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