You Tube Video on the Cosmic Cycles on the Horizon

I don’t know about the quality of this. YouTube is probably censoring me because I’m talking about empowerment and being positive. That certainly goes against the narrative right now. But maybe you’ll see this clearly. I decided to do this spur of the moment.

The E.T. Are Heavily Monitoring Countries With Nukes

I feel it very strongly. They are enforcing the agreement with the Earth Keepers that was agreed to when humans came here as refugees from Maldek. I believe this tension between the government, their people, and the E.T. are raising the Schumann Resonance.

No nuclear weapons allowed again. The GGLN (Global Galactic League of Nations) has the authority to shut them down to protect the Cosmic Web. They’ve already done it previously.

Frankly, most G7 countries have no reason for being on earth if they can’t play with their bombs, decimate the planet, enslave the human race and turn it into a machine world. I think it’s time for them to leave so we can clean things up and have a life…WITHOUT THEM.

Ciao baby…anytime now.

The Cosmic Web Orchestrates the Progression of Galaxies

FEBRUARY 25, 2022

by Sarah Perrin, Ecole Polytechnique Federale de Lausanne

Cosmic web orchestrates the progression of galaxies
Position of the studied filaments. Credit: LASTRO/EPFL

The shape of galaxies and how they evolve depending on a web of cosmological filaments that run across the universe. According to a recent study headed by EPFL’s Laboratory of Astrophysics, this cosmic web plays a much bigger role than previously thought.

Across the universe, galaxies are distributed along what’s called the cosmic web, a complex network of filaments made up of ordinary and dark matter. And where those filaments intersect, galaxy clusters—collections of hundreds or even thousands of galaxies bound to each other by the force of gravity—tend to form. They are the biggest and densest clusters in the universe and are the subject of much research by astrophysicists. But precisely how filaments contribute to galactic evolution is still poorly understood.

To get deeper insight, an international team of scientists led by Prof. Pascale Jablonka and Gianluca Castignani from EPFL’s Laboratory of Astrophysics (LASTRO) examined the vast environment surrounding Virgo, a representative cluster in the local universe. It contains some 1,500 galaxies and is located around 65 million light-years away from our own galaxy, the Milky Way. The team’s findings have been published in two articles: one appearing in Astronomy & Astrophysics this past January and the other in Astrophysical Journal last fall.

“Many properties of galaxies, like their morphology, gas content, and star formation rate, are directly influenced by their environment,” says Jablonka. “We know that galaxies form fewer stars in very dense environments and adopt a more elliptical shape. But the exact role that filaments play in this transformation is still not clear. That’s what we wanted to investigate with our research.”

The scientists analyzed the properties of galaxies located around the Virgo cluster, across a region spanning 12 times the radius of the main cluster. Theirs is the largest study conducted to date on this topic and covers a sample size of some 7,000 galaxies, including 250 that are big enough for scientists to be able to precisely estimate their gas content—and especially the amount of cold, dense atomic hydrogen that stars are made out of. Measurements were taken using the decametric radio telescope in Nançay, France, and the IRAM-30m telescope in Pico Veleta, Spain.

A transitional environment

By combining the new data they collected with measurements from the literature, the scientists found that the properties of galaxies—namely, their shape, star formation rate, gas content, and the age and metal content of their stars—clearly change as the galaxies progress from more isolated positions towards filaments and eventually into clusters.

Filaments, therefore, seem to serve as a transitional environment where galaxies are pre-processed before falling into a cluster. In this environment, star formation slows or even stops altogether, elliptical shapes appear more frequently, and there is less atomic and molecular hydrogen, indicating that the galaxies are reaching the end of their active life. The scientists observed that a galaxy’s evolution through its life cycle corresponds to the local galaxy density: galaxies producing few or no stars made up less than 20% of the sample of isolated galaxies, but they accounted for 20–60% of galaxies in the filaments and some 80% of galaxies in the Virgo cluster. These findings open up new avenues of research on theories to explain galaxy formation and how galaxies evolve in tandem with major cosmic bodies.

Journal information: Astrophysical Journal  Astronomy & Astrophysics 

Provided by Ecole Polytechnique Federale de Lausanne 

This is why physicists suspect the Multiverse very likely exists


A wild, compelling idea without a direct, practical test, the Multiverse is highly controversial. But its supporting pillars sure are stable.


  • One of the most successful theories of 20th century science is cosmic inflation, which preceded and set up the hot Big Bang. 
  • We also know how quantum fields generally work, and if inflation is a quantum field (which we strongly suspect it is), then there will always be more “still-inflating” space out there. 
  • Whenever and wherever inflation ends, you get a hot Big Bang. If inflation and quantum field theory are both correct, a Multiverse is a must.

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When we look out at the Universe today, it simultaneously tells us two stories about itself. One of those stories is written on the face of what the Universe looks like today, and includes the stars and galaxies we have, how they’re clustered and how they move, and what ingredients they’re made of. This is a relatively straightforward story, and one that we’ve learned simply by observing the Universe we see.

But the other story is how the Universe came to be the way it is today, and that’s a story that requires a little more work to uncover. Sure, we can look at objects at great distances, and that tells us what the Universe was like in the distant past: when the light that’s arriving today was first emitted. But we need to combine that with our theories of the Universe — the laws of physics within the framework of the Big Bang — to interpret what occurred in the past. When we do that, we see extraordinary evidence that our hot Big Bang was preceded and set up by a prior phase: cosmic inflation. But in order for inflation to give us a Universe consistent with what we observe, there’s an unsettling appendage that comes along for the ride: a multiverse. Here’s why physicists overwhelmingly claim that a multiverse must exist.The ‘raisin bread’ model of the expanding Universe, where relative distances increase as the space (dough) expands. The farther away any two raisin are from one another, the greater the observed redshift will be by time the light is received. The redshift-distance relation predicted by the expanding Universe is borne out in observations, and has been consistent with what’s been known all the way back since the 1920s. (Credit: NASA/WMAP Science Team)

Back in the 1920s, the evidence became overwhelming that not only were the copious spirals and ellipticals in the sky actually entire galaxies unto themselves, but that the farther away such a galaxy was determined to be, the greater the amount its light was shifted to systematically longer wavelengths. While a variety of interpretations were initially suggested, they all fell away with more abundant evidence until only one remained: the Universe itself was undergoing cosmological expansion, like a loaf of leavening raisin bread, where bound objects like galaxies (e.g., raisins) were embedded in an expanding Universe (e.g., the dough).

If the Universe was expanding today, and the radiation within it was being shifted towards longer wavelengths and lower energies, then in the past, the Universe must have been smaller, denser, more uniform, and hotter. As long as any amount of matter and radiation are a part of this expanding Universe, the idea of the Big Bang yields three explicit and generic predictions:null

  1. a large-scale cosmic web whose galaxies grow, evolve, and cluster more richly over time,
  2. a low-energy background of blackbody radiation, left over from when neutral atoms first formed in the hot, early Universe,
  3. and a specific ratios of the lightest elements — hydrogen, helium, lithium, and their various isotopes — that exist even in regions that have never formed stars.

This snippet from a structure-formation simulation, with the expansion of the Universe scaled out, represents billions of years of gravitational growth in a dark matter-rich Universe. Note that filaments and rich clusters, which form at the intersection of filaments, arise primarily due to dark matter; normal matter plays only a minor role. (Credit: Ralf Kaehler and Tom Abel (KIPAC)/Oliver Hahn)

dark matter

All three of these predictions have been observationally borne out, and that’s why the Big Bang reigns supreme as our leading theory of the origin of our Universe, as well as why all its other competitors have fallen away. However, the Big Bang only describes what our Universe was like in its very early stages; it doesn’t explain why it had those properties. In physics, if you know the initial conditions of your system and what the rules that it obeys are, you can predict extremely accurately — to the limits of your computational power and the uncertainty inherent in your system — how it will evolve arbitrarily far into the future.

But what initial conditions did the Big Bang need to have at its beginning to give us the Universe we have? It’s a bit of a surprise, but what we find is that:

  • there had to be a maximum temperature that’s significantly (about a factor of ~1000, at least) lower than the Planck scale, which is where the laws of physics break down,
  • the Universe had to have been born with density fluctuations of approximately the same magnitude of all scales,
  • the expansion rate and the total matter-and-energy density must have balanced almost perfectly: to at least ~30 significant digits,
  • it must have been born with the same initial conditions — same temperature, density, and spectrum of fluctuations — at all locations, even causally disconnected ones,
  • and its entropy must have been much, much lower than it is today, by a factor of trillions upon trillions.

If these three different regions of space never had time to thermalize, share information or transmit signals to one another, then why are they all the same temperature? This is one of the problems with the initial conditions of the Big Bang; how could these regions all obtain the same temperature unless they started off that way, somehow? (Credit: E. Siegel/Beyond the Galaxy)

Whenever we come up against a question of initial conditions — basically, why did our system start off this way? — we only have two options. We can appeal to the unknowable, saying that it is this way because it’s the only way it could’ve been and we can’t know anything further, or we can try to find a mechanism for setting up and creating the conditions that we know we needed to have. That second pathway is what physicists call “appealing to dynamics,” where we attempt to devise a mechanism that does three important things.

  1. It has to reproduce every success that the model it’s trying to supersede, the hot Big Bang in this instance, produces. Those earlier cornerstones must all come out of any mechanism we propose.
  2. It has to explain what the Big Bang cannot: the initial conditions the Universe started off with. These problems that remain unexplained within the Big Bang alone must be explained by whatever novel idea comes along.
  3. And it has to make new predictions that differ from the original theory’s predictions, and those predictions must lead to a consequence that is in some way observable, testable, and/or measurable.

The only idea we’ve had that met these three criteria was the theory of cosmic inflation, which has achieved unprecedented successes on all three fronts.Exponential expansion, which takes place during inflation, is so powerful because it is relentless. With every ~10^-35 seconds (or so) that passes, the volume of any particular region of space doubles in each direction, causing any particles or radiation to dilute and causing any curvature to quickly become indistinguishable from flat. (Credit: E. Siegel (L); Ned Wright’s Cosmology Tutorial (R))

What inflation basically says is that the Universe, before it was hot, dense, and filled with matter-and-radiation everywhere, was in a state where it was dominated by a very large amount of energy that was inherent to space itself: some sort of field or vacuum energy. Only, unlike today’s dark energy, which has a very small energy density (the equivalent of about one proton per cubic meter of space), the energy density during inflation was tremendous: some 1025 times greater than dark energy is today!

The way the Universe expands during inflation is different from what we’re familiar with. In an expanding Universe with matter and radiation, the volume increases while the number of particles stays the same, and hence the density drops. Since the energy density is related to the expansion rate, the expansion slows over time. But if the energy is intrinsic to space itself, then the energy density remains constant, and so does the expansion rate. The result is what we know as exponential expansion, where after a very small period of time, the Universe doubles in size, and after that time passes again, it doubles again, and so on. In very short order — a tiny fraction of a second — a region that was initially smaller than the smallest subatomic particle can get stretched to be larger than the entire visible Universe today.In the top panel, our modern Universe has the same properties (including temperature) everywhere because they originated from a region possessing the same properties. In the middle panel, the space that could have had any arbitrary curvature is inflated to the point where we cannot observe any curvature today, solving the flatness problem. And in the bottom panel, pre-existing high-energy relics are inflated away, providing a solution to the high-energy relic problem. This is how inflation solves the three great puzzles that the Big Bang cannot account for on its own.

SPACE Wild New Paper Claims Earth May Be Surrounded by a Giant Magnetic Tunnel

Corey Goode posted this article on LinkedIn this morning.

“Who else thinks this sounds a lot like my 20-and-Back testimony from my movie ABOVE MAJESTIC where I described how the Galactic Portal System worked? These electromagnetic filaments ultimately connect to the Cosmic Web. CG:

Wild New Paper Claims Earth May Be Surrounded by a Giant Magnetic Tunnel -“


Left: what the tunnel would look like; right: what the sky does look like. (Image Credit Below)


Mysterious structures in the sky that have puzzled astronomers for decades might finally have an explanation – and it’s quite something. The North Polar Spur and the Fan Region, on opposite sides of the sky, may be connected by a vast system of magnetized filaments. These form a structure resembling a tunnel that circles the Solar System, and many nearby stars besides.

“If we were to look up in the sky,” said astronomer Jennifer West of the University of Toronto in Canada, “we would see this tunnel-like structure in just about every direction we looked – that is, if we had eyes that could see radio light.”

We’ve known about the two structures for quite some time – since the 1960s, in fact – but they have been difficult to understand. That’s because it’s really hard to work out exactly how far away they are; distances have ranged from hundreds to thousands of light-years away. However, no analysis had ever linked the two structures together.

West and her colleagues were able to show that the two regions, and prominent radio loops in the space between them, could be linked, solving many of the puzzling problems associated with both. Comparison with a real tunnel showing orientation. (Left: Pixabay/wal_172619/J. West; Right: Dominion Radio Astrophysical Observatory/Villa Elisa telescope/ESA/Planck Collaboration/Stellarium/J. West)

“A few years ago, one of our co-authors, Tom Landecker, told me about a paper from 1965, from the early days of radio astronomy. Based on the crude data available at this time, the authors (Mathewson & Milne), speculated that these polarized radio signals could arise from our view of the Local Arm of the galaxy, from inside it,” West explained. “That paper inspired me to develop this idea and tie my model to the vastly better data that our telescopes give us today.”

Using modelling and simulations, the researchers figured out what the radio sky would look like, if the two structures were connected by magnetic filaments, playing with parameters such as distance to determine the best fit. From this, the team was able to determine that the most likely distance for the structures from the Solar System is around 350 light-years, consistent with some of the closer estimates. This includes an estimate for the distance of the North Polar Spur earlier this year based on Gaia data, which found that almost all of the spur is within 500 light-years.

The entire length of the tunnel modeled by West and her team is around 1,000 light-years. Light intensity of the North Polar Spur (top) and Fan Region (bottom). (West et al., arXiv, 2021) This model is in agreement with a wide range of observational properties of the North Polar Spur and Fan Region, including the shape, the polarization of the electromagnetic radiation (that is, how the wave is twisted), and the brightness.

“This is extremely clever work,” said astronomer Bryan Gaensler of the University of Toronto. “When Jennifer first pitched this to me, I thought it was too ‘out-there’ to be a possible explanation. But she was ultimately able to convince me! Now I’m excited to see how the rest of the astronomy community reacts.”

More work is needed to first confirm the findings, and then model the structure in greater detail. But doing so may help to solve an even bigger mystery: the formation and evolution of magnetic fields in galaxies, and how these fields are maintained. It could also, the researchers said, provide context for understanding other magnetic filament structures found around the galaxy. The team is planning to perform more complex modelling; but, they suggest, more sensitive, higher-resolution observations would help reveal hidden details that show how the structure fits into the broader galactic context.

“Magnetic fields don’t exist in isolation. They all must connect to each other. So a next step is to better understand how this local magnetic field connects both to the larger-scale galactic magnetic field, and also to the smaller scale magnetic fields of our Sun and Earth,” West said. “I think it’s just awesome to imagine that these structures are everywhere, whenever we look up into the night sky.” The research is due to appear in The Astrophysical Journal, and is available on arXiv.

Cover image credit:  Dominion Radio Astrophysical Observatory/Villa Elisa telescope/ESA/Planck Collaboration/Stellarium/J. West © ScienceAlert US LLC. All rights reserved

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