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