From Ethan Siegel: “The future of astronomy: thousands of radio telescopes that can see beyond the stars”

Ethan Siegel
June 21, 2017

[SO, DID ETHAN FINALLY DISCOVER SKA? IT LOOKS LIKE THAT IS TRUE. I DID A SEARCH, “ETHAN SIEGEL AND SKA” AND CAME UP WITH NOTHING BUT THIS POST. ETHAN, WHAT ROCK HAVE YOU BEEN LIVING UNDER? COME BACK TO ME AND ENLIGHTEN ME.]

The future of astronomy: thousands of radio telescopes that can see beyond the stars.

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The Square Kilometer Array will, when completed, be comprised of an array of thousands of radio telescopes, capable of seeing farther back into the Universe than any observatory that has measured any type of star or galaxy. Image credit: SKA Project Development Office and Swinburne Astronomy Productions.

Never heard of SKA, the square kilometer Array? Once it starts taking data, you’ll never forget it.

SKA Square Kilometer Array

SKA South Africa

“Not all chemicals are bad. Without chemicals such as hydrogen and oxygen, for example, there would be no way to make water, a vital ingredient in beer.” -Dave Barry

By building bigger telescopes, going to space, and looking from ultraviolet to visible to infrared wavelengths, we can view stars and galaxies as far back as stars and galaxies go. But for millions of years in the Universe, there were no stars, no galaxies, nor anything that emitted visible light. Prior to that, the only light that existed was the leftover glow from the Big Bang, along with the neutral atoms created during the first few hundred thousand years.

CMB per ESA/Planck

ESA/Planck

For those millions of years, there’s simply never been a way to gather information from the electromagnetic part of the spectrum. But a combination of advances in computing and the new construction of an array of thousands of large-scale radio telescopes across twelve countries opens up an incredible possibility like never before: the ability to map the neutral atoms themselves.

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Distant sources of light — even from the cosmic microwave background [CMB, above] — must pass through clouds of gas. If there’s neutral hydrogen present, it can absorb that light, or, if it’s excited in some way, it can emit light of its own. Image credit: Ed Janssen, ESO [Includes inage of ESO’s VLT at Cerro Paranel, Chile].

How can you see neutral atoms? After all, unless you’re dealing in either reflected light or with atoms that are themselves in an excited state, neutral atoms are some of the most optically boring materials that there are. Atoms are made of negatively charged electrons surrounding a positively charged nucleus, capable of occupying a variety of quantum states. But early on, for millions of years after the Big Bang, 92% of the atoms are the most boring type that exists: hydrogen, with a single proton and electron. While many different energy states exist, without any external source to excite it, hydrogen atoms are doomed to live in the lowest-energy (ground) state.

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The energy levels and electron wavefunctions that correspond to different states within a hydrogen atom. The energy levels are quantized in multiples of Planck’s constant, but even the lowest energy, ground state has two possible configurations depended on the relative electron/proton spin. Image credit: PoorLeno of Wikimedia Commons.

But when you first make neutral hydrogen, not all the atoms are perfectly in the ground state. You see, in addition to energy levels, the particles in atoms also have a property called spin: their intrinsic angular momentum. A particle like a proton or an electron can either be spin up (+½) or spin down (-½), and so a hydrogen atom can either have the spins aligned (both up or both down) or anti-aligned (one up and the other down). The anti-aligned combination is slightly lower in energy, but not by much. The transition from an aligned state to an anti-aligned one takes millions of years to occur, and when it does, the atom emits a photon of a very particular wavelength: 21 centimeters.

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The 21-centimeter hydrogen line comes about when a hydrogen atom containing a proton/electron combination with aligned spins (top) flips to have anti-aligned spins (bottom), emitting one particular photon of a very characteristic wavelength. Image credit: Tiltec of Wikimedia Commons.

Every time you undergo a burst of star formation, you ionize hydrogen atoms, meaning that electrons will fall back onto protons eventually, forming a large number of aligned atoms. By looking for this 21-cm signal, we can:

construct a map of nearby, recent star formation,
detect absorbing, neutral sources of anti-aligned gas,
build a 3D map of neutral gas throughout the Universe,
detect how star clusters and galaxies formed and evolved over time,
and possibly detect the absorption and emission features of hydrogen gas immediately after, during, and possibly even before the formation of the first stars.

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Before the formation of the first stars, there’s still neutral hydrogen gas to observe, if we look for it in the right way. Image credit: European Southern Observatory.

Lambda-Cold Dark Matter, Accelerated Expansion of the Universe, Big Bang-Inflation (timeline of the universe) Date 2010 Credit: Alex MittelmannColdcreation


Somehow, this image seems fitting at this point.

Next year, in 2018, just as the James Webb Space Telescope prepares for launch,

NASA/ESA/CSA Webb Telescope annotated

construction will begin on the Square Kilometer Array (SKA) [This is not correct. much has already been done. If Ethan skips over it, I will not let it pass uncovered.] SKA will wind up, at completion, being an array of some 4,000 radio telescopes, each approximately 12 meters in diameter, and capable of detecting this 21-cm line back farther than any galaxy we’ve ever seen. While the current galactic record-holder comes from when the Universe was just 400 million years old — 3% of its current age — SKA should be able to get the first 1% of the Universe that even James Webb might not see.

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Only because this distant galaxy, GN-z11, is located in a region where the intergalactic medium is mostly reionized, can Hubble reveal it to us at the present time. James Webb will go much farther, but SKA will image the hydrogen that’s invisible to all other optical and infrared observatories. Image credit: NASA, ESA, and A. Feild (STScI).

To go beyond the first stars, or to arrive at a cosmic destination where no ultraviolet or visible light can pass through the opaque, intergalactic medium, you need to probe what’s actually there. And in this Universe, the overwhelming majority of what’s there, at least that we can detect, is hydrogen. That’s what we know is out there, and that’s what we’re building SKA with the intention of seeing. It will collect more than ten times the data per second than any array today; it will have more than ten times the data collecting power; and it is expected to map the entire Universe from here all the way back to before the first galaxies. We will learn, in the most powerful way ever, how stars, galaxies, and the gas in the Universe grew up and evolved over time.

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A single dish that’s currently part of the MeerKAT array will be incorporated into the Square Kilometer Array, along with around 4,000 other equivalent dishes. Image credit: SKA Africa Technical Newsletter, 1 (2016).

A better image, and this is just South Africa:

SKA Meerkat telescope, 90 km outside the small Northern Cape town of Carnarvon, SA

According to Simon Ratcliffe, SKA scientist, we know some of what we’re going to find with SKA, but it’s the unknowns that are the most exciting.

“Every time we’ve set out to measure something, we’ve discovered something entirely surprising.”

Radio astronomy has brought us pulsars, quasars, microquasars, and mysterious sources like Cygnus X-1, which turned out to be black holes. The entire Universe is out there, waiting for us to discover it. When SKA is completed, it will shed a light on the Universe beyond stars, galaxies, and even gravitational waves. It will show us the invisible Universe as it truly is. As with anything in astronomy, all we need to do is look with the right tools.

O.K., not O.K., here is some of what Ethan did not include:

SKA/ASKAP radio telescope at the Murchison Radio-astronomy Observatory (MRO) in Mid West region of Western
Australia

Murchison Widefield Array,SKA Murchison Widefield Array, Boolardy station in outback Western Australia, at the Murchison Radio-astronomy Observatory (MRO)

Artist’s impression of the Mid-Frequency Aperture Array telescope when deployed on the African site (C) SKA Organisation

SKA LOFAR core (“superterp”) near Exloo, Netherlands

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EMBRACE is the Electronic MultiBeam Radio Astronomy ConcEpt which is the Pathfinder instrument for the SKA at frequencies between 500MHz and 1500MHz.

Seriously, Ethan, come back to me and tell me why you did not include these assets. After that, do a serious piece on Radio Astronomy that includes the Jansky VLA, the EHT, the European VLBI, The Global mm-VLBI Array, the NRAO VLBA. GBO, Parkes, The Goldstone Deep Space Communications Complex, NASA’s DEEP SPACE NETWORK, and whatever else is slipping my mind. I could put in all of the images because I have them. But, you are fantastic with images, so I will leave it to you to do it right.

See the full article here .

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“Starts With A Bang! is a blog/video blog about cosmology, physics, astronomy, and anything else I find interesting enough to write about. I am a firm believer that the highest good in life is learning, and the greatest evil is willful ignorance. The goal of everything on this site is to help inform you about our world, how we came to be here, and to understand how it all works. As I write these pages for you, I hope to not only explain to you what we know, think, and believe, but how we know it, and why we draw the conclusions we do. It is my hope that you find this interesting, informative, and accessible,” says Ethan

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