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Author: admin, 07.06.2014. Category: The Power Of Attraction

Wikipedia a€?Year of Sciencea€? Edita€?aa€?thon (by Meredith Rawls)Whata€™s your first go-to source for an unfamiliar topic on the internet? To address this, the AAS Astronomy Education Board teamed up with the Wiki Education Foundation to host an edit-a-thon as part of the Wikipedia Year of Science. The Year of Science initiative seeks to bring Wikipedia editing skills to the classroom and help new editors find sustainable ways to contribute to Wikipedia in the long term. As a first-time Wikipedia contributor, I took the time to go through nearly all the tutorial exercises and familiarize myself with the process of editing a page. After the town-hall with an open mic that raised exceptional questions in the morning, some of the pioneers of the field of scientific cosmology were here with their concluding remarks about the future of the field. He touched upon multiverses with his analogy of a€?a submarine floating in a sea with just the right amount of buoyancy balancing gravitya€™ a€“ a multiverse can have universes with different parameterized cosmological constants! This a€?The Limits of Scientific Cosmologya€? series at #aas228 has been absolutely fantastic. Press Conference a€“ Black Holes and Gamma-Ray Bursts (by Susanna Kohler)The final press conference of the meeting covered three topics from the categories of black holes and gamma-ray bursts.
Rasio focused on the second theory, in which that black holes are formed in dense stellar clusters.
Next up was Richard Henry (Johns Hopkins University), who spoke about the internal structure of spinning black holes (known as Kerr black holes). The final press conference presentation was given by Maria Dainotti (Stanford University) on the subject of using gamma-ray bursts (GRBs) as standard candles. Type Ia supernovae (which always have roughly the same source brightness) are a typical example of a standard candle, and led to the discovery of dark energy in the 1990s.
Mike Normana€™s (University of California a€“ San Diego) plenary talk concluded the AAS Plenary sessions with a treatise on the current generation of simulations that aim to characterize the first stars and galaxies that formed in the Universe. Mike has been working in the field for a long time, and his collaboratorsa€™ work on the Enzo simulations is very well known. Michael Norman shows some new computational simulations of ionization in the early Universe.
The statistics of these first galaxies (from the above mentioned Renaissance simulations) show that the first galaxies formed around a redshift of z = 20, roughly around the same time as the first stars, and way before the actual epoch of reionization (at z ~ 7, the concept is described here).
Juno will go in to orbit at Jupiter on July 5 (July 4 in North and South American time zones), and it's carrying a camera that's going to take really awesome photos of Jupiter. A guide to interesting stuff going on in space science, space exploration, and space advocacy. Today ESA released ExoMars Trace Gas Orbiter's first photo of Mars, taken from a distance of 41 million kilometers. The idea that dark matter is made of primordial black holes is very old but has always been in the backwater of particle physics. So, let us do a recap of what was the situation for the strength of the signals for the decays of the Higgs particle.
From the table one can see that the signal strengths for decays in ATLAS are somewhat beyond unity while in CMS these are practically unity for but, more interestingly, 0.85 for . At LHCP2016 new data have been presented from the two collaborations, at least for the decay.
This result is striking per seA as shows a tendency toward a decreasing value when, in precedence, it was around unity. I was travelling back from Cambridge on the train yesterday afternoon when I saw the announcement that the Advanced LIGO team had found a second gravitational wave source.
TheA  signal shown above, code-named GW151226, like the previous one, appears to be from a black hole binary coalescence but it involves two black holes of rather lower masses (about 14 and 8 solar masses respectively). Actually from my point of view the really interesting challenge is to make full use of the low signal-to-noise detections that are probable sources but with some uncertainty. Well, this conversation (for the book) takes place in a (famous) railway station, so it would be neglectful of me to not have people scurrying around and so forth. This is a screen shot (literally, sort of - I just pointed a camera at it) of a detailed large panel in progress. SpaceX placed two communications satellites into orbit today, but the company's attempt to go four-in-a-row on first stage drone ship recoveries fell short. Curiosity is at a turning point in its mission to Mount Sharp, both literally and figuratively.
Among the sessions I attended yesterday, I really liked the one on robustness and model mispecification.
The first session on Wednesday at 228th AAS Meeting was the Newton Lacy Pierce Prize Lecture by Heather Knutson (California Institute of Technology). One of her first points is the well-known idea that the Solar System is an oddball, compared to the exoplanet systems we have found so far: most of these systems contain hot Jupiters and mini-Neptunes at very close-in orbits around their host stars. On December 26th 2015, LIGO detected its second full-fledged gravitational wave event, dubbed GW151226 (the numbers signify the date it was detected).
This discovery further solidifies this nascent field into astronomy, and has given astronomers a new sense to explore the Universe.
Our zoo of stellar-mass black holes, including the 2 confirmed LIGO event, the 1 LIGO candidate, and indirect evidence from X-ray binaries. Star Formation in a Range of Environments (by Benny Tsang)David Cook began our morning star formation session with his work on the connection between the slopes of luminosity functions for star-forming regions and the host-galaxy properties. Kaveh Vasei took us on his journey estimating the escape fraction of Lyman continuum photons from galaxies.
Philip Hopkins then continued the theoretical discussion and showed that enough ionizing photons for cosmic reionization could be obtained if we consider binary stars. Following this morninga€™s exciting press conference, Gabriela GonzA?lez, spokesperson for the LIGO Scientific collaboration, gave the Kavli Foundation Plenary Lectureship.
GonzA?lez opened the plenary by digging a little further into the physics of LIGO detections. Our ability to localize gravitational-wave detections currently relies on the timing of the observations: noting the difference in time between when the signal passes the LIGO Livingston and LIGO Hanford detectors (on the scale of 10 ms) can give us a broad sense of where in the sky the signal came from.
Gonzalez: the addition of Virgo will significantly improve our ability to localize the sources. As a final note, GonzA?lez pointed out that detections by ground-based gravitational-wave interferometers are only the start of gravitational-wave astronomy.
For a second time, scientists from the LIGO and Virgo collaborations saw gravitational waves from the merger of two black holes. Scientists from the LIGO and Virgo collaborations announced today the observation of gravitational waves from a set of merging black holes.
This follows their previous announcement, just four months ago, of the first ever detection of gravitational waves, also from a set of merging black holes. The detection of gravitational waves confirmed a major prediction of Albert Einsteina€™s 1915 general theory of relativity. Gravity is by far the weakest of the known forces, but if an object is massive enough and accelerates quickly enough, it creates gravitational waves powerful enough to be observed experimentally. LIGO consists of two huge interferometers in Livingston, Louisiana, and Hanford, Washington. Scientists on the Virgo collaboration have been working with LIGO scientists to analyze their data. With this second observation, a€?we are now a real observatory,a€? said Gabriela Gonzalez, LIGO spokesperson and professor of physics and astronomy at Louisiana State University, in a press conference at the annual meeting of the American Astronomical Society. On Christmas evening in 2015, a signal that had traveled about 1.4 billion light years reached the twin LIGO detectors. The black holes were 14 and eight times as massive as the sun, and they merged into a single black hole weighing 21 solar masses. The LIGO detectors saw almost 30 of the last orbits of the black holes before they coalesced, Gonzalez said during the press conference. Additional detectors will make it possible not only to find evidence of gravitational waves, but also to triangulate their origins. On its own, LIGO is a€?more of a microphone,a€? capturing the a€?chirpsa€? from these events, Gonzalez said. The next event scientists are hoping to a€?heara€? is the merger of a pair of neutron stars, said Caltecha€™s David Reitze, executive director of the LIGO laboratory, at the press conference.
Whereas two black holes merging are not expected to release light, a pair of neutron stars in the process of collapsing into one another could produce a plethora of observable gamma rays, X-rays, infrared light and even neutrinos. In the future, gravitational wave hunters hope to be able to alert astronomers to an event with enough time and precision to allow them to train their instruments on the area and see those signals. Therea€™s additional news from LIGO (the Laser Interferometry Gravitational Observatory) about gravitational waves today. The signal is not so a€?brighta€? as the first one, so it cannot be seen by eye if you just look at the data; to find it, some clever mathematical techniques are needed. It is interesting that we already have two, maybe three,A mergers of large black holesa€¦ and no mergers of neutron stars with black holes or with each other, which are harder to observe.
Highlights include black holes mosh pits leading to LIGO sources, using GRBs as standard candles, cosmological simulations of the early universe, and changing the scientific information on the internet with a Wikipedia edit-a-thon.
A team of astrobiters isA attending the conference this year, and we will report highlights from each day here on astrobites.
More than forty attendees spent the better part of three hours working through tutorials, creating new articles, and editing existing ones.


John Carlstrom laid down the pipeline for future surveys that not only provide us with interesting constraints on current physics, but give us the opportunity to test new physics. Moreover, in Susskinda€™s opinion, the only true limit that inhibits our understanding of the features of our universe beyond the cosmic event horizon was the event horizon of an event or phenomena. These black holes then sink (via dynamical friction) to the centers of the clusters like dust particles settling on the floor of a room, where they form binaries in a a€?black hole mosh pita€? a€” eventually getting kicked out of the cluster by dynamical interactions. Because no light can escape from black hole interiors, we cana€™t learn whata€™s in them via observation.
But if GRBs could be used in a similar way, they would be a much more powerful tool: theya€™re visible out to significantly further distances because theya€™re so bright.
This talk was centered around some of the latest Enzo results, with a special emphasis on tracking down the Epoch of Reionization with a new series of runs called the Renaissance simulations. The simulation results extended this evolution to the epoch of reionization and put interesting constraints on observations of this epoch, when we can actually see the ionized gas from this epoch in our observations.
It's no more detail than you can get through a pair of a binoculars, just a little taste of what's to come. The WIMP or asymmetric dark matter paradigms are preferred for several reasons such as calculability, observational opportunities, and a more direct connection to cherished theories beyond the Standard Model. We all have seenA the history unfolding since the epochal event on 4 July 2012 where the announcement of the great discovery happened.
Data gathered on 2015 seem to indicate a further state at 750 GeV but this is yet to be confirmed. As I pointed out here, there is a curious behavior of the strengths of the signals of Higgs decay in and some tension, even if small, appeared between ATLAS and CMS results. If the state at 750 GeV should be confirmed, as the spectrum given by the exact solution of the Higgs sector is given by an integer multiplied by a mass, this would be at .
Then, summer conferences will start and, paraphrasing Coleman: God knows, I know and by the end of the summer we all know. Actually, I knew this one was coming a€“ the event actually registered last Christmas a€“ but I had forgotten that it was to be announced at the American Astronomical Society meeting thata€™s happening now in San Diego. I hope to write a blog post soon about how Bayesian methods can help a great deal with that. After three days in Cambridge as External Examiner, I now have to chair our undergraduate finalist examination board here at Sussex.
Having drilled at three sample sites in 7 weeks, the rover took a left turn, changing its trajectory from a generally westward driving path to a southward one.
Especially the talk by Steve McEachern on Bayesian inference based on insufficient statistics, with a striking graph of the degradation of the Bayes factor as the prior variance increases.
This morning LIGO reporting on the results from its first observing run and announced the confirmation of a second gravitational wave event - GW151226! This talk featured a broad range of research efforts on exoplanets, with the main focus on how we study the composition of their atmospheres, and how multi-body interactions carve the structure of the planetary systems we observe.
Moreover, even when studying their transmission spectra, it is difficult to know the exact composition of their atmospheres.
The next observing run of LIGO will commence later in 2016 and will be more sensitive due to system upgrade, increasing the rate at which LIGO should detect these types of astrophysical events. A moderate-strong trend was found: galaxies with higher star formation rate surface densities (the star formation rate per area projected on the sky) tend to have flatter luminosity functions. He argued that the commonly used indirect methods in determining the escape fraction should only be interpreted as upper limits, and showed us the highest-resolution image of Lyman continuum leakers so far.
The idea is that material transfer within binary systems could extend the lifetimes of massive stars, thereby allowing them to produce enough ionizing photons before they die.
Though the Kavli lecture usually opens the AAS meeting, it was moved this week to accommodate the schedule for LIGOa€™s big announcement today! She described how the detectors work, pointing out that theya€™re designed to detect a strain of 1 part in 1021. Our ability to localize will significantly improve when future detectors like Virgo (Europe), LIGO-India, and KAGRA (Japan) come online within the next decade. There were actually three significant gravitational-wave triggers in the first science run; the third has an 85% probability of being astrophysical, compared to the nearly 100% probability of the two official detections.
Future observatories and missions (like eLISA, and improved-sensitivity pulsar timing arrays) will expand the search for gravitational waves to different frequency ranges.
Einstein posited that every object with mass exerts a gravitational pull on everything around it. LIGO, or Laser Interferometer Gravitational-wave Observatory, caught the two sets of gravitational waves using lasers and mirrors. The distant merging of two black holes caused a slight shift in the fabric of space-time, equivalent to changing the distance between the Earth and the sun by a fraction of an atomic diameter. That might sound like a lot, but these were relative flyweights compared to the black holes responsible for the original discovery, which weighed 36 and 29 solar masses. The black holes had 14 solar masses and 8 solar masses, and merged into a black hole with 21 solar masses, emitting 1 solar mass of energy in gravitational waves. It seems there really are a lot of big black holes in binary pairs out there in the universe. When LIGO starts its next run, six months long starting in September, the improvements over last yeara€™s run will probably give a 50% to 100% increase in the rate for observed mergers. For many people, Wikipedia is the primary source of information about astronomy and science.
Others created biography pages from scratch or selected various astronomical topics to write about. He discussed the CMB, galaxy cluster growth, the Hubble constant and Baryonic Acoustic oscillations as parameters that would define our model of the universe cohesively in the future. Jim Peebles concluding this mesmerizing series of talks with his opinions on how physics ought to be direct and assertive with its theories, and should take pride in its explanatory power (or should it?). After all, in Sean Carrolla€™s words, we do live in a a€?preposterous universea€?, and the time is almost right to explain it all. We can use the light we observe from standard candles to estimate their distance, making them useful tools for testing cosmological models. Dainotti and collaborators are analyzing a subset of GRBs from Swift observations that they term a€?gold GRBsa€?. Investigations are ongoing, and Mike Normana€™s team is positive that the Enzo simulations are here to stay for a long time, challenging and collaborating with observations along the way. But in the recent months there has been more interest, triggered in part by the LIGO observations of black hole binary mergers.
Anyway, both ATLAS and CMS see this bump in the data and this seems to follow the story of the discovery of the Higgs particle.
Indeed, ATLAS seemed to have seen more events than CMS moving these contributions well beyond the unit value but, as CMS had them somewhat below, the average was the expected unity agreeing with expectations from the Standard Model.
In order to see if the scenario provided from the exact solution of the Higgs sector is in agreement with data, these should be confirmed from run II and those from ATLAS should go down significantly.
The value seen is again in agreement with that given in the exact solution of the Higgs sector. Together with the production strengths, if further data will confirm them, the proper scenario for the breaking of electroweak symmetry is exactly the one described by the exact solution. It may not look visually as clear as the first source, GW150914, which involved black holes with masses in the region of 30 solar masses, but ita€™s a clear detection and ita€™s also interesting that the models suggest that at least one of the black holes has a significant spin. I was wondering last night how long it will take before every individual discovery like this is no longer reported. I sadly had no time to grab a picture of the graph, which compared this poor performance against a stable rendering when using a proper summary statistic.
Knutson and her group a€” The Friends of Hot Jupiters a€” study systems with close-in gas giants and their frequency of binary companions, which are supposed to be the main culprits causing gas-giant migration. In addition, more detectors will be joining the network of gravitational wave observatories over the next few years, which will further constrain the location at which these events occur in the cosmos and increase the likelihood of detecting an electromagnetic counterpart to a gravitational wave event.
It was interpreted as the result of increased star formation efficiencies in high-density environments, which led to a large number of bright regions. David Guszejnov then led the first theoretical talk on modeling star formation using semi-analytical models a€“ an approach between full-blown numerical simulations and pen-and-paper calculations. This is roughly the same as measuring if the Earth-Sun distance changed by the size of a single atom! The fact that there have been so many detections already a€” despite the fact that LIGO is only at 40% of its design sensitivity a€” suggest that we can expect many more to come!
When a massive object moves, its pull changes, and that change is communicated in the form of gravitational waves. At the end of each arm, the split beams bounce off of mirrors and return to recombine in the center. In contrast to the September event, which was short and showed just a few orbits before the merger, in this event nearly 30 orbits over a full second are observed, making more information available to scientists about the black holes, the merger, and general relativity. If it is really due to gravitational waves, it would be merging black holes againa€¦ midway in size between the September and December eventsa€¦ but it is borderline, and might just be a statistical fluke.
Incidentally, the question of whether they might form the dark matter of the universe has been raised; ita€™s still a long-shot idea, since there are arguments against it for black holes of this size, but seeing these merger rates one has to reconsider those arguments carefully and keep an open mind aboutA the evidence. More detectors will allow scientists to know where on the sky the merger took place, which then can allow normal telescopes to look for flashes of light (or other forms of electromagnetic radiation) that might occur simultaneously with the mergera€¦ as is expected for neutron star mergers but not widely expected for black hole mergers.


However, many Wikipedia articles about science topics are incomplete or missing, and women are underrepresented among scientists with biographies.
To me, the editing process felt like a cross between writing a blog post and a journal article, in a hack day type environment. The importance of facilities like LSST, SKA, DESI, CMB-S4 were discussed, and Carlstrom emphasized that over the next two decades these fantastic machines will decide the fate of scientific cosmology. If the binary survives the process of both stars collapsing into black holes, then a binary black hole system results. Henry and collaborators have developed a new coordinate-invariant depiction of the structure of black holes that reframes how we think about visualize their interiors. By examining the correlations between parameters of these gold GRBs, Dainotti attempts to understand whether they can be used as standard candles.
Mikea€™s team uses Blue Waters, USAa€™s fastest supercomputer, situated in NCSA at Urbana-Champaign, Illinois (which also manages the large datasets coming out of the Dark Energy Survey!). In the first observed event, the mass of each of the black holes was estimated at around 30 solar masses.
What is still there is our need of a deep understanding of the Higgs sector of the Standard Model. The strength of the signals is essential to understand if the propagator of the Higgs field is the usual free particle one or has some factor reducing it significantly with contributions from higher states summing up to unity. The value 0.85 is really in agreement with the already cited exact computations from the Higgs sector but, within the error, in overall agreement with the Standard Model. Of course, this should be obviously true but an experimental confirmation is essential for a lot of reasons, last but not least the form of the Higgs potential that, if the numbers are these, the one postulated in the sixties would be the correct one. The same thing happened with the first few extra-solar planets but now that we have thousands, ita€™s only a subset a€“ those that might plausibly be similar to Earth a€“ that get press attention. It clearly relates to our work on ABC model choice, as well as to my worries about the Bayes factor, so this explains why I am quite excited about this notion of restricted inference. They found that approximately half of the observed systems have long-distance companions, providing strong validation of the migration scenario. Though less visible by eye in the data, sophisticated search algorithms that match theoretically-produced templates of the gravitational waveform were able to extract it from the data and build up enough statistical confidence to declare it as a detection.
Next, Daniel Carson presented his dissertation work on the observations of nuclear star clusters in disk galaxies.
The advantage of such an approach is that you could explore different star formation models (with or without feedback) very quickly. An asymmetric distribution of nitrogen-bearing species was found, which could be due to disk fragmentation on unresolved scales and the formation of multiple sources with different ages.
If a gravitational wave passes through the laser beams as they travel, it stretches space-time in one direction and compresses it in another, creating a mismatch between the two. Working through the tutorial and some examples renewed my empathy for learners who are tackling a new skill set for the first time.
Leonard Susskind followed this up with a theoretical framework of how the ideas of inflation and vacuum energy could lead to our understanding of whether String Theory could be the correct theory of the universe.
The talk described the initial dark matter and gas dynamics along with a dark energy-supported metric evolution using simulations of a cosmic box that was the initial universe. While such a system may well be of boring astrophysical origin, it is somewhat unexpected because typical black holes we come across in everyday life are either a bit smaller (around one solar mass) or much larger (supermassive black hole in the galactic center). Quite recently, LHC restarted operations at the top achievable and data are gathered and analysed in view of the summer conferences. The reason is that, in run I, gathered data were not enough to reduce the error bars to such small values to decide if Standard Model wins or not. In this case, the observed state at 125 GeV would be just the ground state of a tower of particles being its excited states. This seems to point toward on overestimated number of events in ATLAS but a somewhat reduced number of events in CMS, at least for decay.
This is the most shocking result: They see a significant reduced set of events and the signal strength they obtain isA now alignedA to the one of CMS (see Strandberga€™s talk at page 11).
An other important reason is that coupling with other matter does not change the spectrum of the theory in a significant way.
At the current rate of discovery gravitational-wave sources may well become quite common over the next few years.
In this session, Chris Holmes also summarised his two recent papers on loss-based inference, which I discussed here in a few posts, including the Statistical Science discussion Judith and I wrote recently. The system was estimated to have merged at a distance of 1.4 billion light-years, and, due to its lower mass, stayed in LIGOa€™s detection band for a full second (5 times longer than the more massive GW150914).
The semi-analytical models with feedback reproduced observables such as the slope and turnover of the initial mass function well, and this technique can also further the understanding of binary-star formation. The linear fluctuations of this a€?initial universea€™ formed the first stars (called Population III stars in the astrophysics community) from hydrogen and helium generated in the Big Bang. On the other hand, if the dark matter halo were made of black holes, scattering processes would sometimes create short-lived binary systems. As I showed recently, this is not physics beyond the Standard Model, rather is obtained by solving exactly the quantum equations of motion of the Higgs sector (see here).
In fact a reasonable prediction for when LIGO is switched on again at the end of the summer that there might be a detection every week or so.
Knutson speculates that wide binaries have more massive disks, which in turn produce more gas giants, populating our surveys with such planets.
Stellar population modeling also revealed the star formation histories and stellar masses of the clusters. Mike and his team established a catalogue of these first stars, and parameterized these into a function that modeled how these stars became the first galaxies, and eventually into the larger galaxies from the merger of smaller galaxy halos. Assuming a significant fraction of dark matter in the universe is made of primordial black holes, this paper estimated that the rate of merger processes is in the right ballpark to explain the LIGO events.Primordial black holes can form from large density fluctuations in the early universe. So, several theoretical proposals for the Higgs sector still stand up and could be also confirmed already in August this year.
This is done considering the other fields interacting with the Higgs field just a perturbation.
The stellar mass surface density of IC342 was measured to lie above the theoretical maximum set by stellar feedback. On the largest observable scales the universe is incredibly homogenous, as witnessed by the uniform temperature of the Cosmic Microwave Background over the entire sky. However on smaller scales the primordial inhomogeneities could be much larger without contradicting observations. A From the fundamental point of view, large density fluctuations may be generated by several distinct mechanism, for example during the final stages of inflation in the waterfall phase in the hybrid inflation scenario.
While it is rather generic that this or similar process may seed black hole formation in the radiation-dominated era, severe fine-tuning is required to produce the right amount of black holes and ensure that the resulting universe resembles the one we know.All in all, it's fair to say that the scenario where all or a significant fraction of A dark matter A is made of primordial black holes is not completely absurd.
Moreover, one typically expects the masses to span a fairly narrow range.A Could it be that the LIGO events is the first indirect detection of dark matter made of O(10)-solar-mass black holes?
A Black holes sloshing through the early dense universe accrete the surrounding matter and produce X-rays which could ionize atoms and disrupt the Cosmic Microwave Background. In astrophysics, however, not only signals but also constraints should be taken with a grain of salt.
A In this particular case, the word in town is that the derivation contains a numerical error and that the corrected limit is 2 orders of magnitude less severe than what's shown in the plot.
Moreover, this limit strongly depends on the model of accretion, and more favorable assumptions may buy another order of magnitude or two. All in all, the possibility of dark matter made of A primordial black hole in the 10-100 solar mass range should not be completely discarded yet. Another possibility is that black holes make only a small fraction of dark matter, but the merger rate is faster, closer to the estimate of this paper.Assuming this is the true scenario, how will we know?
Direct detection of black holes is discouraged, while the usual cosmic ray signals are absent. Instead, in most of the mass range, the best probes of primordial black holes are various lensing observations. These are strong radio signals of (probably) extragalactic origin and millisecond duration.
The radio signal passing near a O(10)-solar-mass black hole could be strongly lensed, leading to repeated signals detected on Earth with an observable time delay. In the near future we should observe hundreds of such repeated bursts, or obtain new strong constraints on primordial black holes in the interesting mass ballpark. A When more statistics is accumulated, we will be able to say something about the spatial distributions of the merger events. Primordial black holes should be distributed like dark matter halos, whereas astrophysical black holes should be correlated with luminous galaxies. Also, the typical eccentricity of the astrophysical black hole binaries should be different.



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