# The Largest 2D Map of the Universe Has Just Been Revealed

An episode of [Bedtime Astronomy](https://invisiblenetwork.ai/podcast/1736397134), 28 Aug 2026, 37 min.

Audio: https://dts.podtrac.com/redirect.mp3/api.spreaker.com/download/episode/73840648/2dmap.mp3

The DESI Legacy Imaging Surveys have unveiled the largest 2D color map of the universe, cataloging nearly four billion celestial objects across 75% of the sky. Built from more than 260,000 telescope exposures and infrared data, this publicly available atlas will help scientists explore dark energy, dark matter, and gravitational lenses—while providing a crucial foundation for future observatories. Thank you for listening to Bedtime Astronomy — your guide to the cosmos. New episodes on space exploration, NASA missions & the latest astronomy breakthroughs. This episode includes AI-generated content.

## Transcript

[0:03] Speaker 1: Welcome to Bedtime Astronomy. Explore the wonders of the cosmos
[0:07] Speaker 1: with our soothing Bedtime Astronomie podcast. Each episode offers a
[0:12] Speaker 1: gentle journey through the stars, planets, and beyond, perfect for
[0:16] Speaker 1: unwinding after a long day. Let's travel through the mysteries
[0:20] Speaker 1: of the universe as you drift off into a peaceful
[0:22] Speaker 1: slumber under the night sky.
[0:26] Speaker 2: I want you to start by doing a quick auditory
[0:28] Speaker 2: and visual thought experiment with you.
[0:30] Speaker 3: Okay, I'm game.
[0:31] Speaker 2: So imagine you are walking outside tonight, You're somewhere completely isolated,
[0:36] Speaker 2: right miles and miles away from the light pollution of
[0:38] Speaker 2: any major city, and you just look up at.
[0:40] Speaker 3: The night sky, and you really have to let your
[0:42] Speaker 3: eyes adjust to the darkness for a good twenty minutes
[0:45] Speaker 3: to get.
[0:46] Speaker 2: The full effect exactly, and under ideal conditions, with perfect
[0:50] Speaker 2: vision and the absolute darkest possible spot on Earth, your
[0:54] Speaker 2: naked eye can pick out roughly, I think it's two
[0:57] Speaker 2: and a half to maybe three thousand individuals.
[1:00] Speaker 3: Yeah, that sounds about right.
[1:01] Speaker 2: And honestly, just staring into that vault of three thousand
[1:06] Speaker 2: points of light is usually enough to trigger this profound
[1:10] Speaker 2: sense of vertigo in anyone who really stops to think
[1:13] Speaker 2: about what they're looking at.
[1:14] Speaker 3: It's that crushing, overwhelming realization of cosmic scale.
[1:18] Speaker 2: Right, It's a physical sensation of feeling incredibly, unfathomably small.
[1:23] Speaker 2: So I want you to hold onto that exact feeling
[1:25] Speaker 2: of awe, and I want you to multiply that feeling
[1:28] Speaker 2: by four billion.
[1:29] Speaker 3: Which I mean the human brain simply does not possess
[1:32] Speaker 3: the cognitive architecture to visualize four billion discrete celestial objects.
[1:37] Speaker 3: We can't do it.
[1:38] Speaker 2: No, it's impossible.
[1:39] Speaker 3: We can write the number down, we can run mathematical
[1:43] Speaker 3: operations on it, but actually holding the visual reality of
[1:46] Speaker 3: four billion distinct galaxies and stars in your mind simultaneously
[1:51] Speaker 3: is just a biological impossibility.
[1:53] Speaker 2: Okay, well, let's impact this because we aren't just playing
[1:55] Speaker 2: with theoretical math today. Yesterday, August tenth, twenty twenty six,
[2:00] Speaker 2: this monumental event occurred in the astrophysics community.
[2:03] Speaker 3: A literal paradigm shift.
[2:04] Speaker 2: Yeah, the team behind the DIA Legacy imaging surveys officially
[2:08] Speaker 2: released the largest, most detailed, two dimensional color map of
[2:11] Speaker 2: the universe that humanity has ever assembled.
[2:13] Speaker 3: And we should clarify this isn't just a loose collection
[2:16] Speaker 3: of disparate photographs in a folder somewhere right.
[2:18] Speaker 2: No, it is a single, unified, continuously navigable image comprising
[2:22] Speaker 2: an unfathomable five point six trillion pixels.
[2:26] Speaker 3: The release of this data fundamentally alters our relationship with
[2:29] Speaker 3: the cosmos. It really moves astronomy from a discipline of
[2:33] Speaker 3: isolated observation into an era of holistic total environment modeling.
[2:40] Speaker 2: Because it's practically everything we can see exactly.
[2:43] Speaker 3: This massive map is serving as the foundational blueprint that
[2:47] Speaker 3: astrophysicists are currently using to unravel some of the most
[2:51] Speaker 3: stubborn mysteries in physics. I mean, it is the framework
[2:54] Speaker 3: upon which the next century of cosmology will be built.
[2:58] Speaker 2: So the stakes here are well astronomical in every sense
[3:02] Speaker 2: of the word. We're going to explore the mechanical and
[3:04] Speaker 2: the computational nightmare of how an image of this magnitude
[3:08] Speaker 2: was actually engineered in the.
[3:09] Speaker 3: First place, because it is a nightmare.
[3:11] Speaker 2: Oh completely. And we're also going to look at the
[3:13] Speaker 2: hidden structure of dark manner that this map brings into
[3:16] Speaker 2: the light. But the real destination of this conversation, and
[3:19] Speaker 2: I think the reason this map is dominating every single
[3:21] Speaker 2: scientific channel today. Is this shocking recent discovery enabled by
[3:25] Speaker 2: this very data.
[3:26] Speaker 3: A discovery that might force us to entirely rewrite the
[3:29] Speaker 3: ultimate fate of our universe.
[3:31] Speaker 2: Yeah, we're looking at early data indicators that challenge what
[3:35] Speaker 2: decades of deeply entrenched foundational cosmological theory.
[3:39] Speaker 3: Yes, the standard models of physics are actively being interrogated
[3:43] Speaker 3: right now because of what is hidden in those five
[3:45] Speaker 3: point six trillion pixels.
[3:47] Speaker 2: But before we reach the actual edge of the universe
[3:50] Speaker 2: and the unraveling of theoretical physics as we know it,
[3:53] Speaker 2: we really need to anchor ourselves in the sheer physical
[3:56] Speaker 2: scale of this.
[3:57] Speaker 3: Map, right, we need to understand what we're looking at first.
[3:59] Speaker 2: Exactly five point six trillion pixels. Let's just try to
[4:03] Speaker 2: contextualize that for a second. If you were to display
[4:05] Speaker 2: this map on a high end four K monitor, yeah,
[4:08] Speaker 2: which pushes about eight million pixels on its own, you
[4:12] Speaker 2: need to stack nearly seven hundred thousand of those monitors
[4:16] Speaker 2: edge to edge just to view the entire map at
[4:18] Speaker 2: its native, uncompressed resolution.
[4:21] Speaker 3: And that's just a staggering physical footprint.
[4:23] Speaker 2: It catalogs nearly four billion objects. And we aren't just
[4:26] Speaker 2: talking about local stars here.
[4:28] Speaker 3: Right now now, mostly we are looking at entire distant galaxies,
[4:31] Speaker 3: each one containing hundreds of billions of their own stars.
[4:34] Speaker 2: But in reading the technical specs of the release yesterday,
[4:38] Speaker 2: there's this massive caveat that immediately jumped out of me.
[4:42] Speaker 2: This map is being touted as the most comprehensive few
[4:45] Speaker 2: of the cosmos ever created, but it only covers roughly
[4:48] Speaker 2: seventy five percent of the sky.
[4:50] Speaker 3: Yeah, that limitation is dictated entirely by our physical location
[4:54] Speaker 3: in space.
[4:54] Speaker 2: Wait, hold on, if the objective was to map the
[4:57] Speaker 2: entire universe, why stop at seventy five percent? Like what
[5:01] Speaker 2: physical barrier is hiding a full quarter of the cosmos
[5:05] Speaker 2: from our most advanced telescopes.
[5:07] Speaker 3: Well, to visualize this, think about trying to look out
[5:09] Speaker 3: of a heavily smudged, dirty window while someone has a
[5:13] Speaker 3: brutally bright halogen lamp turned on right behind you inside
[5:17] Speaker 3: the room.
[5:17] Speaker 2: Okay, yeah, I can picture that.
[5:18] Speaker 3: You want to see the distant mountains outside, right, but
[5:21] Speaker 3: the glare reflecting off the grime right in front of
[5:23] Speaker 3: your face completely blinds you to the landscape.
[5:26] Speaker 2: You literally can't see past the glass exactly.
[5:28] Speaker 3: So the dirty window and the blinding lamp represent the
[5:31] Speaker 3: structural reality of the Milky Way galaxy. We as observers
[5:36] Speaker 3: operate from a highly disadvantageous vantage point for extra galactic.
[5:39] Speaker 2: Astronomy because we're stuck inside it.
[5:42] Speaker 3: Right Our solar system is embedded deep within one of
[5:46] Speaker 3: the spiral arms of the Milky Way, roughly halfway out
[5:49] Speaker 3: from the galactic center. So when we look out into
[5:51] Speaker 3: the broader universe, we have to look through our own
[5:54] Speaker 3: galaxy to see it.
[5:55] Speaker 2: And I'm assuming that's the dirty window.
[5:57] Speaker 3: It is. The Milky Way contains hundreds of billions of stars,
[6:01] Speaker 3: generating immense light the halogen lamp, but more problematically, the
[6:05] Speaker 3: galactic plane is choked with vast clouds of interstellar dust
[6:09] Speaker 3: and cold molecular.
[6:10] Speaker 2: Gas the grime on the window.
[6:12] Speaker 3: Yes, interstellar dust is incredibly efficient at scattering and absorbing
[6:16] Speaker 3: visible and ultraviolet light. So astronomers historically refer to the
[6:21] Speaker 3: plane of the Milky Way as the zone of avoidance,
[6:24] Speaker 3: the zone of avoidance.
[6:25] Speaker 2: That sounds like a sci fi movie title.
[6:27] Speaker 3: It does, but it's a real technical term. For decades,
[6:30] Speaker 3: if you pointed a telescope in that direction, the dust
[6:32] Speaker 3: extinction was so severe that the distant extragalactic universe was
[6:36] Speaker 3: completely rendered invisible. You simply couldn't see past our own
[6:39] Speaker 3: local neighborhood.
[6:40] Speaker 2: So let me make sure I have this right. The
[6:42] Speaker 2: seventy five percent of the sky mapped in this five
[6:45] Speaker 2: point six trillion pixel image represents the site lines where
[6:49] Speaker 2: we can look up out of the galactic disk or
[6:51] Speaker 2: down out of it, deliberately avoiding the dense, dusty equator
[6:55] Speaker 2: of the Milky Way.
[6:56] Speaker 3: Precisely by pointing our instruments percindicular to the galactic plane,
[7:00] Speaker 3: we bypass the thickest concentrations of dust. The map surveys
[7:05] Speaker 3: the specific clear regions of the sky in both visible
[7:08] Speaker 3: and near infrared.
[7:09] Speaker 2: Light, because the goal wasn't to map the Milky Way exactly.
[7:12] Speaker 3: The objective of the Legacy surveys was never to map
[7:15] Speaker 3: our own galaxy. It was to achieve the deepest, most
[7:18] Speaker 3: unobstructed view of the extra galactic universe beyond our borders.
[7:22] Speaker 3: When you navigate this map, you are essentially looking past
[7:25] Speaker 3: the scattered foreground stars of our galaxy and plunging directly
[7:29] Speaker 3: into the deep ocean of the ancient universe.
[7:32] Speaker 2: And the landmarks in that deep ocean are just they're staggering.
[7:35] Speaker 2: I want a panamental picture for you listening, because this
[7:38] Speaker 2: specific galactic structures captured in this map really defy simple description.
[7:42] Speaker 3: They are incredibly beautiful.
[7:44] Speaker 2: One of the highlights the survey team isolated yesterday is
[7:47] Speaker 2: Messy A ninety six. It's this massive intermediate spiral galaxy
[7:51] Speaker 2: located in the constellation Leo, and the resolution of this
[7:54] Speaker 2: two D map captures it with such terrifying clarity.
[7:57] Speaker 3: You can see the sweeping, highly asymmetrical spiral.
[8:01] Speaker 2: Arms, yeah, and the intensely bright active galactic nucleus in
[8:04] Speaker 2: the center, and these intricate dark tendrils of cosmic dust
[8:08] Speaker 2: woven through the outer disk. It's breath taking. But the
[8:12] Speaker 2: detail that gives me absolute pause is the distance. Messia
[8:15] Speaker 2: ninety six is situated approximately thirty five million light years
[8:18] Speaker 2: away from.
[8:19] Speaker 3: Earth, and the conceptual leap required to understand that distance
[8:22] Speaker 3: is essentially a loop in understanding the physical nature of
[8:25] Speaker 3: time itself.
[8:25] Speaker 2: Because it's not instantaneous right.
[8:27] Speaker 3: Because light travels at a finite measurable speed roughly one
[8:30] Speaker 3: hundred and eighty six thousand miles per second. Astronomy is
[8:33] Speaker 3: fundamentally the study of the past. When you look at
[8:36] Speaker 3: Messia ninety six. In this map, you are not seeing
[8:38] Speaker 3: the galaxy as it exists on August eleventh, twenty twenty six.
[8:42] Speaker 3: You are interacting with ancient history.
[8:44] Speaker 2: We are looking at a snapshot taken thirty five million
[8:46] Speaker 2: years ago. So the photons hitting the telescope sensor physically
[8:50] Speaker 2: left that galaxy before human beings even existed.
[8:53] Speaker 3: Think about the physical journey of those photons. Thirty five
[8:56] Speaker 3: million years ago. Earth was in the late Eocene.
[9:00] Speaker 2: Epoch, the Eocene epoch.
[9:01] Speaker 3: Wow, Yeah, the supercontinents had broken apart, but the globe
[9:05] Speaker 3: looked vastly different than it does today. Antarctica was just
[9:09] Speaker 3: beginning to develop its first permanent ice sheets.
[9:12] Speaker 2: So no ice on Antarctica yet, basically.
[9:14] Speaker 3: Just starting, and the earliest primitive ancestors of modern mammals
[9:19] Speaker 3: were just establishing their presence now at that precise geological
[9:24] Speaker 3: moment on Earth, deep inside the glowing core of Messia
[9:27] Speaker 3: ninety six, a star underwent nuclear fusion and emitted photons
[9:31] Speaker 3: of light.
[9:31] Speaker 2: And those photons just started flying outward.
[9:34] Speaker 3: They escaped the gravitational pull of their host star. They
[9:37] Speaker 3: navigated out of the spiral arms of Messia ninety six,
[9:40] Speaker 3: and they entered the freezing, near perfect vacuum of intergalactic.
[9:43] Speaker 2: Space, and then they just kept going.
[9:45] Speaker 3: For thirty five million years. Those individual packets of light
[9:48] Speaker 3: traveled across the void completely uninterrupted. They dodged rogue planets,
[9:52] Speaker 3: they navigated the gravitational warping of dark matter halos, and
[9:55] Speaker 3: survived the immense silent stretches between galaxies.
[9:58] Speaker 2: Well you know, entire speed. She rose and went extinct
[10:01] Speaker 2: back here on Earth exactly.
[10:03] Speaker 3: And finally, after a thirty five million year, unfathomably lonely journey,
[10:08] Speaker 3: they crossed into our solar system, penetrated the Earth's atmosphere,
[10:12] Speaker 3: and ended their existence by striking a digital CCD sensor
[10:17] Speaker 3: on a telescope in the mountains.
[10:18] Speaker 2: Of Chile, triggering a microscopic electrical charge that became a
[10:22] Speaker 2: single pixel in this map. Yes, when you frame it
[10:25] Speaker 2: like that, looking at a galaxy isn't just data collection.
[10:28] Speaker 2: It's a literal physical intersection with deep time it is,
[10:32] Speaker 2: and Messia ninety six is just one object out of
[10:35] Speaker 2: four billion. I mean, the map is crowded with these
[10:37] Speaker 2: ancient structures. Take the Copeland septet, which is also featured
[10:40] Speaker 2: prominently in the release. It's this tight, chaotic visual cluster
[10:44] Speaker 2: of galaxies again in the constellation.
[10:46] Speaker 3: Leo and in the map. When you look at that cluster,
[10:48] Speaker 3: you aren't just seeing static shapes.
[10:50] Speaker 2: No, you are looking at a gravitational war. These massive
[10:54] Speaker 2: galaxies are actively dancing with one another, their immense gravitational fields,
[10:57] Speaker 2: pulling and stretching each other, tearing off massive title tales
[11:00] Speaker 2: of stars.
[11:01] Speaker 3: You are viewing a snapshot of structural violence playing out
[11:05] Speaker 3: over millions of years.
[11:07] Speaker 2: And the most incredible aspect of this entire endeavor is
[11:11] Speaker 2: the accessibility. This isn't classified data locked behind some biometric
[11:16] Speaker 2: vault at a defense agency, right.
[11:18] Speaker 3: No, not at all. And the democratization of this massive
[11:21] Speaker 3: data set is arguably as significant as the technological achievement itself.
[11:26] Speaker 3: Oh so well, the astrophysics community has increasingly recognized that
[11:30] Speaker 3: hoarding data restricts discovery. The entire five point six trillion
[11:34] Speaker 3: pixel map is fully public right now today, integrated into
[11:38] Speaker 3: an interface called the Legacy Survey.
[11:40] Speaker 2: Sky Viewer David Schlegel, who's one of the co leads
[11:43] Speaker 2: of the Legacy Surveys out of the Berkeley Lab, made
[11:45] Speaker 2: a comment yesterday that really stuck with me. He noted,
[11:47] Speaker 2: that this map is no longer just a project. It
[11:50] Speaker 2: has become quote part of the fabric of astronomy.
[11:52] Speaker 3: Research, which is entirely accurate.
[11:54] Speaker 2: It's basically the foundational operating system for astronomers. Now, if
[11:57] Speaker 2: you're researching extra galactic phenomena, your very first step is
[12:01] Speaker 2: opening the sky Viewer to establish your coordinates. It functions
[12:05] Speaker 2: like a hyperadvanced Google Earth, but build for the observable universe.
[12:09] Speaker 3: The ethos behind this was perfectly articulated by Argent Day,
[12:13] Speaker 3: an astronomer at the NSF Nor Lab and another co
[12:18] Speaker 3: lead on the project. He stated, quite simply, the skies
[12:22] Speaker 3: belong to everyone.
[12:23] Speaker 2: The skies belong to everyone.
[12:25] Speaker 3: I love that the interface is specifically designed so that
[12:28] Speaker 3: anyone with an Internet connection can interrogate the data.
[12:31] Speaker 2: So this means you listening to this right now can
[12:34] Speaker 2: literally open your laptop, pull up the sky Viewer, and
[12:38] Speaker 2: actively pan through thirty five million years of deep space history.
[12:43] Speaker 2: And because there are four billion objects in this map,
[12:46] Speaker 2: the statistical probability is actually very high that you could
[12:49] Speaker 2: zoom into a sector and be the first human being
[12:51] Speaker 2: in history to lay eyes on a specific distant galaxy.
[12:54] Speaker 3: That happens quite frequently.
[12:56] Speaker 2: Actually, there is a massive active community of citizen scientists
[12:59] Speaker 2: using the exact data set to hunt for transient phenomena.
[13:03] Speaker 2: They're manually scrubbing through regions looking for fleeting supernovae, you
[13:07] Speaker 2: know those stars that undergo catastrophic collapse and explode, appearing
[13:11] Speaker 2: brightly for a brief window before fading.
[13:13] Speaker 3: Or they're hunting for rare gravitational.
[13:15] Speaker 2: Lenses right where a massive four ground object literally warps
[13:19] Speaker 2: the fabric of space, time bending and magnifying the light
[13:23] Speaker 2: of an entirely different galaxy hidden far behind it. You
[13:26] Speaker 2: can literally participate in cutting edge astrophysics from your couch
[13:30] Speaker 2: in your living room.
[13:31] Speaker 3: But while the public access is beautifully seamless, the interface
[13:35] Speaker 3: heavily masks the brutal complexity of the maps creation. Navigating
[13:39] Speaker 3: the data is easy to understand the engineering challenge here.
[13:43] Speaker 3: You really have to discard the notion of a photograph entirely.
[13:46] Speaker 3: This map is a composite mathematical construction.
[13:49] Speaker 2: I explained that the.
[13:49] Speaker 3: Final image is the culmination of two hundred and six
[13:52] Speaker 3: three thousand, four hundred and seven individual highly calibrated telescope
[13:57] Speaker 3: exposures over a quarter.
[13:59] Speaker 2: Of a million in separate observations.
[14:01] Speaker 3: Let that sink in unmasked over two two hundred and
[14:04] Speaker 3: eighty five distinct nights of observation. Wow, that represents thousands
[14:08] Speaker 3: of nights where operators sat in freezing control rooms on
[14:11] Speaker 3: high altitude mountain peaks, monitoring minute fluctuations and atmospheric pressure
[14:16] Speaker 3: and humidity, just waiting for the elusive pockets of perfect
[14:19] Speaker 3: visual clarity known as good scene conditions.
[14:22] Speaker 2: And this wasn't just a single telescope slowly scaling the
[14:25] Speaker 2: sky over those two two hundred and eighty five nights, either.
[14:28] Speaker 2: The data was stitched together from three massive, distinct ground
[14:32] Speaker 2: based astronomical surveys.
[14:34] Speaker 3: Right correct, to cover the entire mapped area, you need
[14:37] Speaker 3: multiple vantage points on Earth.
[14:39] Speaker 2: So in the southern hemisphere you had the DECAL Survey
[14:41] Speaker 2: operating out of Chile. They utilized the Victor M. Blanco
[14:46] Speaker 2: four meter telescope which was outfitted with the Dark Energy Camera,
[14:50] Speaker 2: which is this five hundred and seventy megapixel sensor specifically
[14:54] Speaker 2: fabricated by the Department of Energy for this exact kind
[14:58] Speaker 2: of wide field.
[14:58] Speaker 3: Mapping right the southern sky.
[15:01] Speaker 2: Then to cover the northern sky, they ran the MZLS
[15:03] Speaker 2: Survey out of the kitt Peak National Observatory and the
[15:06] Speaker 2: base survey at the Stewart Observatory in Arizona. And as
[15:10] Speaker 2: if harmonizing three different ground based observatories wasn't complex enough,
[15:15] Speaker 2: they integrated years of space based data from NASA's Y's satellite.
[15:19] Speaker 3: And integrating the y satellite data was an absolute necessity
[15:23] Speaker 3: for structural mapping.
[15:25] Speaker 2: Why why weren't the ground telescopes enough?
[15:27] Speaker 3: Ground based optical telescopes are phenomenal, but they are inherently
[15:31] Speaker 3: limited by the Earth's atmosphere, which actively absorbs and blocks
[15:34] Speaker 3: vast portions of the electromagnetic spectrum, particularly infrared.
[15:38] Speaker 2: Light right the atmosphere Ecxica filter.
[15:39] Speaker 3: Furthermore, visible light struggles to penetrate the massive clouds of
[15:42] Speaker 3: cosmic dust we discussed.
[15:44] Speaker 2: Earlier the dirty window.
[15:45] Speaker 3: Exactly by layering the space based infrared data from WHYS,
[15:50] Speaker 3: the map can reveal the thermal signatures of deeply dust
[15:53] Speaker 3: and shrouded galaxies, active black holes, and ancient, highly red
[15:58] Speaker 3: shifted stars that are completely invisible in standard optical wavelength.
[16:03] Speaker 2: Okay, let's talk about the stitching process, because this is
[16:06] Speaker 2: where my mind hits an absolute wall. If I'd take
[16:09] Speaker 2: my smartphone to the edge of the Grand Canyon. To
[16:12] Speaker 2: shoot a panorama, I slowly pan the camera from left
[16:15] Speaker 2: to right, and.
[16:16] Speaker 3: We all know how that usually goes.
[16:18] Speaker 2: Right. The internal processor and software desperately try to match
[16:21] Speaker 2: the edges of the frames and stitch them together into
[16:24] Speaker 2: a wide shot. But if a bird flies through the
[16:27] Speaker 2: frame or my hand shakes even a little bit, the
[16:29] Speaker 2: parallax effect completely ruins the image.
[16:31] Speaker 3: Yeah, the software gets confused by the depth exactly.
[16:33] Speaker 2: And you end up with a photograph where a mountain
[16:35] Speaker 2: looks digitally sheared in half, where the sky is jaggedly pixelated.
[16:40] Speaker 2: It's incredibly fragile technology on a phone.
[16:42] Speaker 3: The parallax effect and the limitations of consumer gyroscopes make
[16:45] Speaker 3: seamless panoramic photography on Earth notoriously difficult.
[16:49] Speaker 2: So how on Earth do you avoid that? When your
[16:50] Speaker 2: panorama consists of two hundred and sixty three four hundred
[16:54] Speaker 2: and seven photos, and you didn't just pan a single
[16:56] Speaker 2: camera from one spot. You took some photos in the
[16:59] Speaker 2: Andes Mountains, some in the Arizona Desert, and some from
[17:02] Speaker 2: a satellite hurtling through a low earth orbit.
[17:04] Speaker 3: All operating under totally different conditions.
[17:06] Speaker 2: Yes, these exposures were captured years apart. During some observations,
[17:11] Speaker 2: the moon was full, flooding the sky with ambient light.
[17:15] Speaker 2: During others, it was pitch black. Atmospheric turbulence varied wildly
[17:19] Speaker 2: from night to night. How do you align a quarter
[17:22] Speaker 2: million desperate exposures into a unified, flat, five point six
[17:27] Speaker 2: trillion pixel map without creating a distorted, misaligned, funhouse mirror
[17:32] Speaker 2: version of the universe.
[17:33] Speaker 3: You cannot rely on physical sensors like gyroscopes to track
[17:36] Speaker 3: the camera's position. In modern astrophysics, alignment relies entirely on
[17:39] Speaker 3: celestial reference frames and immensely complex algorithms.
[17:43] Speaker 2: Oh, okay, break that down for me.
[17:44] Speaker 3: The fundamental challenge you were highlighting is why modern astronomy
[17:47] Speaker 3: has evolved into a highly specialized branch of computer science.
[17:50] Speaker 3: We no longer primarily observe the universe. We compute it.
[17:53] Speaker 2: The computational bottleneck. Tell me how the algorithm actually takes
[17:57] Speaker 2: a blurry photo from Arizona and a sharp photo from
[18:00] Speaker 2: Chile and forces them to agree on the precise location
[18:04] Speaker 2: of a star.
[18:04] Speaker 3: So the software must account for something called the point
[18:07] Speaker 3: spread function or PSF.
[18:08] Speaker 2: Point spread function.
[18:09] Speaker 3: Okay, Because of the Earth's atmosphere, a perfectly sharp point
[18:12] Speaker 3: of starlight gets smeared and blurred by the time it
[18:15] Speaker 3: hits the telescope sensor. This smearing changes every millisecond based
[18:19] Speaker 3: on temperature and wind.
[18:21] Speaker 2: The atmosphere is basically constantly boiling above the telescope exactly.
[18:24] Speaker 3: So the algorithms written for this map have to mathematically
[18:27] Speaker 3: analyze every single star in every single exposure, calculate the
[18:32] Speaker 3: exact nature of the atmospheric blurring for that specific microsecond,
[18:35] Speaker 3: and then run complex deconvolution matrixes to reverse engineer the
[18:40] Speaker 3: true sharp position of the light source.
[18:42] Speaker 2: Wait, so the software isn't just overlapping images. It is
[18:45] Speaker 2: actively mathematically repairing the atmospheric distortion in millions of stars simultaneously.
[18:52] Speaker 3: Yes, but it goes further than that. The software must
[18:54] Speaker 3: also differentiate between a genuine cosmic object and a transient error,
[18:59] Speaker 3: Like what kind of error? While high altitude sensors are
[19:02] Speaker 3: constantly bombarded by cosmic rays, these are high energy particles
[19:06] Speaker 3: that strike the silicon and register as a bright pixel
[19:09] Speaker 3: on the image.
[19:10] Speaker 2: Oh so it looks like a star, but it's just
[19:12] Speaker 2: a particle hitting.
[19:12] Speaker 3: The camera exactly, So the algorithm must compare multiple exposures
[19:17] Speaker 3: of the same patch of sky, identify the pixels that
[19:20] Speaker 3: only appear in one frame, classify them as cosmic ray
[19:23] Speaker 3: strikes or passing satellite streaks, and digitally excize them from
[19:27] Speaker 3: the final composite.
[19:28] Speaker 2: That sounds like an insane amount of data processing it is.
[19:31] Speaker 3: Writing the custom software architecture capable of performing these millions
[19:35] Speaker 3: of simultaneous calculations took the development team an entire year.
[19:40] Speaker 2: A full year of just coding the logic before they
[19:43] Speaker 2: could even attempt to render.
[19:44] Speaker 3: The actual map, And when the code was finally optimized,
[19:47] Speaker 3: it required a hardware environment far beyond standard high performance
[19:50] Speaker 3: computing clusters.
[19:51] Speaker 2: You can't just run this on a MacBook, No, they had.
[19:55] Speaker 3: To deploy this architecture on the Pearl Mutter supercomputer housed
[19:59] Speaker 3: at the National Energy Research Scientific Computing Center or NERSC
[20:04] Speaker 3: at the Berkeley Lab. Pearlmutter is explicitly designed for extreme
[20:08] Speaker 3: scale scientific computing, and.
[20:10] Speaker 2: Even with millions of processing cores operating in parallel chewing
[20:14] Speaker 2: through petabytes of raw observational data, the rendering process was
[20:18] Speaker 2: not instantaneous, right far from it. It took eight grueling,
[20:22] Speaker 2: continuous weeks of supercomputing time just to process the math
[20:26] Speaker 2: and synthesize the final five point six trillion pixel image.
[20:31] Speaker 2: I read that if a standard high end commercial laptop
[20:34] Speaker 2: attempted to run those calculations, it would take centuries of
[20:37] Speaker 2: constant processing.
[20:38] Speaker 3: The scale of the computation reflects the scale of the ambition.
[20:42] Speaker 3: But you know, it is frugial to understand that rendering
[20:44] Speaker 3: this beautiful two D map was never the ultimate goal.
[20:46] Speaker 2: It wasn't.
[20:47] Speaker 3: No, the legacy imaging surveys did not commandeer years of
[20:50] Speaker 3: supercomputing time just to produce a static visual catalog for
[20:53] Speaker 3: people to look at. This two D image is functionally
[20:55] Speaker 3: a stepping stone, okay to what it is, the highly
[20:59] Speaker 3: calibrated foundational blueprint for a three D structural model of
[21:02] Speaker 3: the universe designed to interrogate the most dominant invisible forces
[21:07] Speaker 3: in nature.
[21:07] Speaker 2: Oh wow, okay, this transitions us perfectly from the map
[21:10] Speaker 2: itself to the actual reason the map exists. We need
[21:13] Speaker 2: to talk about DSi because if you want to understand
[21:16] Speaker 2: why astrophysicists are currently questioning the long term fate of
[21:19] Speaker 2: the universe, you have to understand the interplay between this
[21:22] Speaker 2: newly released two D map and the dark energy spectroscopic
[21:26] Speaker 2: instrument right.
[21:26] Speaker 3: Exactly, the legacy imaging surveys were commissioned and executed specifically
[21:31] Speaker 3: to provide the targeting data for d SI.
[21:34] Speaker 2: To make this concrete for the listener, let's look at
[21:36] Speaker 2: the limitations of the five point six trillion pixel map.
[21:40] Speaker 2: As detailed and as massive as it is, it is
[21:42] Speaker 2: ultimately a flat two dimensional projection.
[21:45] Speaker 3: Right. It has no depth.
[21:46] Speaker 2: It provides exact X and y celestial coordinates, and it
[21:50] Speaker 2: provides precise photometric brightness. But a two D photograph suffers
[21:54] Speaker 2: from a fundamental astronomical ambiguity. It cannot inherently tell you distance.
[21:59] Speaker 3: You lose the Z access entirely.
[22:01] Speaker 2: Exactly. If I look at the map and see a
[22:04] Speaker 2: small dim smudge of a galaxy, and right next to
[22:07] Speaker 2: it I see a massive bright galaxy, I cannot automatically
[22:11] Speaker 2: assume the dim one is physically smaller.
[22:13] Speaker 3: Right, The dim galaxy might be relatively close to Earth
[22:16] Speaker 3: but objectively tiny, while the massive bright galaxy might be
[22:20] Speaker 3: an absolute behemoth located billions of late years further away.
[22:23] Speaker 2: In a flat image, depth is collapsed.
[22:26] Speaker 3: The two D map is an exquisite, comprehensive catalog of
[22:29] Speaker 3: where objects appear in the sky, but it lacks that
[22:32] Speaker 3: crucial Z axis. It is essentially the menu from which
[22:36] Speaker 3: d SI selects its targets.
[22:37] Speaker 2: So how does DSi extract that Z axis? How does
[22:40] Speaker 2: it take this flat map of four billion objects and
[22:43] Speaker 2: begin assigning them a physical depth in a three D model?
[22:45] Speaker 3: DSY utilizes the exact coordinates provided by the two D
[22:49] Speaker 3: map to aim its instrument. But DSi doesn't take photographs.
[22:52] Speaker 3: It is a spectrograph.
[22:53] Speaker 2: A spectrograph, okay, how does that work?
[22:55] Speaker 3: It uses thousands of robotic positioners to point microscopic optical
[22:59] Speaker 3: fibers at specific targeted galaxies identified in the map. Once
[23:04] Speaker 3: locked on, DSi collects a light from that specific galaxy
[23:07] Speaker 3: and fractures it into a highly detailed spectrum basically a
[23:11] Speaker 3: rainbow of its constituent wavelength.
[23:13] Speaker 2: And hidden within that spectrum are the chemical fingerprints of
[23:16] Speaker 2: the galaxy.
[23:16] Speaker 3: Specifically, DSi is looking for emission and absorption lines because,
[23:21] Speaker 3: as we know, the universe is expanding, which means the
[23:25] Speaker 3: fabric of space time itself is stretching. Right as the
[23:28] Speaker 3: light from a distant galaxy travels toward Earth, the physical
[23:31] Speaker 3: expansion of the universe stretches the wavelength of that light,
[23:35] Speaker 3: shifting it toward the red end of the electromagnetic spectrum.
[23:38] Speaker 3: This is known as cosmological redshift.
[23:40] Speaker 2: So wait, it is just the Doppler effect, like a
[23:42] Speaker 2: police siren changing pitch as it dries past you on
[23:45] Speaker 2: the highway.
[23:46] Speaker 3: Not exactly. The galaxy isn't merely moving through space. The
[23:49] Speaker 3: space between us and the galaxy is actually expanding, stretching
[23:52] Speaker 3: the photon's wave while it's in transit.
[23:55] Speaker 2: Okay, that distinction is vital.
[23:56] Speaker 3: By precisely measuring how far those spectral lines have been
[24:00] Speaker 3: shifted toward the red, DSi can calculate exactly how much
[24:03] Speaker 3: the universe has expanded since that light was originally emitted.
[24:07] Speaker 2: And because we know the rate of expansion, the red
[24:10] Speaker 2: shift measurement gives us an exact, highly precise distance to
[24:13] Speaker 2: that galaxy exactly.
[24:15] Speaker 3: DSi combines its precise depth measurements with the x and
[24:19] Speaker 3: y coordinates of the two D map to build a sprawling,
[24:22] Speaker 3: immensely detailed three D topographic map of the cosmos.
[24:26] Speaker 2: But the ultimate purpose of plotting millions of galaxies in
[24:29] Speaker 2: three D isn't just to know where they are. It's
[24:31] Speaker 2: to trace the massive invisible scaffolding that governs their movement.
[24:36] Speaker 2: We are hunting dark matter and dark energy. Here.
[24:38] Speaker 3: The structure of the universe is dictated by a cosmic
[24:40] Speaker 3: tug of war between these two invisible dominators.
[24:43] Speaker 2: Okay, let's break down the teams in this tug of war.
[24:46] Speaker 2: Dark matter first.
[24:48] Speaker 3: Dark matter acts as the gravitational glue. It exerts a
[24:51] Speaker 3: powerful attractive force. It is the underlying mass that forms
[24:54] Speaker 3: the immense cosmic web, pulling regular baryonic matter together to
[24:58] Speaker 3: form galaxies and cluster those galaxies into massive superstructures.
[25:02] Speaker 2: So if dark matter were removed, what would happen.
[25:05] Speaker 3: The rotational velocity of galaxies would cause them to instantly
[25:08] Speaker 3: fly apart. There isn't enough visible matter to hold them together.
[25:12] Speaker 2: Wow. Okay, so dark matter pulls in, but we know
[25:15] Speaker 2: the universe is currently expanding, meaning something else is pushing
[25:19] Speaker 2: back and that something else is winning.
[25:21] Speaker 3: Dark energy is the opposing force. It acts as a
[25:24] Speaker 3: repulsive pressure inherent to the vacuum of space itself, driving
[25:28] Speaker 3: the accelerated expansion of the.
[25:29] Speaker 2: Universe, and DSi is measuring this Yes.
[25:32] Speaker 3: By analyzing the three D distribution of galaxies over vast
[25:35] Speaker 3: cosmic time scales, scientists can study baryon acoustic oscillations.
[25:40] Speaker 2: Baryon acoustic oscillations, Yeah, it's a mouthful. What are those?
[25:43] Speaker 3: There are essentially frozen sound waves from the early universe
[25:46] Speaker 3: that dictate how galaxies cluster together today. By measuring the
[25:49] Speaker 3: exact distances between these clusters at different epochs in the
[25:53] Speaker 3: universe's history, we can precisely chart the behavior of dark
[25:56] Speaker 3: energy over time.
[25:57] Speaker 2: Which brings us directly to the absolute bombshell discovery that
[26:01] Speaker 2: is actively rocking the physics world right now.
[26:03] Speaker 3: Yes, the early DSi results.
[26:06] Speaker 2: DSi was initially utilizing an older, smaller iteration of this
[26:10] Speaker 2: two D map to select its targets, and the instrument
[26:14] Speaker 2: proved so incredibly efficient at mapping the Z axis that
[26:17] Speaker 2: it burned through its initial target list way faster than expected.
[26:21] Speaker 3: It completed its primary five year survey ahead of schedule
[26:24] Speaker 3: in April of twenty twenty six.
[26:26] Speaker 2: They literally ran out of galaxies to measure. They desperately
[26:29] Speaker 2: needed the expanded boundaries of this new five point six
[26:32] Speaker 2: trillion pixel map to continue the hunt, and the day
[26:35] Speaker 2: SI team actually began quietly utilizing this new data behind
[26:38] Speaker 2: the scenes in June of twenty twenty six to select
[26:41] Speaker 2: fresh targets.
[26:42] Speaker 3: The influx of new targets from this expanded map was
[26:45] Speaker 3: critical because the initial data crunch from day SI's first
[26:48] Speaker 3: years of operation revealed something deeply, deeply unsettling about the
[26:52] Speaker 3: nature of dark energy.
[26:53] Speaker 2: Let's clarify why this is so unsettling. For essentially my
[26:57] Speaker 2: entire life, and for decades of established cosmogical fear, dark
[27:01] Speaker 2: energy was assumed to be a cosmological constant.
[27:03] Speaker 3: It was a fixed rule of the universe.
[27:05] Speaker 2: When Albert Einstein formulated general relativity, he introduced the cosmological constant,
[27:11] Speaker 2: represented by the Greek letter Lambda, to basically balance his equations.
[27:15] Speaker 2: In the modern consensus model, which is known as Lambda's CDM,
[27:19] Speaker 2: dark energy is a constant, unchanging property of space.
[27:22] Speaker 3: Meaning as the universe expands and creates more space, the
[27:26] Speaker 3: density of dark energy remains exactly the same.
[27:28] Speaker 2: It applies a constant uniform outward pressure, causing the universe
[27:32] Speaker 2: to expand faster and faster into eternity. But the early
[27:36] Speaker 2: results from the DSi data are actively defying this model.
[27:39] Speaker 2: The clustering of the galaxies suggests that the impact of
[27:42] Speaker 2: dark energy is not constant.
[27:44] Speaker 3: It is showing significant hints of weakening over time weakening. Yes,
[27:48] Speaker 3: the implications of dynamic dark energy cannot be overstated. If
[27:52] Speaker 3: dark energy is weakening, if its density or its repulsive
[27:54] Speaker 3: force changes as the universe ages, that Einstein's cosmological constant
[27:59] Speaker 3: is fundamentally incorrect. That is massive, we would be forced
[28:03] Speaker 3: to abandon the land of CDM model entirely and adopt
[28:06] Speaker 3: entirely new theoretical frameworks, such as quintessence, which posits dark
[28:11] Speaker 3: energy as a dynamic evolving scaler field rather than a
[28:15] Speaker 3: static property of the vacuum.
[28:17] Speaker 2: But wait, I need to push back on the actual
[28:18] Speaker 2: millionnix of this for a second. If dark energy is
[28:22] Speaker 2: the physical pressure causing the expansion of the universe to accelerate,
[28:26] Speaker 2: and that pressure is running out of gas and weakening,
[28:29] Speaker 2: what happens to the physical.
[28:31] Speaker 3: Expansion, Well, it changes everything about our future.
[28:34] Speaker 2: If I'm pressing the accelerator on a car and I
[28:36] Speaker 2: slowly lift my foot, the car doesn't stop immediately, but
[28:39] Speaker 2: the acceleration drops. If dark energy weakens enough, does the
[28:43] Speaker 2: expansion of the universe just coast to a halt? Does
[28:46] Speaker 2: it reverse?
[28:47] Speaker 3: You are outlining the exact existential scenarios currently being fiercely
[28:51] Speaker 3: debated by theoretical physicists.
[28:53] Speaker 2: Right now, let's talk about the traditional scenario first.
[28:55] Speaker 3: Under the traditional model, where dark energy remains a constant,
[28:58] Speaker 3: relentless force, the fate of the universe is locked into
[29:02] Speaker 3: a scenario known as the Big Freeze.
[29:04] Speaker 2: Or heat death the Big Freeze.
[29:06] Speaker 3: The expansion continues accelerating infinitely. Galaxies drift so far apart
[29:11] Speaker 3: that they can no longer be seen from one another.
[29:14] Speaker 3: The stars burn through their fuel and die. The remaining
[29:17] Speaker 3: matter decays, and the universe becomes an endlessly expanding, dark,
[29:22] Speaker 3: freezing void approaching absolute zero.
[29:25] Speaker 2: An infinitely lonely frozen eternity. Not a great way to
[29:29] Speaker 2: go out.
[29:30] Speaker 3: No, it's quite bleak. However, if the d side data
[29:33] Speaker 3: holds true and dark energy is dynamically weakening, that fate
[29:36] Speaker 3: is completely rewritten. Okay, how So, if the repulsive force
[29:40] Speaker 3: of dark energy diminishes enough over cosmic time, the outward
[29:43] Speaker 3: expansion of the universe will inevitably slow down. The critical
[29:47] Speaker 3: threshold occurs if dark energy weakens to the point where
[29:49] Speaker 3: it is finally overpowered by the collective gravitational pull of
[29:53] Speaker 3: the dark matter scaffolding.
[29:54] Speaker 2: The moment gravity wins the tug of war exactly.
[29:57] Speaker 3: If gravity becomes the dominant force once again, the expansion
[30:00] Speaker 3: of the universe stops and it begins to contract. This
[30:02] Speaker 3: leads to the big Crunch scenario.
[30:05] Speaker 2: Big crunch, so everything comes rushing back together.
[30:07] Speaker 3: Yes, billions of years from now, galaxies would begin rushing
[30:12] Speaker 3: toward each other. The ambient temperature of the universe would
[30:15] Speaker 3: violently rise as all matter and radiation are compressed into
[30:19] Speaker 3: a smaller and smaller volume, eventually collapsing back into a
[30:22] Speaker 3: state of infinite.
[30:23] Speaker 4: Density, basically a reversal of the Big Bang. Precisely, the
[30:26] Speaker 4: fact that this five point six trillion pixel map, which
[30:29] Speaker 4: was officially released to the public yesterday, is the primary
[30:32] Speaker 4: instrument dictating whether our universe freezes into infinite nothingness or
[30:37] Speaker 4: collapses into a catastrophic singularity, is genuinely difficult to process.
[30:42] Speaker 3: It's happy, for sure, and we.
[30:43] Speaker 2: Won't even have to wait decades for an answer. DSi
[30:47] Speaker 2: is scheduled to publish a highly refined analysis of its
[30:49] Speaker 2: first five years of data in twenty twenty seven, and
[30:52] Speaker 2: it will aggressively continue observations using this new two D
[30:55] Speaker 2: map well into twenty twenty eight. We are sitting on
[30:58] Speaker 2: the precipice of a complete paradise shift in physics.
[31:01] Speaker 3: The immediacy of these discoveries is thrilling, But the utility
[31:04] Speaker 3: of this map extends far beyond just the DSi project.
[31:07] Speaker 2: Really, how much more can we get out of this data.
[31:09] Speaker 3: Legacy Surveys team has fundamentally constructed an infrastructural asset that
[31:14] Speaker 3: will anchor observational astronomy for the next fifty years.
[31:18] Speaker 2: Oh, we are talking about the technological foundation for the
[31:21] Speaker 2: next generation of massive observatories exactly. We are currently building phenomenal,
[31:26] Speaker 2: multi billion dollar machines like the NSF Doe Veric Reuben
[31:30] Speaker 2: Observatory in Chile and NASA's Nancy Grace Roman Space Telescope.
[31:36] Speaker 2: The capabilities of these new instruments are just unprecedented.
[31:39] Speaker 3: They are the absolute pinnacle of human engineering.
[31:42] Speaker 2: But to use an analogy, building these massive telescopes is
[31:45] Speaker 2: sort of like engineering a hyper advanced sniper rifle. It
[31:49] Speaker 2: has incredible range and terrifying precision, But if you look
[31:52] Speaker 2: through the high powered scope, your field of view is
[31:54] Speaker 2: incredibly narrow.
[31:55] Speaker 3: Right, you can only see a tiny sliver of the sky.
[31:58] Speaker 2: You can see a microscopic patch of the horizon in
[32:01] Speaker 2: incredible detail, but you have zero situational awareness. You can't
[32:05] Speaker 2: just blindly sweep a sniperscope across the sky hoping to
[32:08] Speaker 2: find a specific target. You need a wide angle drone feed,
[32:12] Speaker 2: a highly detailed map of the entire battlefield to tell
[32:15] Speaker 2: you the exact coordinates of where to aim the rifle.
[32:18] Speaker 3: And that is exactly what this map provides. The two
[32:21] Speaker 3: D map is that comprehensive wide angle feed. Because telescope
[32:25] Speaker 3: time on the Reuben Observatory or the Roman Space Telescope
[32:29] Speaker 3: will be incredibly expensive and highly contested among scientists worldwide,
[32:33] Speaker 3: efficiency is paramount.
[32:35] Speaker 2: They can't waste time looking in the wrong place.
[32:37] Speaker 3: They cannot waste hours blindly scanning. When these next generation
[32:41] Speaker 3: observatories achieve first light, their targeting algorithms will pull directly
[32:45] Speaker 3: from the five point six trillion pixel map to execute
[32:49] Speaker 3: their deep field observations.
[32:50] Speaker 2: And it isn't just human astronomers writing grant proposals who
[32:54] Speaker 2: will rely on this data. The map is actively training
[32:57] Speaker 2: the non human intelligence that will dictate the future of discs.
[33:00] Speaker 3: This is a huge shift in the field.
[33:02] Speaker 2: We are crossing the threshold into an era where AI
[33:05] Speaker 2: fundamentally drives astrophysics.
[33:07] Speaker 3: Because the volume of data has simply surpassed human biological limits.
[33:11] Speaker 3: When you have a unified image containing four billion objects,
[33:14] Speaker 3: human review is mathematically impossible.
[33:17] Speaker 2: You could have a million grad students staring at screens
[33:19] Speaker 2: and they wouldn't finish it exactly.
[33:21] Speaker 3: This is why the maps data has immediately been integrated
[33:23] Speaker 3: into a massive astrophysics pilot project within the American Science
[33:27] Speaker 3: Cloud operating under the Department of Energy's Genesis mission.
[33:31] Speaker 2: So the objective isn't to have an AI just counter galaxies, right.
[33:36] Speaker 2: They are feeding this petabyte scale map into massive neural
[33:41] Speaker 2: networks to teach the AI the fundamental visual and structural
[33:46] Speaker 2: rules of the universe.
[33:47] Speaker 3: The neural network analyzes the millions of variations of spiral arms,
[33:51] Speaker 3: the typical thermal decay of cosmic dust, the standard luminosity
[33:55] Speaker 3: gradients of elliptical.
[33:56] Speaker 2: Galaxies, basically learning what normal looks like.
[33:58] Speaker 3: By ingestin trillions of pixels of standard cosmic behavior, the
[34:02] Speaker 3: AI establishes a rigorous mathematical baseline for what normal physics
[34:06] Speaker 3: looks like. And in astronomy, discovery does not come from
[34:09] Speaker 3: observing the normal, it comes from isolating the anomalis AH.
[34:13] Speaker 2: So If a bizarre burst of radiation occurs, or a
[34:15] Speaker 2: galaxy exhibits a structural deformity that doesn't align with the
[34:19] Speaker 2: standard model of gravity, the AI flags it immediately. Instead
[34:22] Speaker 2: of a graduate student spending six months staring at photographic
[34:25] Speaker 2: plates hoping to notice a slight discrepancy, the AI will
[34:28] Speaker 2: theoretically scan incoming data feeds, cross reference them with the
[34:32] Speaker 2: five point six trillion pixel baseline, and instantly alert a
[34:36] Speaker 2: research team to an anomaly in the fabric of space.
[34:39] Speaker 3: We are rapidly transitioning from human led observation to AI
[34:43] Speaker 3: driven anomaly detection. The algorithms will highlight the fractures in
[34:47] Speaker 3: our understanding of physics, and human scientists will investigate those fractures.
[34:51] Speaker 2: It is a radically different landscape for exploration than we
[34:54] Speaker 2: had even ten years ago. If we step back and
[34:56] Speaker 2: look at the trajectory of everything we've explored today, the
[34:59] Speaker 2: scale is almost overwhelming.
[35:00] Speaker 3: It really is.
[35:01] Speaker 2: We started with the sheer logistical terror of compiling two
[35:04] Speaker 2: hundred and sixty three four hundred and seven atmospheric exposures,
[35:07] Speaker 2: utilizing a year of custom coding and eight weeks of
[35:10] Speaker 2: supercomputer processing to render a five point six trillion pixel image.
[35:14] Speaker 3: Just a monumental effort.
[35:16] Speaker 2: And then we transition from that two D map into
[35:18] Speaker 2: a three D hunt for the invisible scaffolding of dark matter.
[35:22] Speaker 2: We navigated the stunning, deeply unsettling early data suggesting that
[35:26] Speaker 2: the force pushing our universe apart is actively weakening, threatening
[35:30] Speaker 2: a total cosmic collapse.
[35:32] Speaker 3: The big crunch right.
[35:34] Speaker 2: And finally we look at how this massive public map
[35:37] Speaker 2: is currently training the AI that will run the next
[35:39] Speaker 2: generation of massive observators.
[35:42] Speaker 3: But I think the defining characteristic of this achievement is
[35:45] Speaker 3: that the map is not a closed system.
[35:47] Speaker 2: What do you mean?
[35:48] Speaker 3: The entire five point six trillion pixel catalog of the
[35:52] Speaker 3: universe is sitting on open servers right now. The barrier
[35:55] Speaker 3: to entry for cosmic exploration has been completely dissolved.
[36:00] Speaker 2: Can access it. Which leaves me with a final lingering
[36:02] Speaker 2: thought for you listening. I want you to genuinely consider
[36:05] Speaker 2: this the next time you step outside and look up
[36:06] Speaker 2: at the dark sky. We know that the early targeting
[36:09] Speaker 2: data pulled from this map has already provided the initial
[36:12] Speaker 2: hints that dark energy is weakening, a revelation that could
[36:15] Speaker 2: entirely break the standard model of cosmology.
[36:17] Speaker 3: The biggest discovery in decades.
[36:20] Speaker 2: Yeah, if that pariim shifting discovery was unearthed just in
[36:23] Speaker 2: the initial passes of the data, what completely unimaginable alien
[36:28] Speaker 2: forces are currently hiding inside those five point six trillion pixels.
[36:32] Speaker 3: It's just waiting to be found.
[36:33] Speaker 2: The architecture of new physics is sitting on a public
[36:35] Speaker 2: server right now, silently waiting for a future AI or
[36:39] Speaker 2: perhaps a deeply curious citizen scientist panning to the sky
[36:42] Speaker 2: viere on a quiet Tuesday evening to finally notice it.
[36:46] Speaker 2: Thank you so much for joining us on this journey today.
[36:48] Speaker 2: Keep looking up

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