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.
Neutrinos are absorbed in the upper atmosphere.
There are no astronomical sources of neutrinos.
2. The Chandra Observatory is an observatory for
Radio astronomy.
Infra-red astronomy.
Neutrino astronomy.
X-Ray 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:
visible radiation.
infrared radiation.
ultra-violet radiation.
gamma radiation.
5. Karl Jansky was the pioneer of
infra-red astronomy.
radio astronomy.
UV astronomy.
optical astronomy.
6. A grazing incidence mirror is used to focus
visible light.
gravitational waves.
gamma rays.
x-rays.
7. Modern observatories are placed on mountains
to be able to observe X-rays
to reduce the amount of turbulent atmosphere
to get closer to the stars
because it is cheaper to build them on mountains
8. The Super Kamiokande Neutrino observatory
is located underground in Japan
is located in the Mediterranean sea
is located underground in the USA
is a future planned detector in Japan
9. Cerenkov radiation is given off when
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
an electron recombines with an ionised atom
10. The typical sensitivity of interferometric gravitational wave detectors is of the order
1 micrometer
1 attometer
1 millimeter
1 nanometer
11. The Compton Gamma Ray Observatory
uses a large tank of water as a scintillation detector
has grazing incidence mirrors to focus the high energy gamma rays
has imaging CCDis
has instruments to look at multiple energy bands
12. Radio telescopes
do not require a very smooth surface.
require a very smooth surface.
operate only at night.
need to be cooled.
13. LIGO is an acronym for:
Laser Incoming Ground Observation.
Light Incident Gravitational Observation.
Laser Interferometric Gravitational-wave Observatory.
Light Ingoing Ground Observations.
14. Long Baseline Interferometry is a technique often used in radio astronomy to
reduce the effect of light pollution in urban skies.
remove the effect of Cerenkov radiation.
improve the resolution of objects.
image neutrinos.
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