Exploring the Cosmos - Class Test 3 - Mapping the Universe
1. Why are neutrinos so hard to detect in astronomical observatories?
The neutrinos decay before reaching the Earth.
The neutrinos interact only weakly.
There are no astronomical sources of neutrinos.
Neutrinos are absorbed in the upper atmosphere.
2. The Chandra Observatory is an observatory for
X-Ray astronomy.
Radio astronomy.
Neutrino astronomy.
Infra-red astronomy.
3. Why are astronomers interested in different parts of the spectrum?
The different colours are nice.
At some locations at the sky certain detectors do not work.
Different parts of the spectrum contain different information.
The results would otherwise interfere destructively.
4. An electromagnetic wave having a wavelength of 550 nm is:
infrared radiation.
ultra-violet radiation.
visible radiation.
gamma radiation.
5. Karl Jansky was the pioneer of
radio astronomy.
UV astronomy.
infra-red astronomy.
optical astronomy.
6. A grazing incidence mirror is used to focus
x-rays.
gamma rays.
gravitational waves.
visible light.
7. Modern observatories are placed on mountains
because it is cheaper to build them on mountains
to be able to observe X-rays
to get closer to the stars
to reduce the amount of turbulent atmosphere
8. The Super Kamiokande Neutrino observatory
is located in the Mediterranean sea
is located underground in the USA
is a future planned detector in Japan
is located underground in Japan
9. Cerenkov radiation is given off when
an electron is ionised from an atom
a particle is travelling slower than the speed of light in a medium
a particle is travelling faster than the speed of light in a medium
an electron recombines with an ionised atom
10. The typical sensitivity of interferometric gravitational wave detectors is of the order
1 micrometer
1 millimeter
1 attometer
1 nanometer
11. The Compton Gamma Ray Observatory
has imaging CCDis
has instruments to look at multiple energy bands
uses a large tank of water as a scintillation detector
has grazing incidence mirrors to focus the high energy gamma rays
12. Radio telescopes
require a very smooth surface.
do not require a very smooth surface.
need to be cooled.
operate only at night.
13. LIGO is an acronym for:
Light Incident Gravitational Observation.
Laser Incoming Ground Observation.
Laser Interferometric Gravitational-wave Observatory.
Light Ingoing Ground Observations.
14. Long Baseline Interferometry is a technique often used in radio astronomy to
remove the effect of Cerenkov radiation.
image neutrinos.
reduce the effect of light pollution in urban skies.
improve the resolution of objects.
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