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Quizzes > Science > Earth & Space Science

Think You Know Cosmology? Take the Quiz!

Take this cosmic quiz and ace your cosmology test!

Editorial: Review CompletedCreated By: Amaury Burgos GarciaUpdated Aug 25, 2025
Difficulty: Moderate
2-5mins
Learning OutcomesCheat Sheet
Paper art style cosmic scene with planets stars galaxies dark matter swirl and big bang burst on dark blue background

This cosmology quiz helps you check how well you understand the Big Bang, dark matter, cosmic expansion, and more. Play to spot gaps and pick up quick facts. When you're done, explore Dark Matter & Dark Energy or try Astrophysics next.

The Big Bang model describes the universe as expanding from a hot, dense initial state.
True
False
undefined
What is the approximate temperature of the cosmic microwave background today?
0.27 K
0.027 K
2.7 K
27 K
undefined
Hubble–Lemaître law relates a galaxy's recessional velocity to its
angular size
distance
metallicity
mass
undefined
Dark matter is inferred primarily because visible matter alone cannot explain
solar flares
galaxy rotation curves
planetary orbits
stellar spectra
undefined
Type Ia supernovae are used in cosmology as
standard rulers
neutrino detectors
timekeeping pulsars
standard candles
undefined
Recombination allowed photons to travel freely because
stars began to shine
electrons combined with nuclei to form neutral atoms
gravity was switched off
photons gained mass
undefined
Baryon acoustic oscillations serve as a
probe of stellar interiors
standard ruler in the galaxy distribution
standard candle for supernovae
gravitational lensing calibrator
undefined
Big Bang nucleosynthesis primarily produced significant amounts of
hydrogen, helium, and trace lithium
carbon and oxygen
iron and nickel
uranium and thorium
undefined
Gravitational lensing can be used to map dark matter in galaxy clusters.
True
False
undefined
Flat galaxy rotation curves at large radii indicate
stars move on parabolic orbits
black holes dominate all galactic mass
the presence of extended dark matter halos
no need for gravity
undefined
The Integrated Sachs–Wolfe effect arises when CMB photons travel through gravitational potentials that
convert photons into neutrinos
trap photons permanently
are perfectly static
evolve with time due to dark energy or curvature
undefined
The Sunyaev–Zel'dovich effect is caused by
gravitational redshift near black holes
atomic absorption in stellar atmospheres
inverse Compton scattering of CMB photons by hot electrons in galaxy clusters
synchrotron radiation from pulsars
undefined
The first acoustic peak in the CMB power spectrum corresponds roughly to an angular scale of about
90 degrees
0.01 degrees
10 degrees
1 degree
undefined
The BAO scale imprinted in the galaxy distribution is approximately
150 kpc
1 AU
150 Mpc (comoving)
1 pc
undefined
Cosmic variance limits the precision with which we can measure large-scale CMB modes.
False
True
undefined
Primordial tensor fluctuations would imprint primarily which CMB polarization pattern at large angular scales?
Circular polarization
E-modes only
B-modes
Unpolarized intensity
undefined
The nearly scale-invariant spectrum of primordial curvature perturbations is often parametrized by the scalar spectral index n_s close to
much greater than 3
exactly 0
exactly 2
but slightly less than 1
undefined
The Sachs–Wolfe effect on large angular scales is primarily due to
gravitational redshift of photons climbing out of potential wells at last scattering
Doppler boosting by Earth's motion
atomic line absorption in our atmosphere
synchrotron emission from galaxies
undefined
In ΛCDM, cold dark matter is assumed to be
faster than light
composed of photons
non-relativistic during structure formation
hotter than the CMB at all times
undefined
The Press–Schechter formalism provides a way to predict
stellar lifetimes from mass
nuclear reaction rates
planetary transits
the halo mass function from the initial density field
undefined
0

Study Outcomes

  1. Understand Core Cosmology Concepts -

    Gain a solid grasp of fundamental ideas like dark matter, cosmic expansion, and the Big Bang as presented in this cosmology quiz.

  2. Identify Celestial Phenomena -

    Recognize and distinguish key universe features - galaxies, nebulae, and black holes - through targeted questions in the cosmic quiz.

  3. Analyze Evidence for Dark Matter -

    Examine the observational clues and scientific reasoning behind dark matter's role in cosmic structure via our interactive cosmology trivia.

  4. Evaluate Big Bang Theory Basics -

    Assess the timeline, supporting data, and major debates surrounding the Big Bang by engaging with our concise universe quiz questions.

  5. Apply Cosmological Principles -

    Use learned concepts to solve real-world cosmology test scenarios, reinforcing your understanding and critical thinking skills.

  6. Measure Your Universe IQ -

    Track your quiz performance to identify strengths and areas for further exploration, turning this cosmology test into a personalized learning tool.

Cheat Sheet

  1. Hubble's Law and Universal Expansion -

    Review the relation v = H₀ × d (velocity equals Hubble constant times distance), which underpins the expanding universe concept. Remember H₀ ≈ 70 km/s/Mpc and use the mnemonic "Hubble's Horizon" to recall how more distant galaxies recede faster. This formula often appears in a cosmology quiz when interpreting redshift data.

  2. Cosmic Microwave Background (CMB) Radiation -

    Understand that the CMB is relic radiation from ~380,000 years after the Big Bang, observed today at ~2.7 K. Data from COBE, WMAP, and Planck missions (NASA/ESA) map tiny temperature fluctuations that seed galaxy formation. In cosmology trivia, you may be asked about its blackbody spectrum or angular power spectrum peaks.

  3. Dark Matter Evidence -

    Familiarize yourself with galaxy rotation curves showing flat orbital speeds at large radii, indicating unseen mass (Rubin et al., 1970s). Recall gravitational lensing examples like the Bullet Cluster, where lensing maps (Hubble Space Telescope) align mass with dark matter. A handy phrase is "Mass hides in plain sight" to remember these observational pillars on a universe quiz.

  4. Cosmic Inflation Theory -

    Inflation posits a brief period of exponential expansion (Guth 1981; Linde 1983) that solves the horizon and flatness problems. Use the formula a(t) ∝ e^(Ht) to represent scale factor growth, and remember "rapid stretch smooths rough patches." Quiz questions often ask how inflation explains the uniformity of the CMB across vast regions.

  5. Dark Energy and ΛCDM Model -

    Dark energy drives accelerated expansion, represented by the cosmological constant Λ in the Friedmann equation: H² = (8πG/3)ϝ + Λ/3 - k/a². The ΛCDM model (Planck Collaboration) successfully fits supernova and CMB data. When tackling a universe quiz, note that ΩΛ ≈ 0.7 denotes dark energy's share of total cosmic density.

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