The Infrared Advantage: Seeing Through Cosmic Dust Quiz

If a Bok Globule is a very concentrated cloud of dust and gas, then it is completely opaque to visible light; if we want to see if a star is forming inside, then we must use infrared sensors to detect the thermal glow of the infant star.

If a facility is optimized for Infrared, Sub-millimeter, or Millimeter wavelengths, then it is built to see through dust or see the dust itself; Hubble is primarily a visible light telescope, though it has limited IR capabilities.

If a protostar is still surrounded by its birth cocoon of dust, then visible photons cannot escape; if the protostar's heat warms the surrounding dust and the IR light escapes, then the star will appear as a bright source only in the infrared image.

If the path of a photon is changed by an interaction with a physical particle without being completely absorbed, then the behavior is defined as scattering.

If infrared sensors detect heat, and if the telescope's own electronics generate heat, then the image will be contaminated with noise. If we take a photo with the shutter closed (dark frame) and subtract it from the data, then we can isolate the true signal from space.

If interstellar dust is formed in the cooling envelopes of aging stars, and if those stars produce heavy elements like silicon and carbon, then the resulting dust grains will be composed of rocky silicates and soot-like carbon.

If the optical depth (tau) is high, then the number of photons reaching the detector is exponentially reduced; if the reduction is wavelength-dependent, then the blue end is lost first (reddening) and eventually all visible light is blocked.

If water vapor and CO2 in the Earth's atmosphere are highly efficient at absorbing infrared photons, then ground-based IR observations are severely limited. If we place the telescope in space, then it has a clear, unobstructed view of all infrared wavelengths.

If astronomers measure the amount of extinction per unit of distance to map the 3D distribution of dust, and if the standard scientific unit for galactic distance is the parsec, then that is the correct term.

If infrared light is the primary spectrum used to resolve the internal structures of dusty regions with high detail, then "dust penetration" is most commonly associated with infrared. While radio waves also pass through dust, they are generally used to study gas rather than the stars themselves.

If the size of a dust particle is comparable to the wavelength of incoming radiation, then the radiation will be scattered (Mie scattering). If visible light wavelengths (0.4-0.7 micrometers) match the size of interstellar dust grains, then those grains will block visible light while allowing longer wavelengths to pass.

If stars form from the collapse of cold, dusty gas clouds, then their earliest stages are physically hidden from visible light telescopes. If infrared light allows us to see through these nurseries, then we can study how stars and planets (disks) actually form.

If astronomers use specialized filters to look through "holes" in Earth's atmospheric water vapor, and if these filters operate between 1.2 and 2.2 micrometers, then they are working in the near-infrared region.

If we want to calculate how much light a dust cloud is blocking, we first need to know the star's intrinsic brightness. If the Inverse Square Law tells us how bright the star should be based on distance alone, then any extra dimming measured can be attributed to dust extinction.

If the Galactic Center is obscured by approximately 30 magnitudes of visual extinction (due to dust), then only 1 out of every trillion visible photons reaches Earth. If infrared light can penetrate this dust, then we can see the orbits of stars around the central black hole (Sgr A*).

If a dust grain absorbs high-energy visible or UV light, it heats up; if the grain reaches a specific temperature, it must radiate that energy back into space to maintain equilibrium. According to Wien's Law, cool objects like dust (30-100 K) emit radiation in the Far-Infrared.

If JWST is designed to see the earliest stars and through dust clouds, then it must operate in the infrared; if its primary instruments like NIRCam and MIRI cover these specific ranges, then Near-IR and Mid-IR are the correct wavelengths.

If starlight must pass through a medium that removes a portion of its photons, then the total intensity of the light is reduced. If this reduction is caused by the interstellar medium, then the scientific term for the effect is extinction.

If dense molecular clouds are opaque to visible and UV light due to high dust density, and if infrared radiation has wavelengths long enough to navigate around these particles, then infrared is the primary tool for observing stars shrouded in these regions.

If scattering efficiency is inversely proportional to the wavelength (Rayleigh scattering), then shorter wavelengths like blue light are diverted by dust more than longer wavelengths like red light. If the blue light is removed, then the remaining light from the star appears shifted toward the red end of the spectrum.