More than meets the eye: the cold and the distant Universe Understand article

In the fifth and final article in this series on astronomy and the electromagnetic spectrum, find out how scientists use the European Space Agency’s missions to observe the sky in far-infrared, sub-millimetre and microwave light.

The Orion A star-formation
cloud seen by ESA’s Herschel
Space Observatory

Image courtesy of ESA /
Herschel / Ph André, D
Polychroni, A Roy, V Könyves,
N Schneider for the Gould Belt
survey Key Programme

Five thousand light years from Earth lies the coldest object found in the Universe, the Boomerang Nebula – a dying star leaving behind a cloud of gas that is only one degree above 0 K – absolute zero. This cloud, like other cold objects in the Universe, is invisible to the naked eye.

The cooler an object is, the longer the wavelengths of light it emitsw1. With temperatures of 50 K or less, cool portions of interstellar gas and cosmic dust emit light at far-infrared (25 to 350 μm) and sub-millimetre (350 μm to 1 mm) wavelengths, much longer than our eyes can see. So how do we know that these cold objects exist? To capture the radiation and ‘see’ the objects in wavelengths beyond the visible range, astronomers use dedicated far-infrared (FIR), sub-millimetre (sub-mm) and microwave telescopes.

This approach comes with challenges: light at these long wavelengths is absorbed by water vapour and other molecules in Earth’s atmosphere, which makes observations from the ground extremely difficult and, at FIR wavelengths, simply impossible. For most infrared wavelengths, the atmosphere itself also emits light, adding an unwanted source of noise to the cosmic signals that astronomers are interested in.

To combat these problems, long-wavelength telescopes can be located in dry, high-altitude regions. The world’s largest radio astronomy facility – the Atacama Large Millimeter/submillimeter Array (ALMA) – is in the Chilean Andes, for example. At an altitude of 5000 metres, ALMA is one of the highest observatory sites on Earth, studying light from some of the coldest objects in the Universe (as described in Mignone & Pierce-Price, 2010).

The Boomerang Nebula is a
young planetary nebula and
the coldest object found in
the Universe so far.

Image courtesy of ESA / NASA

The European Space Agencyw2 (ESA) journeyed even higher on 14 May 2009 when they launched two new space observatories. Operating beyond Earth’s atmosphere, the Herschel Space Observatory and the Planck satellite studied the cold and the distant Universe. In astronomical terms, looking at distant objects means looking back in time. When a telescope observes a galaxy 100 million light years away, we see the galaxy as it was 100 million years ago when the light was emitted. And because our Universe is expanding, the wavelength of light emitted by distant stars and galaxies is stretched even longer by the time it reaches telescopes on or near Earth – a phenomenon known as redshiftw3

The Herschel Space Observatory comprised a 3.5 m telescope for FIR and sub-mm observations, and its mission was to study the origin and evolution of stars and galaxies. The Planck satellite’s goal, on the other hand, was to study the relic radiation from the Big Bang by surveying the entire sky in sub-mm and microwave wavelengths. Until 2013, when the two missions ended, their observations provided many missing clues for astronomers.

The Herschel spacecraft in the clean room at Europe’s Spaceport in Kourou, French Guiana, prior to launch in 2009
Image courtesy of ESA-CNES-Arianespace / Optique Vidéo du CSG
The Planck spacecraft. A reflection of the Herschel spacecraft is visible in the telescope mirror.
Image courtesy of ESA / Thales

How stars are born

What stands out in observations from long-wave telescopes is the cold mixture of gas and dust that pervades galaxies. This interstellar medium is the raw material from which stars and planets are born: within the densest parts of molecular clouds, gravity causes the gas and dust to contract and fragment, eventually leading to stellar birth.

While fully fledged stars shine most brightly in ultraviolet, visible and near-infrared light (as described in Mignone & Barnes, 2014), the earliest stages in star formation are best revealed in other portions of the electromagnetic spectrum. In particular, individual proto-stars within the Milky Way and in nearby galaxies can be detected at FIR and sub-mm wavelengths.
 

The electromagnetic spectrum, with an indication of wavelengths, frequencies and energies. The Planck satellite observed wavelengths from 0.3 mm to 1 cm and the Herschel Space Observatory observed wavelengths from 60 μm to 0.6 mm.
Image courtesy of ESA / AOES Medialab
 

Observations from the Herschel telescope revealed that the interstellar medium in our galaxy is threaded with filamentary structures of gas and dust on every scale. From nearby clouds hosting tangles of filaments a few light years long to gigantic structures stretching hundreds of light years across the Milky Way’s spiral arms, these structures – only a few of which were known prior to the Herschel mission – appear to be everywhere.

Astronomers now believe that filaments are key to star formation: once the density of interstellar gas and dust in a filament exceeds a critical value, it can become gravitationally unstable, giving rise to denser concentrations of matter that might eventually form stars.

Scanning the entire sky, the Planck satellite detected thousands of cold and dense clumps where stars are born and showed that these clumps are not isolated but appear to be all linked to one other. They form huge filamentary structures across our Milky Way, resembling the smaller filaments detected by the Herschel Space Observatory.

The filamentary structure of the interstellar medium in the Galactic Plane, where most of the Milky Way’s stars are born
Image courtesy of ESA / PACS & SPIRE Consortium / S Molinari, Hi-GAL Project

The formation and evolution of galaxies 

Observing star-forming regions of the Milky Way provides a window into the processes that give birth to stars closer to Earth now. However, the Herschel mission was also instrumental in investigating the evolution of star formation in galaxies throughout the history of the cosmos.

For example, studies based on Herschel observations have indicated that most stars in the history of the Universe have formed quietly in galaxies that are considered ‘normal’ for the epoch in which we see them, rather than through violent and tumultuous events such as the mergers of galaxies.

Mergers, although spectacular, are relatively rare and of short duration. They have not dominated the cosmic history of star formation for at least the past 10 billion (1010) years. What is crucial for star formation is that galaxies have sufficient gas available to create stars, which could be provided by intergalactic streams of cold gas.

The early Universe

Ultimately, the oldest light in the history of our 13.8 billion-year-old Universe is the cosmic microwave background (CMB) – the remains of thermal radiation from the Big Bang. A fossil from the hot and dense state of the early cosmos, the CMB was released only 380 000 years after the Big Bang and is the furthest back in time that we can explore using light. It contains a wealth of information about the formation and evolution of structure in the Universe and can be detected using microwaves.

Planck was the third space mission to survey this relic of the early Universe over the entire sky, after NASA’s COBE and WMAP satellites. In unprecedented detail, the Planck satellite mapped the tiny differences in the temperature of the CMB – a mere 0.00001 K plus or minus the background temperature of 2.73 Kw4.
 

The Planck satellite mapped tiny differences in the temperature of the cosmic microwave background, which represent the seeds of today’s stars and galaxies. 
Image courtesy of ESA / Planck Collaboration
 

These minuscule fluctuations trace regions of slightly different density in the fluid that filled the early cosmos, before any stars or galaxies had formed. As such, they are the seeds around which all future cosmic structures, including the stars and galaxies of today, would later take shape.

Planck’s map is the most precise picture of the early Universe so far, confirming the standard view of the cosmos and allowing astronomers to estimate its age, expansion rate and composition with even greater accuracy.

Download

Download this article as a PDF

Web References

Resources

Institution

ESA

Author(s)

Claudia Mignone is a science writer for the European Space Agency Science Directorate (Vitrociset Belgium). 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 is the education officer for the European Space Agency Science Directorate (HE Space Operations). 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 Directorate, contact Rebecca at SciEdu@esa.int.


Review

This article demonstrates how astronomers begin to answer the most probing of questions about the origins of the Universe and how stars formed in the early (and aged) Universe.

It could be used to develop discussions based on questions such as:

  • How do astronomers use the electromagnetic spectrum?
  • What can be gained from studying the cosmic microwave background (CMB)?
  • Can the cost of scientific space missions be justified?

Robert Woodman, Ysgol Bro Gwaun, UK




License

CC-BY