At the North Pole, the analemma would be completely upright (an 8 with the small loop at the top), and you’d only be able to see the top half of it. If you headed south, once you drop below the Arctic Circle, you’d be able to see the entire analemma, and it would start to tilt to one side the closer to the horizon you photographed it. By time you got down to the equator, the analemma would be completely horizontal. Then, as you continued to go south, it would continue rotating so that the small loop was beneath the large loop in the sky. Once you crossed the Antarctic Circle, the analemma, now nearly completely inverted, would start to disappear, until only the lower 50% was visible from the South Pole.
As winter transitions into summer, that arc gets higher and higher in the sky, peaking at its highest point during the summer solstice, and then declining back down to its low point as summer transitions back into the winter. The Earth’s axial tilt — responsible for this phenomenon — explains why the Sun moves along this direction (drawn in white) of the analemma:

So on a planet like Mercury, where the axial tilt is less than one degree, the Sun’s position in the sky doesn’t change from day-to-day, and so an analemma on Mercury is just a single point! But something else must be going on; Mars, which has almost the same axial tilt as Earth, has an analemma that looks like this:

If the Earth’s orbit were a perfect circle, and the Earth always moved at the same speed around the Sun, our analemma would simply be a line and the Sun would simply move along that line, reaching one end on the Summer Solstice and the other end on the Winter Solstice. But, no planet’s orbit is a perfect circle.
When a planet (with an elliptical orbit) is closest to the Sun (perihelion), it moves fastest. When a planet is farthest from the Sun (aphelion), it moves more slowly.

What this means is that the Earth moves different amounts through the sky as it rotates, which is important. You see, the amount of time it takes the Earth to rotate once is not 24 hours. It actually takes 23 hours, 56 minutes, and 4 seconds. Why are our days 24 hours, then? Because, on average, the Earth revolving around the Sun adds an extra 3 minutes and 56 seconds to each day. But during some days (like in March), it appears that the Sun is moving more slowly, so that 24 hours later — what we record as a day — the Sun has shifted its position in the sky.
The Earth’s axial tilt also contributes to the Sun’s apparent motion in not just the up-down direction, but also in the “side-to-side” motion. The following (1-3) contribute to the shape while producing the sum (4).
1. the effect of eccentricity (what I talked about above) [top left image below]
2. the effect of axial tilt (something that most planets have) [top right image below]
3. the combined effects of both of these (which gives us our equation of time) [bottom left image below]
4. the overall path of the analemma, which aligns neatly with the equation of time. [bottom right image below]
