Exploring the Cosmos - Class Test 3 - Mapping the Universe
1. Why are neutrinos so hard to detect in astronomical observatories?
The neutrinos interact only weakly.
The neutrinos decay before reaching the Earth.
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.
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 results would otherwise interfere destructively.
At some locations at the sky certain detectors do not work.
The different colours are nice.
4. An electromagnetic wave having a wavelength of 550 nm is:
infrared radiation.
gamma radiation.
visible radiation.
ultra-violet radiation.
5. Karl Jansky was the pioneer of
UV astronomy.
optical astronomy.
infra-red astronomy.
radio astronomy.
6. A grazing incidence mirror is used to focus
gamma rays.
visible light.
gravitational waves.
x-rays.
7. Modern observatories are placed on mountains
because it is cheaper to build them on mountains
to be able to observe X-rays
to reduce the amount of turbulent atmosphere
to get closer to the stars
8. The Super Kamiokande Neutrino observatory
is located in the Mediterranean sea
is located underground in the USA
is located underground in Japan
is a future planned detector 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
an electron recombines with an ionised atom
a particle is travelling faster than the speed of light in a medium
10. The typical sensitivity of interferometric gravitational wave detectors is of the order
1 attometer
1 micrometer
1 nanometer
1 millimeter
11. The Compton Gamma Ray Observatory
has grazing incidence mirrors to focus the high energy gamma rays
has instruments to look at multiple energy bands
uses a large tank of water as a scintillation detector
has imaging CCDis
12. Radio telescopes
require a very smooth surface.
operate only at night.
do not require a very smooth surface.
need to be cooled.
13. LIGO is an acronym for:
Light Incident Gravitational Observation.
Laser Incoming Ground Observation.
Light Ingoing Ground Observations.
Laser Interferometric Gravitational-wave Observatory.
14. Long Baseline Interferometry is a technique often used in radio astronomy to
improve the resolution of objects.
image neutrinos.
reduce the effect of light pollution in urban skies.
remove the effect of Cerenkov radiation.
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