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
Neutrino astronomy.
Radio astronomy.
Infra-red astronomy.
X-Ray astronomy.
3. Why are astronomers interested in different parts of the spectrum?
The different colours are nice.
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.
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
radio astronomy.
optical astronomy.
infra-red astronomy.
UV astronomy.
6. A grazing incidence mirror is used to focus
x-rays.
gravitational waves.
gamma rays.
visible light.
7. Modern observatories are placed on mountains
to reduce the amount of turbulent atmosphere
to get closer to the stars
because it is cheaper to build them on mountains
to be able to observe X-rays
8. The Super Kamiokande Neutrino observatory
is located in the Mediterranean sea
is located underground in Japan
is a future planned detector in Japan
is located underground in the USA
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 micrometer
1 millimeter
1 attometer
1 nanometer
11. The Compton Gamma Ray Observatory
has instruments to look at multiple energy bands
uses a large tank of water as a scintillation detector
has grazing incidence mirrors to focus the high energy gamma rays
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:
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
remove the effect of Cerenkov radiation.
image neutrinos.
improve the resolution of objects.
reduce the effect of light pollution in urban skies.
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