More than meets the eye: unravelling the cosmos at the highest energies Understand article

Claudia Mignone and Rebecca Barnes explore X-rays and gamma rays and investigate the ingenious techniques used by the European Space Agency to observe the cosmos at these wavelengths.

Viewed with the naked eye, binoculars or a telescope, the starry night sky is an overwhelming and tranquil sight. But if we could view the sky in highly energetic X-rays and gamma rays, rather than the visible light perceived by our eyes, we would see a very different picture – a dramatic cosmic light showw1 (Figure 1).

Figure 1: Above: an all-sky image at high-energy X-ray wavelengths from ESA’s INTEGRAL space observatory, based on data collected in the 18-40 keV energy range (visible light corresponds to 1.65–3.1 eV). Below: an all-sky image at visible wavelengths. Click on images to enlarge
Images courtesy of ESA / F Lebrun / CEA Saclay, Service d’Astrophysique (above); ESO / S Brunier (below)
Figure 2: The Tycho
supernova remnant as
viewed by ESA’s XMM-
Newton. This remnant is
relatively young and is
associated with a supernova
explosion that was observed
in 1572 by the Danish
astronomer Tycho Brahe.
Click on image to enlarge

Image courtesy of Marco
Iacobelli (XMM-Newton SOC)
and ESA

Some of the most powerful and violent phenomena in the Universe shine brightly at these short wavelengths, such as supernova explosions – the fiery demise of a massive star’s life – and black holes, rapidly devouring matter. As a sign of their dynamic nature, many sources of X-rays and gamma rays exhibit distinct changes in their brightness, even over very short periods of time. Gamma-ray bursts, for example, appear as sudden bright flashes that last just a few seconds. These bursts arise from possibly the most extreme explosions in the cosmos (to learn more, see Boffin, 2007). Furthermore, X-rays and gamma rays are released through different physical processes than those responsible for the emission of visible light. This means that galaxies and other astronomical objects look different when imaged at the high-energy end of the electromagnetic (EM) spectrumw2 (Figures 2 and 3).

Figure 3: The Cigar Galaxy (M82), as viewed by XMM-Newton, at visible and ultraviolet (UV) wavelengths (inset left) and at X-ray wavelengths (inset right). The main image is a composite of the visible, UV and X-ray wavelength images. The X-ray emission is shown in blue and reveals plumes of very hot gas bursting out of the galaxy’s disc. Click on image to enlarge
Image courtesy of ESA

This revolutionary view of the cosmos was revealed to astronomers in the early 1960s, with the beginning of the space age, when rockets and satellites allowed specially developed instruments to be carried beyond the obscuring barrier of Earth’s atmospherew3. The European Space Agency (ESA; see box)w4 soon joined in, with the gamma-ray mission COS-B (1975) and the X-ray observatory EXOSAT (1983). Today, ESA operates two such observatories: the X-ray Multi-Mirror satellite (XMM-Newton), launched in 1999, and the International Gamma-Ray Astrophysics Laboratory (INTEGRAL), launched in 2002.

How do they work? As we explained in an earlier article (Mignone & Barnes, 2011), there is no physical distinction between X-rays, gamma rays, visible light and other types of EM radiation. All are forms of light, differing only in their wavelength (or, as the three are correlated, their frequency or energy; Figure 4). However, depending on their wavelength (or frequency, or energy), they interact very differently with matter. This has major implications for astronomy.

Figure 4: A scheme of the EM spectrum highlighting X-rays and gamma rays, with indications of wavelength, frequencies and energies across the spectrum. Click on image to enlarge
Image courtesy of ESA / AOES Medialab

Traditional optical systems, such as our eyes, cameras, microscopes or telescopes, rely on lenses (or mirrors) that refract (or reflect) light rays and focus them into a single point to produce images. However, this is difficult with some light rays. Because X-rays and gamma rays have wavelengths of a similar size to atoms and sub-atomic particles, respectively, they cannot easily be reflected or focused like visible light, but tend instead to be absorbed when they strike denser materials (Figure 5).

Figure 5: Light rays striking a surface will be absorbed if their energy is higher than a certain threshold value, which depends on the surface material. The energy of the absorbed light is transferred to electrons in the material, which are then emitted. This phenomenon, known as the photoelectric effectw5, is one of several phenomena that occur when highly energetic radiation interacts with matter. For a dramatic way to teach the subject at school, see Bernardelli (2010).
Click on image to enlarge

Image courtesy of ESA / AOES Medialab

The fact that X-rays and gamma rays are absorbed by dense materials makes them suitable for many applications, including medical scans and investigations of materials. For astronomers, however, it is a problem: being easily absorbed, these types of radiation are very difficult or impossible to focus; thus obtaining sharp images of their sources is a challenge.

Nonetheless, scientists have developed techniques to detect X-rays and gamma rays coming from the cosmos. They differ greatly from techniques used in traditional optics and that, together with the fact that they operate in space, means that telescopes for high-energy astronomy look nothing like optical telescopes.

Skimming stones
Image courtesy of Killy Ridols;/
image source: Wikimedia
Commons

X-ray observing techniques

Although it is difficult to reflect X-rays, it is not impossible if they hit the telescope’s mirror at a very small angle – think of a pebble skimming across the surface of the water. However, whereas an incidence angle as large as 20° will allow the stones to bounce, X-rays can be reflected only at much smaller angles: 1° or even less. The X-rays must barely graze the mirror, or they are likely to be absorbed.

To achieve this small angle – and focus the X-rays to a single point – the mirrors used in X-ray telescopes look rather like a funnel (Figure 6). In fact, the mirror shape is a combination of a paraboloid and a hyperboloid, ensuring that the X-rays that graze it are reflected twice. In this way, light is focused onto a detector to form an image of the X-ray source.

Figure 6:
a) The light path of X-rays through XMM-Newton. The spacecraft carries three telescopes each consisting of
58 nested, gold-coated, tube-like mirrors.
b) The combination of parabolic and hyperbolic mirrors used is shown in cross section through one of the telescopes
c) X-rays that graze the mirror surfaces are reflected twice and focused onto a detector. The X-rays must graze the mirror at angles of 1° or even less, or they are likely to be absorbed. Click on image to enlarge

Image courtesy of ESA / AOES Medialab
Figure 7: The nested mirrors
constituting one of the three
telescopes on board
XMM-Newton

Image courtesy of ESA

This ingenious technique, called grazing incidence optics, has one main drawback: to be reflected and focused, the X-rays must be travelling almost parallel to the tube-like mirrors, so these telescopes collect only limited amounts of X-ray radiation. A powerful telescope is one that collects large amounts of light from distant cosmic sources; this is usually achieved with very large mirrors. In contrast, to maximise their power, X-ray telescopes have several mirrors nested within one another, creating a structure that resembles a giant leek. The three telescopes on board ESA’s XMM-Newton space observatory, for example, each consist of 58 nested mirrors (Figure 7)w6.

Besides their bizarre shape, XMM-Newton’s mirrors differ from conventional telescope mirrors in that they are made of gold-coated nickel rather than aluminium-coated glass: the heavier elements are more likely to reflect incoming X-rays (to learn more, see Singh, 2005).

Gamma-ray observing techniques

Figure 8a) Artist’s impression
of INTEGRAL highlighting SPI,
one of the coded-mask
instruments on board the
spacecraft.
Click on image to enlarge

Image courtesy of ESA / AOES
Medialab

If focusing X-rays is challenging, focusing gamma rays – the most energetic form of light – is almost impossible. To produce images of cosmic sources in this portion of the EM spectrum, therefore, astronomers had to find alternative methods.

Many instruments for gamma-ray astronomy, including those on board ESA’s INTEGRAL space observatory, rely on a technique called coded-mask imaging. This works similarly to a pinhole camera, which has no lens, just a tiny hole through which light rays pass, projecting an inverted image on the opposite wall of the camera.

Figure 8b) How the coded-
mask camera works: gamma-
rays from two different
astronomical sources pass
through the mask’s holes.
Some of the incident gamma
-rays can pass through the
mask and illuminate pixels
on the detector below (shown
in blue and red, depending
on the source), while others
are blocked by the mask’s
opaque spots, casting
shadows on the detector
(shown in white).
Click on image to enlarge

Image courtesy of ESA / AOES
Medialab

In place of the pinhole camera’s single hole, a coded-mask camera has a mask with a special pattern of holes and opaque spots in front of a detector. Gamma rays that pass through the holes illuminate some pixels on the detector, while others are blocked by the mask’s opaque spots and cast shadows on the detector.

The pattern of bright and dark pixels contains information about the location of gamma-ray sources in the sky, and the intensity of the illuminated pixels gives information about their brightnessw7. Albeit not detailed, the resulting images are useful to probe some of the most powerful phenomena in the Universe (Figuras 8a and 8b, 9 and 10).

Figure 9: INTEGRAL images of the intermittent source IGR J16328-4726 (encircled). This astronomical source has been monitored over several years with INTEGRAL in the energy range 20-50 keV. As can be seen, the brightness of the source varies significantly over time. Astronomers believe that the source is a supergiant fast X-ray transient: a binary system consisting of a very luminous, supergiant star and a compact object, such as a neutron star or a black hole, orbiting one another. The irregular flow of matter from the supergiant star to the compact object is believed to cause the intermittent nature of these sources. Click on image to enlarge
Image courtesy of ESA / INTEGRAL / M Fiocchi
Figure 10: Artist’s impression
of a supergiant fast X-ray
transient.
Click on image to enlarge

Image courtesy of ESA

Coming up…

As you read this article, ESA’s XMM-Newton and INTEGRAL observatories are circling Earth, keeping watch over the ever-changing, high-energy Universe and helping to unravel celestial wonders. In our next article, we will explore some of these phenomena, such as the turbulent life and death of stars in the Milky Way, and gigantic black holes at the centres of distant galaxies.

 

More about ESA

The European Space Agency (ESA)w4 is Europe’s gateway to space, organising programmes to find out more about Earth, its immediate space environment, our Solar System and the Universe, as well as to co-operate in the human exploration of space, develop satellite-based technologies and services, and to promote European industries.

The Directorate of Science and Robotic Exploration is devoted to ESA’s space science programme and to the robotic exploration of the Solar System. In the quest to understand the Universe, the stars and planets and the origins of life itself, ESA space-science satellites peer into the depths of the cosmos and look at the furthest galaxies, study the Sun in unprecedented detail, and explore our planetary neighbours.

ESA is a member of EIROforumw8, the publisher of Science in School.

 

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References

Web References

Resources

  • The Science@ESA vodcasts explore our Universe through the eyes of ESA’s fleet of science spacecraft. Episode 5 (‘The untamed, violent Universe’) offers a glimpse of the hot, energetic and often violent universe, and the ESA missions that detect it using X-ray and gamma-ray astronomy. See: http://sci.esa.int/vodcast

Institution

ESA

Author(s)

Claudia Mignone, Vitrociset Belgium for ESA – European Space Agency, is a science writer for ESA. She has a degree in astronomy from the University of Bologna, Italy, and a PhD in cosmology from the University of Heidelberg, Germany. Before joining ESA, she worked in the public outreach office of the European Southern Observatory (ESO).

Rebecca Barnes, HE Space Operations for ESA – European Space Agency, is the education officer for the ESA Science and Robotic Exploration Directorate. She has a degree in physics with astrophysics from the University of Leicester, UK, and previously worked in the education and space communications departments of the UK’s National Space Centre. To find out more about the education activities of the ESA Science and Robotic Exploration Directorate, contact Rebecca at SciEdu@esa.int


Review

This article explains simply and comprehensibly how X-rays and gamma rays are collected from cosmic sources using modern space telescopes, and it provides some dramatic images.

For science teachers in primary schools, the article may provide motivation to build a model telescope in lessons, for example using recycled materials – or to use the downloadable satellite models on the ESA websitew4. The colourful images can also form part of a class exhibit.

Science or physics teachers at secondary school (students aged 11-16) can link to the topic of gamma-ray imaging techniques using a pinhole camera. This would be appropriate in optics lessons, emphasising that both the pinhole camera and coded-mask imaging work without an optical lens.

Images taken by ESA’s observatoriesw4 would be a useful support for teaching space observation, helping to familiarise students with the different astronomical phenomena (e.g. galaxies, black holes, supernovas, neutron stars, or the annihilation of matter and anti-matter) mentioned in the article. It could also encourage students to do some research of their own on related areas within the curriculum.

For teachers of older school students, it would be interesting to discuss the type of telescopes for high-energy astronomy that are on board the space observatories XMM-Newton and INTEGRAL, and the techniques used to filter the data until the images are fully extracted (this could be linked to IT lessons). Students could compare the structure of telescopes in the high-energy end of the spectrum to that of the optical telescope, and investigate the difficulties encountered when building them.


Stephanie Maggi-Pulis, Malta




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