a powerful arc lamp is arranged with the arc at the focus of a parabolic reflector, which sends all reflected light forward in a pencil of parallel rays. The most powerful searchlight in existence gives a light equal to that of 350 million candles. THE COMPOUND MICROSCOPE. We have already observed (Fig. 110) that the nearer an object approaches a lens the further off behind it is the real image formed, until the object has reached the focal distance, when no image at all is cast, as it is an infinite distance behind the lens. We will assume that a certain lens has a focus of six inches. We place a lighted candle four feet in front of it, and find that a diminished image is cast on a ground-glass screen held seven inches behind it. If we now exchange the positions of the candle and the screen, we shall get an enlarged image of the candle. This is a simple demonstration of the law of —namely, that the distance between the lens and an object on one side and that between the lens and the corresponding image on the other bear a definite relation to each other; and an object placed at either focus will cast an image at the other. Whether the image is larger or smaller than the object depends on which focus it occupies. In the case of the object-glass of a telescope the image was at what we may call the focus. sharp conjugate foci short Now, a compound microscope is practically a telescope with the object at the focus, very close to a short-focus lens. A greatly enlarged image is thrown ( ) at the conjugate focus, and this is caught and still further magnified by the eye-piece. We may add that the object-glass, or , of a microscope is usually compounded of several lenses, as is also the eye-piece. long see Fig. 129 objective THE MAGIC-LANTERN. The most essential features of a magic-lantern are:—(1) The ; (2) the for concentrating the light rays on to the slide; (3) the for projecting a magnified image on to a screen. source of light condenser lens Fig. 130 shows these diagrammatically. The is most commonly an oil-lamp, or an acetylene gas jet, or a cylinder of lime heated to intense luminosity by an oxy-hydrogen flame. The natural combustion of hydrogen is attended by a great heat, and when the supply of oxygen is artificially increased the temperature of the flame rises enormously. The nozzle of an oxy-hydrogen jet has an interior pipe connected with the cylinder holding one gas, and an exterior, and somewhat larger, pipe leading from that containing the other, the two being arranged concentrically at the nozzle. By means of valves the proportions of the gases can be regulated to give the best results. illuminant The is set somewhat further from the illuminant than the principal focal length of the lenses, so that the rays falling on them are bent inwards, or to the slide. condenser The , or object lens, stands in front of the slide. Its position is adjustable by means of a rack and a draw-tube. The nearer it is brought to the slide the further away is the conjugate focus ( ), and consequently the image. The exhibitor first sets up his screen and lantern, and then finds the conjugate foci of slide and image by racking the lens in or out. objective see p. 239 If a very short focus objective be used, subjects of microscopic proportions can be projected on the screen enormously magnified. During the siege of Paris in 1870–71 the Parisians established a balloon and pigeon post to carry letters which had been copied in a minute size by photography. These copies could be enclosed in a quill and attached to a pigeon's wing. On receipt, the copies were placed in a special lantern and thrown as large writing on the screen. Micro-photography has since then made great strides, and is now widely used for scientific purposes, one of the most important being the study of the crystalline formations of metals under different conditions. THE BIOSCOPE. "Living pictures" are the most recent improvement in magic-lantern entertainments. The negatives from which the lantern films are printed are made by passing a ribbon of sensitized celluloid through a special form of camera, which feeds the ribbon past the lens in a series of jerks, an exposure being made automatically by a revolving shutter during each rest. The positive film is placed in a lantern, and the intermittent movement is repeated; but now the source of illumination is behind the film, and light passes outwards through the shutter to the screen. In the Urban bioscope the film travels at the rate of fifteen miles an hour, upwards of one hundred exposures being made every second. The impression of continuous movement arises from the fact that the eye cannot get rid of a visual impression in less than one-tenth of a second. So that if a series of impressions follow one another more rapidly than the eye can rid itself of them the impressions will overlap, and give one of , if the position of some of the objects, or parts of the objects, varies slightly in each succeeding picture. motion THE PLANE MIRROR. This chapter may conclude with a glance at the common looking-glass. Why do we see a reflection in it? The answer is given graphically by Fig. 131. Two rays, a , a , from a point a strike the mirror m at the points and . Lines n, o, drawn from these points perpendicular to the mirror are called their . The angles a n, a o are the of rays a , a . The paths which the rays take after reflection must make angles with n and o respectively equal to a n, a o. These are the . If the eye is so situated that the rays enter it as in our illustration, an image of the point a is seen at the point a1, in which the lines d , e meet when produced backwards. b c b c b c normals b c angles of incidence b c b c b c angles of reflection b c When the vertical mirror is replaced by a horizontal reflecting surface, such as a pond (Fig. 132), the same thing happens. The point at which the ray from the reflection of the spire's tip to the eye appears to pass through the surface of the water must be so situated that if a line were drawn perpendicular to it from the surface the angles made by lines drawn from the real spire tip and from the observer's eye to the base of the perpendicular would be equal. About HackerNoon Book Series: We bring you the most important technical, scientific, and insightful public domain books. This book is part of the public domain. Archibald Williams (2009). How it Works. Urbana, Illinois: Project Gutenberg. Retrieved https://www.gutenberg.org/cache/epub/28553/pg28553-images.html This eBook is for the use of anyone anywhere at no cost and with almost no restrictions whatsoever. You may copy it, give it away or re-use it under the terms of the Project Gutenberg License included with this eBook or online at , located at . www.gutenberg.org https://www.gutenberg.org/policy/license.html

THE MICROSCOPE, THE TELESCOPE, AND THE MAGIC-LANTERN.

Nowadays, an essential part of the development process is to track the performance of an application. Analyzing the processes in the system allows you to better understand which part of the project is working well, and where urgent fixes are needed. Among the many tools that allow you to monitor and debug, there is one that is very easy to customize in the Laravel framework, because it is made by the creators of the framework themselves. Its name is Telescope. Laravel Telescope is a debugging panel, with a user-friendly and modern design. Inside the panel you can find logs and statuses of all elements of the system. Features Laravel Telescope is a customized debugging panel with different aspects of the application, where each aspect is highlighted in a separate menu item. Telescope allows you to see all parts of the system, such as database accesses, cache accesses, how to work with built-in events, how to work with custom events. Also there is realized the display of requests to the system or errors. We will talk more about the features a little later, but for now let's set up the application. Local and production installation The main convenience of working with Telescope is that it can be configured literally in a couple of clicks. After installing the package you need to load the assets with the command telescope:install , and then run migrations. When installing only locally we need, after adding the package to dev dependencies and loading the assets, to remove the TelescopeServiceProvider connection from config/app.php, but set the provider connection depending on the environment in AppServiceProvider, for example as follows if ($this->app->environment('local')) {
   $this->app->register(\Laravel\Telescope\TelescopeServiceProvider::class);
   $this->app->register(TelescopeServiceProvider::class);
} After that you need to remove the Telescope package from discover in composer.json.
As for the production solution, there can't be one opinion. On the one hand - when installing and on production environment there is no need to finalize the connection, because in this case it will be available everywhere. It is also a plus, as it gives you the opportunity to quickly see what is happening with the state of production.
However, such a solution has a disadvantage and quite a big one.
Due to the fact that the data that is shown in Telescope is extremely sensitive, it is necessary to correctly configure the routing and disable it from being available without access to the corporate network.
In my opinion, the ideal connection would be to access a local Laravel Telescope that accesses all data sources within the corporate network.
The last step in setting up this tool is to set up the configuration in config/telescope.php Let's see how it works By default Telescope runs at /telescope. With a fresh installation, you probably won't see any requests or other data. But what we can say with certainty is that there is a lot of possibilities for this tool, if you look even just at the list of menus. As for the settings for connecting different services, we will talk about it below. In the meantime, it is still necessary to understand how to set up the panel for yourself. Prune command The first problem in our application is the problem with data deletion. Since Telescope collects all the data it sees, the database often quickly reaches its limit without deleting old records. Because of this, we need to update the database by force. Every application has a different frequency of data refresh, but if we're talking about a small project, we can do it on a daily basis. This can be achieved by running the artisan command telescope:prune, or by setting it automatically in Console\Kernel. Accessing the Telescope panel By default, working with the panel is only allowed locally. To fix this, you need to add some modified logic to the Gate check in TelescopeServiceProvider and specify there, for example, your email address. protected function gate(): void
{
   Gate::define('viewTelescope', function ($user) {
       return in_array($user->email, [
           'example@gmail.com'
       ]);
   });
} As you can see in the listing - adding a rule for validation is not a difficult task. Filters From time to time, when working with Telescope, especially in production, there is a problem with disk space. In order to avoid this and not to disable all logs so often, Laravel Telescope provides filters. They allow us to record only important parts, such as errors or dropped jobs. To change this we need to add or remove necessary/unnecessary parts in TelescopeServiceProvider, for example like this: Telescope::filter(function (IncomingEntry $entry) {
   if ($this->app->environment('local')) {
       return true;
   }


   return $entry->isReportableException() ||
          $entry->isFailedRequest() ||
          $entry->isFailedJob() ||
          $entry->hasMonitoredTag();
}); So the filters helped to limit the set of logs when working on production. Tags If you look at the previous listing, there is a method hasMonitoredTag(). It allows you to show all records that have a tag set, regardless of which watcher it belongs to. In order to set a tag on, for example, a query, you will need to add the following to the TelescopeServiceProvider: Telescope::tag(function (IncomingEntry $entry) {
   return $entry->type === 'request'
       ? ['status:'.$entry->content['response_status']]
       : [];
}); All tracked tags can be viewed by clicking on the button in the top right corner of the admin panel interface. Available watchers Finally, we have observed all the formalities and come to the most interesting part. Laravel Telescope contains a huge number of integrations with different services. Let's take a look at the most popular watchers. Adding a watcher to the system is done in the config/telescope configuration file. If you need to add login data to a new watcher, the new data is written directly to the 'watchers' key. The full list is quite large and while some work with obvious entities like CacheWatcher, CommandWatcher, RequestWatcher, others need a bit more detail. BatchWatcher - this watcher keeps track of sending jobs in batches. Read more about this method here EventWatcher and ModelWatcher - it's worth noting that EventWatcher does not track changes to models that use standard model events, unlike ModelWatcher GateWatcher - records all checks of gates and policies and their results. Below, for information, are examples of how some of the pages work. CacheWatcher Tracks cache hits, including unsuccessful ones. You can also see the passed arguments and options DumpWatcher Shows all calls to dump() function It is worth noting that this watcher does not work when using as a cache driver. array EventWatcher Shows all custom events that have occurred recently. You can also track the listener that worked on a particular event. ExceptionWatcher One of the most useful watchers, as it allows you to see errors, including the code where the error is thrown, as well as stacktrace Upgrade Telescope version It cannot be ignored that upgrading the Telescope version can cause some difficulties. To solve them, you need to follow all the steps of the guide on the official website, and make a couple of points. Due to the fact that the published assets may change during the upgrade, you need to upload them again during the upgrade, either manually or by setting post-update-cmd in composer.json Conclusion There are a huge number of all sorts of options on the market right now for debugging and tracking the state of a project. Laravel Telescope may not be very suitable for Production solutions, but for local development the tool is almost indispensable. It is worth noting that Laravel Telescope is updated quite often, which gives hope for long term support.

Companion for working with Laravel — Telescope

Navigating the Enigmatic Labyrinth of Web3 Gaming: A Trilogy of Riveting Challenges Welcome to the enigmatic labyrinth of Web3 gaming, an exhilarating new realm teeming with uncharted territories, unforeseen challenges, and unexplored potential. Amidst its intoxicating intrigue, we grapple with three colossal challenges that demand our immediate attention: forging sustainable virtual economies, deciphering the enigma of player behavior, and harnessing the power of advanced data analysis tools. So buckle up and let's embark on this riveting odyssey. I. Virtual Economies: The High-Stakes Chess of Balancing Supply and Demand Picture yourself as the sovereign of an enigmatic, pulsating metropolis. Your mission: ensure prosperity flourishes, balance prevails, and citizens revel in their existence. Intimidating, isn't it? Now, transpose this scenario onto an expansive, kinetic gaming universe and you'll fathom the bewitching complexity of governing virtual economies. Just like their tangible counterparts, in-game economies thrive on equilibrium. Too much abundance leads to debilitating hyperinflation, rendering those hard-earned, coveted in-game trophies mere trinkets. On the flip side, extreme scarcity catapults us into a vortex of deflation, where even mundane items demand a king's ransom. The objective: conjure a harmonious sweet spot between these extremes - a precarious endeavor akin to ballet dancing on a razor's edge, but ecstatically exhilarating when mastered. The stakes are high. A striking revelation from a in 2020 disclosed players shelled out a whopping $64.4 billion on in-game purchases, reinforcing the gargantuan significance of virtual economies in games. SuperData Research study II. Decoding Player Behavior: The Da Vinci Code of Gaming Every player is a unique, enigmatic conundrum. Some are intrepid explorers, some tactical maestros, while others thrive on anarchy. Unraveling these multifarious behaviors is akin to deciphering the Da Vinci code - baffling, hair-pulling, yet incredibly gratifying when you crack it. The era when game developers could release games with blithe disregard for player sentiment is a relic of the past. Player behavior analysis now occupies the throne. Reinforcing this reality, an Entertainment Software Association survey revealed a : 64% of adults and 70% of minors in the U.S. are gamers, underlining the necessity to cater to a diverse symphony of player behaviors. riveting statistic III. Game Data Analysis: The Oracle's Vision in Decision-Making Visualize game data analysis as an oracle's crystal ball. It foretells the future (or a close facsimile thereof), furnishes critical insights, and steers decision-making. Within the gaming cosmos, such a tool empowers developers to fine-tune game economies, refine gameplay mechanics, and comprehend why players bid their game adieu. Traditional tools often falter, overwhelmed by the colossal avalanche of data spawned by games or failing to deliver actionable insights. With DFC Intelligence projecting the global video game market to catapult to , potent data analysis transcends being a luxury and morphs into a veritable imperative. $250 billion by 2025 In summary, these imposing challenges, albeit intimidating, represent an exhilarating opportunity to redefine the world of Web3 gaming. Like a captivating puzzle, they infuse this journey with an element of enigma and excitement that only adds to the allure of this dynamic frontier! Stepping into the Spotlight: How Telescope Labs Aims to Game-Change the Web3 Landscape Picture this: you're standing on the edge of an unexplored gaming universe, teeming with exciting quests, hidden treasures, and thrilling challenges. But wait! You're not alone. Right beside you, wielding an arsenal of AI-powered tools, stands a formidable ally - . Telescope Labs : Vested Interest Disclosure This author is an independent contributor publishing via our . Be it through direct compensation, media partnerships, or networking, the author has a vested interest in the company/ies mentioned in this story. HackerNoon has reviewed the report for quality, but the claims herein belong to the author. #DYOR brand-as-author program From its humble beginnings in London, is on a daring mission to solve the riddles we just spoke about. So, hold onto your gaming controllers as we embark on this roller coaster ride! Telescope Labs Battling Virtual Hyperinflation and Deflation with a Secret Weapon Remember how we discussed the wild fluctuations in in-game economies that can send players packing? Well, Telescope Labs has found a magic potion that could stabilize these virtual economies and maintain harmony. Their secret weapon? Groundbreaking Market Intelligence and Data Analytic tools! This dynamic duo brings harmony to chaotic game economies, ensuring neither hyperinflation nor deflation spoils your virtual shopping spree. It's as if they've unlocked the cheat code to a balanced game economy. Deciphering the Enigma of Player Behavior To tackle the Rubik's cube of diverse player behaviors, Telescope Labs has brought in a special guest: artificial intelligence. Leveraging AI, the company has crafted a unique lens that offers a deep understanding of the myriad player behaviors. It's like having a secret playbook that reveals the thoughts, preferences, and playstyles of gamers. Suddenly, the Rubik's cube doesn't seem so daunting, does it? Unleashing the Crystal Ball of Game Data Analysis The crystal ball we fantasized about? It's real! And it goes by the name of Vantage. Telescope Labs' crown jewel, Vantage, is a marvel in the realm of game data analysis and decision-making. This nifty tool is like the Sherlock Holmes of data analysis, adept at deciphering clues and revealing insights that can transform your game universe. It enables gaming companies to unlock the full potential of their game economies. What's even cooler? Vantage speaks human! With its natural language query interface, anyone, even a beginner, can converse with it. Crafting Partnerships that Forge New Frontiers Telescope Labs is not going solo on this epic quest. They've formed alliances with industry titans like Gamevolution, PlayEmber, Widow Games, and Pink Moon Studios. It's as if the Avengers of the gaming world have assembled to revolutionize the Web3 landscape! As the gaming world stands on the brink of a new era, Telescope Labs is poised to steer it towards a future teeming with sustainability, understanding, and innovation. So, gamers and developers alike, buckle up, because with Telescope Labs, we're all in for a gaming revolution that's set to transcend Web 2.0 and 3.0! In the immortal words of ' CEO, Semih Gilan, "We can't wait to embark on this exciting journey together with our partners and clients. By unlocking the power of LLMs, we pioneer evolution on game analytics and empower developers to revolutionize the industry." Telescope Labs And revolutionize, they will! Ready to join this thrilling adventure with Telescope Labs? Game on! Don’t forget to like and share the article!

Web3 Gaming Redefined by Telescope Labs: Master the New Frontier

Juegos Web3 redefinidos por Telescope Labs: domina la nueva frontera

Web3 Gaming redéfini par Telescope Labs : maîtrisez la nouvelle frontière

टेलीस्कोप लैब्स द्वारा वेब3 गेमिंग को पुनर्परिभाषित: मास्टर द न्यू फ्रंटियर

Telescope Labs によって再定義された Web3 ゲーム: 新しいフロンティアをマスターする

Web3 Gaming Redefinido pelo Telescope Labs: Domine a Nova Fronteira

Trò chơi Web3 được Telescope Labs định nghĩa lại: Làm chủ biên giới mới

Telescope Labs 重新定义 Web3 游戏：掌握新领域

Pleasures of the telescope by Garrett Putman Serviss, is part of the HackerNoon Books Series. Read this book online for free on HackerNoon! : Pleasures of the telescope Title : Garrett Putman Serviss Author : May 10, 2009 [eBook #28752] Release date : English Language Table of Links CHAPTER 1 CHAPTER 2 CHAPTER 3 CHAPTER 4 CHAPTER 5 CHAPTER 6 CHAPTER 7 CHAPTER 8 CHAPTER 9 CHAPTER 1 About HackerNoon Book Series: We bring you the most important technical, scientific, and insightful public domain books. This book is part of the public domain. Garrett Putman Serviss (2009). Pleasures of the telescope. Urbana, Illinois: Project Gutenberg. Retrieved October 2022 https://www.gutenberg.org/cache/epub/28752/pg28752-images.html . This eBook is for the use of anyone anywhere at no cost and with almost no restrictions whatsoever. You may copy it, give it away or re-use it under the terms of the Project Gutenberg License included with this eBook or online at www.gutenberg.org , located at .html https://www.gutenberg.org/policy/license

Pleasures of the telescope by Garrett Putman Serviss - Table of Links

is a technology that corrects the distortion in an image caused by natural effects such as air turbulence and change in the local temperature and atmosphere. Adaptive Optics The agile development of professional astronomy, plus the growing awareness regarding the benefits of using lightweight materials in manufacturing, are expected to offer positive momentum to the adaptive optics component market during the forecast period, 2019–2026. Telescope technology is evolving and is close to the next generation of discoveries, which offer an opportunity for the introduction and use of lightweight materials such as carbon fiber-reinforced polymer (CFRP) in the manufacturing of telescopes and optics. Segmental Insights The has been segmented on the basis of type, application, and region. global adaptive optics components market , the adaptive optics components market has been segmented into wavefront sensors, wavefront modulators, control systems, and others. On the basis of type The wavefront sensor segment is projected to register an increase in demand, in part due to the growth of the biomedical sector. This has also contributed to increasing the application of wavefront sensors in ophthalmology in recent years. By application, the adaptive optics components market has been segmented into consumer goods, astronomy, military & defense, biomedical, and others. Recently, the use of adaptive optics has become more popular in astronomy to improve image resolution, which is expected to fuel the growth of the adaptive optics component market in the segment. Regional Analysis Geographically, the global adaptive optics component market has been segmented into North America, Europe, Asia Pacific, and Latin America, Middle East and Africa (LAMEA). North America is expected to witness significant growth, owing to the increasing focus on the development of advanced optics systems and their adoption in the astronomical field for the delivery of sharper images. Adequate support from government agencies in terms of funding for the development of advanced telescopes and astronomical equipment is also pegged to be a key factor favoring the market growth. For instance, in , which would help astronomers study the outer reaches of the known universe. April 2015, the Canadian Federal Government announced funding of approximately USD 234.5 million for the development of a 30-meter telescope Europe is expected to witness considerable growth in the adaptive optics components market during the forecast period, 2019–2026. This can be attributed to the key role of technology in the success of the European Extremely Large Telescope (E-ELT) project. Asia Pacific is anticipated to witness substantial growth in the adaptive optics technology market. It should be noted though that while adaptive optics significantly improve image quality, the high cost of the overall system is a factor that restricts the market growth in the region. The LAMEA region is expected to witness moderate growth, due to the integration of high-end adaptive optics in military vehicles and equipment for the enhancement of surveillance efficiency. Key Players Some of the major players identified in the adaptive optics component market are Northrop Grumman Corporation (U.S.), Iris AO, Inc. (U.S.), HOLOEYE Photonics AG (Germany), A.D.S. International S.r.l. (Italy) and Canon Inc. (Japan). Segmentation By Type Wavefront sensors Wavefront Modulators Control Systems Others By Application Consumer Goods Astronomy Military & Defense Biomedical Others By Region North America Europe Asia Pacific LAMEA Previously published here.

How Will the Adaptive Optics and Telescope Industries Help Each Other Evolve? 

The Next Steps for Primordial Black Hole Research

Authors:
(1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland;
(2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction 2 Some open questions 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 3.3 Plugging the pair instability gap with PBH? An equally powerful mass challenge for PBH arises from the pair instability gap. This is generated by the catastrophic core collapse of massive stars that results from pair-instability SNe, and predicts a deficit of astrophysical BH between ∼ 50 M⊙ and ∼ 120 M⊙. The full LIGO-Virgo O3 data set reveals a definitive decline in merger rates above ∼ 40 M⊙ [55] but with several candidates filling this gap at high credibility [56]. Could PBH populate the pair instability gap? A smoking gun signature would be a feature in the BH mass spectrum, most likely indicative of a new formation mechanism. 3.4 PBH eccentricity Even though PBH binaries are formed with large eccentricity at high redshift, they have enough time to circularize before the GW signal can enter the observation band of current and future detectors. This implies that an observation of a non-zero eccentricity e would rule out the interpretation as a primordial binary formed in the early Universe, while it may still be compatible with a PBH binary formed in the late-time universe [57, 58]. 3.5 PBH spin The PBHs form in the early universe through the standard scenario of the collapse of large overdensities inherit a characteristic mass-spin correlations induced by accretion effects [7]. Using this criterion for determining the possible primordial nature of individual GW events would require reducing uncertainties on the accretion model and studied at the population level [59]. Fig. 3 presents a flowchart from Ref. [47] one might follow to assess the primordial nature of a binary merger based on measurements of the redshift z, eccentricity e, tidal deformability Λ, component masses m, and dimensionless spins χ. This paper is available on arxiv under CC BY 4.0 DEED license. Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Authors: Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction Abstract and 1 Introduction 2 Some open questions 2 Some open questions 2.1 What is the abundance of PBHs? 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3 The PBH Roadmap 3.1 High redshift mergers 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 4 Conclusions and References 3.3 Plugging the pair instability gap with PBH? An equally powerful mass challenge for PBH arises from the pair instability gap. This is generated by the catastrophic core collapse of massive stars that results from pair-instability SNe, and predicts a deficit of astrophysical BH between ∼ 50 M⊙ and ∼ 120 M⊙. The full LIGO-Virgo O3 data set reveals a definitive decline in merger rates above ∼ 40 M⊙ [55] but with several candidates filling this gap at high credibility [56]. Could PBH populate the pair instability gap? A smoking gun signature would be a feature in the BH mass spectrum, most likely indicative of a new formation mechanism. 3.4 PBH eccentricity Even though PBH binaries are formed with large eccentricity at high redshift, they have enough time to circularize before the GW signal can enter the observation band of current and future detectors. This implies that an observation of a non-zero eccentricity e would rule out the interpretation as a primordial binary formed in the early Universe, while it may still be compatible with a PBH binary formed in the late-time universe [57, 58]. 3.5 PBH spin The PBHs form in the early universe through the standard scenario of the collapse of large overdensities inherit a characteristic mass-spin correlations induced by accretion effects [7]. Using this criterion for determining the possible primordial nature of individual GW events would require reducing uncertainties on the accretion model and studied at the population level [59]. Fig. 3 presents a flowchart from Ref. [47] one might follow to assess the primordial nature of a binary merger based on measurements of the redshift z, eccentricity e, tidal deformability Λ, component masses m, and dimensionless spins χ. This paper is available on arxiv under CC BY 4.0 DEED license. This paper is available on arxiv under CC BY 4.0 DEED license. available on arxiv

Cab the Pair Instability Gap Be Plugged With Primordial Black Holes?

Authors:
(1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland;
(2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction 2 Some open questions 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 3.2 Sub-solar PBHs The detection of sub-solar BHs in a compact binary merger is regarded as one of the smoking gun signatures of PBHs. Indeed, BHs of astrophysical origin are not expected. The sub-solar mass range may be however populated by other compact objects like neutron stars, white dwarfs, or exotic compact objects [51] (e.g. boson stars [52]). GW signatures of any population of PBH below the astrophysical production provide a powerful statistical constraint on any solar or subsolar component, as evidenced by the sharp decline observed in 03 events. There could of course be rare events generated by solar or subsolar PBHs that might contribute to DM at the O(10%) level. One key ingredient is therefore to distinguish PBHs from other compact objects, e.g. through the measurements of the tidal disruption and tidal deformability Λ. A recent analysis has shown that for subsolar neutron-star binaries, the O4 and O5 projected sensitivities would allow measuring the effect of tidal disruption on the waveform in a large portion of the parameter space, also constraining the tidal deformability at O(10%) level, thus excluding a primordial origin of the binary. Viceversa, for subsolar PBH binaries, model-agnostic upper bounds on the tidal deformability can rule out neutron stars or more exotic competitors. Assuming events similar to the sub-threshold candidate SSM200308 reported in LVK O3b data are PBH binaries, O4 projected sensitivity would allow ruling out the presence of neutron-star tidal effects at ≈ 3σ C.L., thus strengthening the PBH hypothesis. Future experiments would lead to even stronger (> 5σ) conclusions on potential discoveries of this kind, see Fig. 2. PBHs of lunar mass, a regime where hints of unaccounted-for microlensing events have been reported by the OGLE survey of the galactic bulge [53], could be sufficiently numerous that nearby binaries might be detectable with future generation detectors [54]. This paper is available on arxiv under CC BY 4.0 DEED license. Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Authors: Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction Abstract and 1 Introduction 2 Some open questions 2 Some open questions 2.1 What is the abundance of PBHs? 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3 The PBH Roadmap 3.1 High redshift mergers 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 4 Conclusions and References 3.2 Sub-solar PBHs The detection of sub-solar BHs in a compact binary merger is regarded as one of the smoking gun signatures of PBHs. Indeed, BHs of astrophysical origin are not expected. The sub-solar mass range may be however populated by other compact objects like neutron stars, white dwarfs, or exotic compact objects [51] (e.g. boson stars [52]). GW signatures of any population of PBH below the astrophysical production provide a powerful statistical constraint on any solar or subsolar component, as evidenced by the sharp decline observed in 03 events. There could of course be rare events generated by solar or subsolar PBHs that might contribute to DM at the O(10%) level. One key ingredient is therefore to distinguish PBHs from other compact objects, e.g. through the measurements of the tidal disruption and tidal deformability Λ. A recent analysis has shown that for subsolar neutron-star binaries, the O4 and O5 projected sensitivities would allow measuring the effect of tidal disruption on the waveform in a large portion of the parameter space, also constraining the tidal deformability at O(10%) level, thus excluding a primordial origin of the binary. Viceversa, for subsolar PBH binaries, model-agnostic upper bounds on the tidal deformability can rule out neutron stars or more exotic competitors. Assuming events similar to the sub-threshold candidate SSM200308 reported in LVK O3b data are PBH binaries, O4 projected sensitivity would allow ruling out the presence of neutron-star tidal effects at ≈ 3σ C.L., thus strengthening the PBH hypothesis. Future experiments would lead to even stronger (> 5σ) conclusions on potential discoveries of this kind, see Fig. 2. PBHs of lunar mass, a regime where hints of unaccounted-for microlensing events have been reported by the OGLE survey of the galactic bulge [53], could be sufficiently numerous that nearby binaries might be detectable with future generation detectors [54]. This paper is available on arxiv under CC BY 4.0 DEED license. This paper is available on arxiv under CC BY 4.0 DEED license. available on arxiv

Sub-solar Primordial Black Holes

Authors:
(1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland;
(2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction 2 Some open questions 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 3.1 High redshift mergers The PBH model predicts a binary merger rate density which grows monotonically with redshift [31, 32, 33]. Focusing those binaries generated at early epochs, one has a well-defined time evolution with redshift This paper is available on arxiv under CC BY 4.0 DEED license. Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Authors: Authors: (1) Antonio Riotto, Département de Physique Theorique, Universite de Geneve, 24 quai Ansermet, CH-1211 Geneve 4, Switzerland and Gravitational Wave Science Center (GWSC), Universite de Geneve, CH-1211 Geneva, Switzerland; (2) Joe Silk, Institut d’Astrophysique, UMR 7095 CNRS, Sorbonne Universite, 98bis Bd Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, UK. Table of Links Abstract and 1 Introduction Abstract and 1 Introduction 2 Some open questions 2 Some open questions 2.1 What is the abundance of PBHs? 2.1 What is the abundance of PBHs? 2.2 What is the effect of PBH clustering? 2.2 What is the effect of PBH clustering? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.3 What fraction of the currently observed GW events can be ascribed to PBHs? 2.4 Are PBHs the Dark Matter? 2.4 Are PBHs the Dark Matter? 3 The PBH Roadmap 3 The PBH Roadmap 3.1 High redshift mergers 3.1 High redshift mergers 3.2 Sub-solar PBHs 3.2 Sub-solar PBHs 3.3 Plugging the pair instability gap with PBH? 3.3 Plugging the pair instability gap with PBH? 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 3.4 PBH eccentricity, 3.5 PBH spin and 3.6 Future gamma-ray telescopes 4 Conclusions and References 4 Conclusions and References 3.1 High redshift mergers The PBH model predicts a binary merger rate density which grows monotonically with redshift [31, 32, 33]. Focusing those binaries generated at early epochs, one has a well-defined time evolution with redshift This paper is available on arxiv under CC BY 4.0 DEED license. This paper is available on arxiv under CC BY 4.0 DEED license. available on arxiv

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