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.
There are no astronomical sources of neutrinos.
The neutrinos decay before reaching the Earth.
The neutrinos interact only weakly.
2. The Chandra Observatory is an observatory for
Radio astronomy.
Neutrino astronomy.
X-Ray astronomy.
Infra-red astronomy.
3. Why are astronomers interested in different parts of the spectrum?
The results would otherwise interfere destructively.
Different parts of the spectrum contain different information.
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.
ultra-violet radiation.
visible radiation.
5. Karl Jansky was the pioneer of
radio astronomy.
optical astronomy.
infra-red astronomy.
UV astronomy.
6. A grazing incidence mirror is used to focus
visible light.
gamma rays.
x-rays.
gravitational waves.
7. Modern observatories are placed on mountains
to be able to observe X-rays
because it is cheaper to build them on mountains
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 a future planned detector in Japan
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 faster than the speed of light in a medium
a particle is travelling slower 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 attometer
1 micrometer
1 nanometer
1 millimeter
11. The Compton Gamma Ray Observatory
has grazing incidence mirrors to focus the high energy gamma rays
uses a large tank of water as a scintillation detector
has instruments to look at multiple energy bands
has imaging CCDis
12. Radio telescopes
do not require a very smooth surface.
require a very smooth surface.
need to be cooled.
operate only at night.
13. LIGO is an acronym for:
Light Incident Gravitational Observation.
Laser Interferometric Gravitational-wave Observatory.
Light Ingoing Ground Observations.
Laser Incoming Ground Observation.
14. Long Baseline Interferometry is a technique often used in radio astronomy to
image neutrinos.
remove the effect of Cerenkov radiation.
reduce the effect of light pollution in urban skies.
improve the resolution of objects.
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