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From the Space SE question Why has the Earth-Sun libration point L1 been chosen over L2 for NEOCam to detect new NEOs?:

NEOCam

above: Profoundly not-to-scale illustration of NEOCam in an orbit around the Sun-Earth libration point L1, about 1.5 million kilometers from Earth. Presumably Sun-shield and Earth-shield block light (both infrared and visible) from the Sun and the Earth in order for the instrument to work at cold temperature necessary to detect the faint infrared light radiated from NEOs.

NEOCam

above: Infrared astronomer Amy Mainzer illustrates how asteroids warmed by the sun will stand out more brightly in the infrared compared to reflected visible light from the sun. One coffee cup is black the other white in the false-color infrared thermal image. From here.

And discussion under the answer explains the important of phase angle; they will be easier to detect if at least some fraction of the sunlit side of the asteroid is visible from the thermal infrared telescope, but I think that this is because for slowly rotating asteroids you need the sun to be hitting it to warm it up enough so that it will "glow by itself" sufficiently to be visible in the telescope.

If I understand correctly, the advantage of using thermal IR to look for NEOs is that you want to find relatively small ones that aren't previously known, and this method is more sensitive to the smallest objects.

But I am not sure WHY that is true, and also not 100% sure the source of the NIR light; is it strictly Planckian-like thermal gray-body radiation emitted from the warmed asteroid itself, or does it contain a reflected component from the Sun as well, or does that in fact dominate?

Question: Why exactly would one choose a thermal infrared (TIR) versus visible light telescope for NEO hunting? Is the TIR sought gray-body radiation from the object itself, or does it contain a significant component of or is even dominated by reflected light from the Sun?

"Bonus points" for an answer that delineates in which circular orbits and phase angles a 100 meter, albedo = 0.1 (all wavelengths) body is likely to be brighter in say 5 to 10 microns from reflected sunlight than from it's own thermal radiation. Perhaps the answer is different in the limits of zero and high rotation rate?

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OK, let's try some simple calculations. (Short answer: it's overwhelmingly the body's own thermal emission.)

The mid-IR light (let's use 10 microns, since a key design goal for NEOCam was ensuring imaging out to that wavelength) from the Sun can be approximated by emission from a 5800 K blackbody. The reflected 10-micron sunlight for an asteroid at a distance of $D$ is $L_{\rm sun} / (4 \pi D^{2})$, multiplied by the cross-sectional area of the asteroid (for simplicity, $\pi R_{\rm ast}^{2}$), multiplied by the albedo at 10 microns.

The emitted thermal radiation from the asteroid can be approximated by blackbody emission per unit surface area, multiplied by the surface area of the asteroid ($4 \pi R_{\rm ast}^2$), multiplied by the emissivity at 10 microns.

Let's assume a 100-m-radius asteroid located 1 AU from the Sun, with a temperature of 300 K.

The monochromatic (10-micron) luminosity of the Sun is $4 \pi R_{\rm sun}^{2}$ BB$(5800, 10\mu{\rm m}) \approx 2.7 \times 10^{10}$ W/Hz, where BB$(T,\lambda)$ is the monochromatic power at wavelength $\lambda$ emitted per unit surface area for a blackbody with temperature $T$. At 1 AU, a 100-m-radius asteroid could reflect a total of $\approx 3.0 \times 10^{-9}$ W/Hz at 10 microns. (Assuming albedo $= 1$, which is not possible.)

The maximum monochromatic thermal luminosity from the asteroid is $4 \pi R_{\rm ast}^{2}$ BB$(300, 10\mu{\rm m})$, which works out to be $\approx 1.3 \times 10^{-6}$ W/Hz. (Assuming emissivity $= 1$.)

OK, what about albedo and emissivity? A good estimate for the 10-micron emissivity of asteroids seems to be $\approx 0.9$, which would reduce the asteroid's thermal luminosity to $\approx 1.2 \times 10^{-6}$ W/Hz. Since emissivity + albedo $= 1$, this means the 10-micron albedo would be $\approx 0.1$ (so, a good assumption on your part), which reduces the reflected sunlight to $\approx 3.0 \times 10^{-10}$ W/Hz.

I've ignored issues like orientation geometry (how much of the reflected side of the asteroid can you actually see?) and the variation of temperature across the surface of the asteroid (higher on the dayside, lower on the nightside; less difference for faster-rotating asteroids), but these are secondary effects. The upshot is that the asteroid's thermal emission at 10 microns will be several thousand times brighter than the reflected sunlight.

Note that the amount of reflected sunlight is proportional to $R_{\rm ast}^2$, but so is the amount of emitted thermal emission, so the asteroid's size is, to first order, actually irrelevant. (Though not if you look at visible wavelength, where reflected sunlight dominates.)

Edited to add: At 5 microns, the asteroid's thermal emission will still be about a hundred times brighter than the reflected sunlight.

Edited to add: If you want to experiment with different wavelengths, asteroid temperatures, etc., I put some Python code I wrote for the computations in this Github gist.

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