Herschel Space Observatory
A work in progress:
A Brief History of the Herschels: Caroline and William Herschel: The Herschels were pioneers of the systematic classification and investigation of the heavens. William Herschel was one of the first 'professional' astronomers, and discovered infrared radiation. His sister Caroline helped him to develop the modern mathematical approach to astronomy.
William, son of a musician, was born in Hanover, Germany, in 1738. He followed in his father's footsteps, joining the Hanoverian Guard band to play the oboe, but moved to England to teach music in 1755, eventually settling in Bath in 1766.
He became interested in astronomy, and started to build his own telescopes. He developed and refined Isaac Newton‘s designs to avoid problems with poor glass optics. Herschel cast and polished his own mirrors, producing ever bigger and better telescopes.
The Herschel Space Observatory is the largest infrared space telescope ever launched. With its 3.5-m primary mirror, it is four times bigger than any previous infrared space telescope and almost one and a half times larger than the Hubble Space Telescope.
Herschel - the Space Observatory: ESA’s cutting-edge space observatory, carries the largest, most powerful infrared telescope ever flown in space. A pioneering mission, it is studying the origin and evolution of stars and galaxies to help understand how the Universe came to be the way it is today.
The first observatory to cover the entire range from far-infrared to submillimetre wavelengths and bridge the two, Herschel is exploring further into the far-infrared than any previous mission, studying otherwise invisible dusty and cold regions of the cosmos, both near and far. Including the area called NGC281, or the Pacman Nebula, this is the area that SHIPs is researching for their project during 2013.
By tapping these unexploited wavelengths, Herschel is seeing phenomena beyond the reach of other observatories, and studying others at a level of detail that has not been captured before. The telescope’s primary mirror is 3.5 m in diameter, more than four times larger than any previous infrared space telescope and almost one and a half times larger than that of the Hubble Space Telescope. Its size is allowing Herschel to collect almost 20 times more light than any previous infrared space telescope.
The spacecraft carries three advanced science instruments: two cameras and a very high-resolution spectrometer. The detectors in these instruments are cooled to temperatures close to absolute zero by a sophisticated cryogenic system.
Launch: 14 May 2009 on an Ariane 5 from ESA’s Spaceport in Kourou, French Guiana. The launch took place at 13:12:02 GMT. Herschel was launched along with Planck, ESA’s microwave observatory, which is studying the Cosmic Microwave Background. (See other NITARP Projects using Planck)
Herschel's primary mirror is the telescope's light collector. It captures the light from astronomical objects and directs it towards the smaller secondary mirror. The two mirrors work together focusing the light and directing it to the instruments, where the light is detected and analysed, and the results recorded by the onboard computer.
The size of the primary mirror is the key to any telescope's sensitivity: the bigger it is, the more light it collects, and the fainter the objects it sees. It also determines the telescope's ability to distinguish fine details. The surface of the mirror is very important, too. It has to be precisely shaped and perfectly smooth, since the slightest roughness distorts the final image.
A mirror must be light and sturdy to withstand the extreme conditions of launch (where it was shaken with a force several times that of Earth’s gravity), and the low temperatures of outer space; and any bump on its surface must be less than a thousandth of a millimetre high.
This technological marvel has been constructed almost entirely of silicon carbide. The primary mirror has been made out of 12 segments brazed together to form a monolithic mirror which was machined and polished to the required thickness (about 3 mm), shape, and surface accuracy.
Vital Stats: The Herschel satellite is a tall cylinder, about 7.5 m high and 4.0 m wide, with a launch mass of around 3.4 tonnes.
| Dimensions | ~ 7.5 x 4.0 m (height x width) |
| Mass | 3.4 tonnes at launch |
| Telescope mass | 315 kg |
| Spacecraft | 3-axis stabilised |
| Telescope size | 3.5 m diameter primary mirror |
| Science data rate | 130 kbps |
| Lifetime | 3.5 years |
| Operational orbit | Lissajous orbit at an average distance of 800 000 km from L2 |
| Attitude thrusters | 12 thrusters, 20 N each |
| Solar arrays | Flat, fixed panels of triple-junction,Ga As cells, |
| Solar array area: | about 12 m2 |
| Batteries | 39 Ah Lithium ion batteries |
| Communication | 2 low gain antennae,1 medium gain antenna |
Herschel Space Telescope Science Objectives:
Herschel is set to revolutionize our understanding of the Universe. A versatile infrared space telescope, Herschel's main objective is to study relatively cool objects across the Universe: in particular the formation and evolution of stars and galaxies, and the relationship between the two.
Within our Galaxy, the mission’s main science objectives are:
To study Solar System objects such as asteroids, Kuiper belt objects, and comets. Comets are the best-preserved fossils of the early Solar System, and hold clues to the raw ingredients that formed the planets, including Earth.
To study the process of star and planet formation. Herschel is unique in its coverage of a wide range of infrared wavelengths, with which it is looking into star-forming regions in our Galaxy, to reveal for the first time different stages of early star formation and the youngest stars. The telescope is also studying circumstellar material around young stars, where astronomers believe that planets are being formed, and debris discs around more mature stars.
To study the vast reservoirs of dust and gas in our Galaxy and in other nearby galaxies. Herschel is studying in detail the physics and kinematics at work in giant clouds of gas and dust that give rise to new stars and associated planetary bodies. Herschel is also well suited to studying astrochemistry providing fundamental new insights into the complex chemistry of these molecular clouds, the wombs of future stars.
Outside our Galaxy, the mission’s main science objectives are:
To explore the influence the galactic environment has on interstellar medium physics and star formation. Most of what we have learned about the physics and chemistry of the interstellar medium, and about the processes there such as star formation has been gained by studies in our own Galaxy. With Herschel, we can carry out similar studies in relatively nearby galaxies as well. For example, studies of nearby low-metallicity galaxies can open the door to the understanding of these processes in the early Universe.
To chart the rate of star formation over cosmic time. We know that star and galaxy formation commenced relatively early after the Big Bang. We also know that when the Universe was about half its current age, star formation was much more intense than it is today. Herschel is ideal for studying infrared-dominated galaxies at the peak of star formation.
To resolve the infrared cosmic background and characterise the sources. About half the energy produced and emitted throughout cosmic history now appears as a diffuse infrared cosmic background. With its large telescope, Herschel is resolving the far-infrared background and characterising its constituent sources to a level of detail never achieved before.
What is infrared light?
The electromagnetic spectrum spans a wide range of wavelengths from very short wavelength and highly energetic gamma rays to very long wavelength and low-energy radio waves. The visible part of the spectrum is only a small portion. Infrared light is the same as the light that we can see except that the wavelength is longer and outside the range that our eyes can sense.
The electromagnetic spectrum:
Electromagnetic radiation from objects at different temperatures
In fact all objects glow (emit electromagnetic radiation), and they do this in the part of the electromagnetic spectrum that depends on their temperature. The diagram below shows how bright objects of different temperatures appear at difference wavelengths.
The Sun has a surface temperature of nearly 6000 Kelvin (where the Kelvin temperature scale is the same as the familiar Centigrade scale except that the zero degrees C is about 273 degrees Kelvin). Its radiation peaks in the visible part of the spectrum at wavelengths of about half a micron, as shown by the yellow-green line in the graph above.
Infrared radiation was discovered by William Herschel in 1800. He was studying the heating effect of different colours of light by using a prism to produce a spectrum of colours and thermometers to measure their heating effect. He noticed that the heating effect got stronger as he went from the blue end of the spectrum to the red. In a moment of inspiration, he moved the thermometer beyond the visible red end and found that the heating effect was even greater.
It is interesting that the basic technique used by Herschel to discover infrared radiation is still used in modern instruments today, including instruments on board the Herschel satellite – the only real difference is a factor a billion or so in sensitivity.
The whole region with wavelengths ranging from 1 micron to 1 mm is loosely called the “infrared”, but astronomers tend to break this up into sub-regions: the “near infrared” (from 1 to 5 microns); the “mid infrared” (5 to 30 microns), the “far infrared” (from 30 to 300 microns) and the “submillimetre” (from 300 microns to 1 mm). The exact boundaries are somewhat arbitrary, and the exact definitions can vary.
We humans, slightly warmer than room temperature, glow in the mid infrared and we’re brightest at about 10 microns wavelength (black line in the graph). These days we are all familiar with infrared imaging, which allows us to see in the dark using electronic detectors that record infrared light emitted by warm objects such as people. The pictures below show SPIRE team member Prof. Peter Ade in visible light (wavelength about 0.5 micron) and infrared light (about 10 microns).
Clouds of interstellar gas and dust that form stars are typically at temperatures of about 50 K (that’s about –220oC). They glow at far infrared wavelengths and are brightest at about 100 microns (red line in the graph above). And the universe itself is filled with radiation corresponding to a temperature of just less than 3 K – very cold indeed – with peak emission in the millimetre wavelength range (blue line in the graph above).
Clearly, depending on what it is that we want to observe, we need to look in different parts of the spectrum, and no one part will tell us everything. The Earth's atmosphere transmits well in the visible and radio regions, but it blocks out everything from gamma rays to ultraviolet and most of the infrared. So to study the Universe at those wavelengths we need to launch space-borne observatories.
