Which of the blocked radiation windows will (mostly) open if one where to observe from the surface of Mars, instead of the Earth?

Question

Earth’s atmosphere is composed of about 78 percent nitrogen, 21 percent oxygen, 0.9 percent argon, and 0.1 percent other gases. Trace amounts of carbon dioxide, methane, water vapor, and neon are some of the other gases that make up the remaining 0.1 percent.

Mars' atmosphere is 95% carbon dioxide, 3% nitrogen, 1.6% argon, and it has traces of oxygen, carbon monoxide, water, methane, and other gases, along with a lot of dust.

My QUESTIONS:

1) But I am sure there is a lot of absortion of EM radiation in the atmosphere, due to water vapor, so is this absorption really caused by these trace amounts of water vapor?

2) If one were to make observations from the surface of Mars instead of that of the Earth, what radiation windows will (mostly) open ?

I know that on the Earth execpt for the radio and visible spectrum which are open, the other EM windows of the spectrum are closed due to absorption, diffraction, Ionization and photodissociation whcih are the 4 main ways in which EM radiations interacts with the Earth 's atmosphere. I am basing this claim on the following picture:

My guess is that the gamma ray and UV should open, because there is no ozone, which is what blocks them right? I also thought about IF, becuase I though there was no water in Mars's atmosphere. But both Earth and Mars atmospheres contain traces of water so now I am not sure that the IR window would really open, maybe just like in the Earth there s still absortion.

Answer 1

Question 1:

From Tokunaga (2000):The major atmospheric absorbers [in the infrared] are H₂O [and OH], CO₂, N₂O, CH₄, and O₃.

Question 2:

X- and gamma rays: These would still be strongly attenuated even by a thin atmosphere. It would be better to go with one of @Darth Pseudonym's options in the comments.

Ultraviolet: I did a back of the envelope calculation that the total column density of ozone above the Earth's surface is 100x more than at Mars. So there could generally be a 100x improvement in UV transparency at Mars, although this would vary with UV wavelength.

Visible: Both atmospheres are transparent, but with Mars' lower surface temperature and lower pressure, there would be less distortion. Adaptive optics would not need to work as hard, and you could get sharper images.

Infrared: Roman (2023) provided a nice plot of atmospheric tranmission, calculated for Cerro Paranal in Chile (high transmission is good, so it's the light-blue regions where the atmosphere is transparent enough for astronomy):

So it looks like with low H₂O, a window might open up around 7 µm, and the sky would be better at 18+ µm as well.

But the 15-µm region would not improve. Although Mars has a thinner atmosphere, that atmosphere is full of CO₂, while the Earth has only about 420 ppm of CO₂. That means the total column density of CO₂ is roughly 30x greater on Mars than on Earth.

Submillimeter: Water vapor dominates in this region. This plot from Tokunaga (2000) compares Kitt Peak (altitude 2 km) and Mauna Kea (altitude 4 km):

The "w" in the plot is the column density of water in the atmosphere in precipitable millimeters, that is, if you extracted all the water in the whole vertical column, it would make a 1-mm or 5-mm layer of liquid water. For Mars, that value is typically in the range of 10 precipitable µm, so 100x less than the Mauna Kea value in the plot (which is already 5x better than Kitt Peak). So there should be some nice far-IR/submillimeter windows opening up.