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Starts With A Bang

Galactic Snakes On Our Galactic Plane? What NASA’s Newest Images Reveal

This X-ray/radio panorama of the galactic center takes data from NASA’s Chandra and South Africa’s MeerKAT telescopes. X-rays from Chandra are orange, green, and purple, showing different X-ray energies, and the radio data from MeerKAT are gray. A variety of interconnected features are on display here, enabling us to uncover the origin of galactic energy transport. (X-RAY: NASA/CXC/UMASS/Q.D. WANG; RADIO: NRF/SARAO/MEERKAT)

With radio and X-ray data combined, we’re understanding how energy flows like never before.


When we look out at the Universe on the largest cosmic scales of all, gravity is the only force that matters. Even though the other fundamental forces of nature are far stronger, the weak and strong nuclear forces are only short-range forces, while the Universe is electrically neutral overall, leaving gravitation alone to dominate. But inside large, massive structures like galaxies, the normal matter contracts and collapses, forming stars and gas clouds, interacting with black holes and neutron stars, and experiencing otherwise “messy” physical conditions.

In our nearby Universe, no place is messier than our galactic center. Located some 27,000 light-years away, we’ve discovered the most massive black hole within the nearest ~2 million light-years: Sagittarius A*, containing as much mass as four million Suns. But surrounding that are all sorts of fascinating features: cold gas clouds, clusters of new stars, supernova remnants, and elongated filaments of hot, X-ray emitting matter. With the newest data from NASA’s Chandra X-ray telescope providing a deep, high-resolution view of the Milky Way’s core, it’s now possible to untangle these “snakes” to reveal precisely what’s inside.

Four-color image of the X-rays surrounding the galactic plane. Lower X-ray energies are in orange, escalating upwards through green, blue, and violet. Note the large number of point sources strewn about the image, while the central molecular zone emits the highest energies in the middle of the image, corresponding to the galactic plane. (X-RAY: NASA/CXC/UMASS/Q.D. WANG)

The first thing we can look at, above, is the X-rays themselves, but to look at them color-coded by energy. X-rays, in general, come in two different categories:

  • hard X-rays, which are higher in energies and have wavelengths the size of a single atom or smaller,
  • and soft X-rays, which are lower in energies (but still more energetic than ultraviolet light) and have wavelengths larger than the size of a single atom.

There are four independent features you should notice when looking at the X-ray images. The first feature is that they come in two different colors: orange/red and blue/violet, where the orange-red colors represent soft X-rays and the blue/violet ones are hard X-rays. Second, the soft X-rays exist above and below the galactic plane, while the hard X-rays dominate in the plane of the galaxy itself. Third, there are a large number of “dots” smattered throughout the image; these are point sources, like black holes and neutron stars. And, perhaps most prominently, there are a large number of ultra-luminous, saturating “white” regions, which correspond to regions where the X-ray flux is tremendous across multiple energies.

Radio view of the innermost few degrees of the galactic center from MeerKAT. Unlike the complementary X-ray view, the radio data traces out a different set of features: radio lobes, tightly aligned, narrow filaments, and material appearing to radiate away from the central molecular zone. Many of these filaments emit strongly polarized light. (RADIO: NRF/SARAO/MEERKAT)

One of the ways we gain important information about the Universe is by looking not just in one set of wavelength bands, like the X-ray, but in disparate ones. Above is the same exact region of space, except instead of being imaged in X-rays from space, it’s been imaged in radio wavelengths from the ground: by the MeerKAT array of radio telescopes. Unlike in the X-ray portion of the spectrum, the radio signals appear to trace out filament-like shapes that appear to serve as bridges, connecting the various X-ray emitting regions to one another or at least appearing to be emitted from the brightest X-ray regions.

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This tells us that something is likely happening between the stars — in the interstellar space separating them — that’s being elongated into thread-like features over enormous distance scales: around ~20 light-years across, typically. These thread-like features may seem unusual, but very similar structures have been observed in space before, although not in galactic environments like this. Instead, these threads are most similar to the traced lines we’ve seen in a completely different realm: close to the surface of the Sun.

Solar coronal loops, such as those observed by NASA’s Transition Region And Coronal Explorer (TRACE) satellite here in 2005, follow the path of the magnetic field on the Sun. When these loops ‘break’ in just the right way, they can emit coronal mass ejections, which have the potential to impact Earth. A large CME or solar flare could create a new type of natural disaster: a ‘Flaremageddon’ scenario. (NASA / TRACE)

What you can see, just beyond the Sun’s photosphere, are loop-like structures that are glowing with hot, plasma-rich streams of matter. These can be described as plumes or fountains, appearing as though there are threads connecting different regions of the Sun, and these bright plumes trace out those thread lines.

Physically, we understand what’s happening in terms of magnetism. The Sun has regions across it that vary in temperature, and the ionized nature of the solar plasma tells us that electrons and atomic nulcei will get transported at different rates owing to their different charge-to-mass ratios. This creates charge separations and electric currents, which in turn create magnetic fields, which in turn confine plasmas and create these telltale structures on the Sun.

Also, when these magnetic field lines align, anti-align, break, and/or reconnect, they can trigger the emission of fast-moving particles and the ejection of matter. That provides the origin, at least as far as we know, of events like solar flares, intense ejections of matter, and other examples of space weather.

An X-class solar flare erupted from the Sun’s surface in 2012: an event that was still much, much lower in brightness and total energy output than the 1859 Carrington event, but which could have still caused a catastrophic geomagnetic storm if it had been accompanied by a coronal mass ejection whose magnetic field had the right (or wrong, depending on your point of view) orientation. (NASA/SOLAR DYNAMICS OBSERVATORY (SDO) VIA GETTY IMAGES)

One theory that was put forth as to the nature of these features in the galactic center is that they’re similar in origin. The galactic center has been known, for some time, to possess the following properties:

  • there’s a strong gravitational source there in the form of our central black hole,
  • the interstellar medium has high temperatures and densities,
  • the matter flowing around in that medium has large velocities and displays turbulent properties,
  • and there are strong magnetic fields at play there as well: not coherent over large distance scales but rather with features that only persist for a few light-years at once.

In addition, our central black hole is presently quiet, but the surrounding environment displays evidence that it was active relatively recently. Many nearby regions — which appear as bright spots in the X-ray image — consist of either bright, young star clusters only a few million years old, or dense gas clouds that are either in the process of forming new stars or contracting under their own gravity: a predecessor to star-formation.

Multiwavelength views of the galactic center have been used for a long time to try and identify various features. Shown here, there are a number of point sources, star clusters, and gas features that stand out. However, in order to identify the interstellar features that transport energy from the center to the halo, high-resolution radio observations combined with X-ray observations are needed. (NASA/JPL-CALTECH/ESA/CXC/STSCI)

The densest of these clouds are found in what we call the central molecular zone, which also contain some of the youngest new stars present in the Milky Way. Given that there are also high-energy structures found in the galactic bulge and halo — extending significantly away from the galactic plane itself — many have speculated that there is some type of connection between the central activity in the galaxy with these extended structures. But in order to test that speculation, we needed high-resolution data in multiple wavelengths of light, and specifically in the radio and the X-ray, together.

In particular, there’s one filament — just below and to the left of the galactic center as viewed from the orientations shown here — known as G0.17–0.41, which shows both X-ray and radio light overlapping in this thin, narrow region approximately 20 light-years in extent. A long filament like this can form between two strongly magnetized, ionized regions under similar conditions to what occurs in the Sun: when two magnetic structures with anti-aligned fields suddenly reconnect, releasing an enormous amount of energy. The X-ray emissions, located precisely where this radio “filament” is found, offers some very strong support for this picture.

This X-ray/radio composite of filament G0.17–0.41 spans 20 light-years, but is only ~1/5 of one light-year wide. The tight collimation visible here against the background X-ray point sources is evidence that the X-ray emitting material is confined within a strand of magnetic field with a large strength: 1 milligauss or greater. (X-RAY: NASA/CXC/UMASS/Q.D. WANG; RADIO: NRF/SARAO/MEERKAT)

This is very, very similar to another thread-like feature that had been observed previously: G359.55+0.16. Again, X-ray and radio emissions overlap, but what’s particularly compelling here is that the filaments are so long — about 20 light-years in extent in each case — compared to their width, which is just 1/100th of their lengths. The fact that we can resolve these features and peer into their nature from these multi-wavelength views can help us at last understand just how activity in the galactic center can create not only these intricate features, but give rise to extremely high-energy cosmic rays and other energetic events.

According to Q. Daniel Wang, who wrote the scientific paper associated with this new set of observations and images:

“The galaxy is like an ecosystem. We know the centers of galaxies are where the action is and play an enormous role in their evolution. This thread reveals a new phenomenon. This is evidence of an ongoing magnetic field reconnection event.”

What’s fascinating about this is that it provides direct evidence for a “missing link” phenomenon that takes too long to observe over the timescale of a human lifetime: how energy is transported from the inner regions of a galaxy away from the center, influencing the matter around it.

Magnetic fields in Messier 82, or the Cigar galaxy, are shown as lines over a visible light and infrared composite image of the galaxy from the Hubble Space Telescope and the Spitzer Space Telescope. Stellar winds streaming from hot new stars form a galactic super wind that is blasting out plumes of hot gas (red) and a huge halo of smoky dust (yellow/orange) perpendicular to the narrow galaxy (white). (NASA, SOFIA, L. PROUDFIT; NASA, ESA, HUBBLE HERITAGE TEAM; NASA, JPL-CALTECH, C. ENGELBRACHT)

In galaxies like Messier 82, above, also known as the Cigar galaxy, you can clearly see (in red) how a burst of recent star-formation can translate into strong galactic winds, which impart large amounts of energy to the gas and plasmas found in the environment surrounding the galactic center. Over long periods of time, this can result in energy and matter being transported not only from the inner regions to the outer regions of the galaxy, but can kick material out of the galaxy entirely, removing its ability to form new generations of stars in the future.

Importantly that’s not what’s going on in our Milky Way, at least not from the study shown here. These energetic features we’re discovering are still located within the inner reaches of our galaxy, extending for up to a few hundred light-years away from the galactic center. For contrast, the largest features we’ve found related to energy being transported from the galactic center to the outskirts are known as Fermi bubbles: diffuse, X-ray emitting plasma extending for tens of thousands of light-years above and below the galactic plane. Although both are caused by energetic phenomena originating from the galaxy’s center, there is no identified connection between this study and these outer phenomena.

On either side of the plane of the Milky Way, enormous gamma-ray bubbles are being blown. The energy spectrum seen indicates that positrons had been generated recently in great amounts, creating bubbles some 50,000 light-years in total extent. Both gamma-rays and X-rays are generated, powered by the 4 million solar mass engine at the center of the Milky Way. (NASA/GODDARD SPACE FLIGHT CENTER)

However, what is notable about the magnetic fields that ought to be present in the galaxy’s center is their unusually large strength. When we look out at galaxies in the Universe, we have a technique for how to measure the strength of their fields: a phenomenon called Faraday rotation. When you point your telescope at a background light source in space, the light will typically be unpolarized: the polarizations of the arriving photons will be random, and won’t prefer horizontal to vertical or right-circular to left-circular directions or vice versa.

If that light passes through a region where you have a coherent magnetic field, however, that light will become preferentially polarized in one direction versus the other, proportional to the strength and direction of the magnetic field. For most galaxies where Faraday rotation is detectable, we observe field strengths between a nanogauss and a microgauss, on scales from dozens to thousands of light-years.

What we’re finding along these filaments, however, are fields that are much stronger: greater than one milligauss, or over 1,000 times stronger than a typical galactic magnetic field. This is expected only to occur along radio filaments: thin thermal plasmas powered by magnetic reconnection. When we overlay X-ray and radio data together the two radio/X-ray filaments, highlighted in red boxes, clearly stand out.

This annotated diagram shows many regions of interest in this X-ray/radio composite of the Milky Way’s galactic center. Although the X-ray data and the radio data don’t appear to have much in common, the two filaments, outlined in red, represent the ‘smoking gun’ evidence for radio filament magnetic reconnection, giving us a new window into the high-energy Universe. (X-RAY: NASA/CXC/UMASS/Q.D. WANG; RADIO: NRF/SARAO/MEERKAT)

The center of our galaxy houses some of the most interesting physical and astrophysical phenomena around, and yet it’s maddeningly difficult to observe. From within our own Milky Way, observing other locations is tremendously difficult because of all the intervening matter in the way. Neutral gas, dust grains, and ionized plasmas not only can block a significant fraction of the light we’re interested in, but they also emit their own light. As the old saying goes, however, one astronomer’s noise is another astronomer’s data.

By leveraging high-resolution radio and X-ray images of the central region of the galaxy together, we can finally identify the long sought-after radio filaments that showcase these strong magnetic features in our galaxy, and they match up exquisitely with X-ray emission as well. The magnetic reconnection events that likely underlie them are the first direct evidence we have for the theoretical prediction that solar flare analogues should exist in our galaxy, driven by the hot young star clusters found in the galactic center. With more research, astronomers now hope to learn how cosmic rays accelerate, hot plasma heats up to even greater temperatures, and how turbulence arises in these extreme environments. The high energy galaxy, with both radio and X-ray data combined, just got a lot cooler and hotter in tandem.


Starts With A Bang is written by Ethan Siegel, Ph.D., author of Beyond The Galaxy, and Treknology: The Science of Star Trek from Tricorders to Warp Drive.


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