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It is purely a measurement of angle - essentially how many pixels the star moved and how many arcseconds/pixel the camera+telescope is measured to have.

Previously the stars were measured one at a time with a transit telescope so the angle was directly from the encoder on the declination axis (think vertical) and a clock for the right ascension (direction the stars rotate past a fixed point as the Earth turns).

If you have telescope with a very well calibrated angle scale (pixels/arcsec). And you assume the most distance stars are fixed then you can measure how the foreground star appears to move relative to the same background stars in measurements 6months apart. You know the satellite has moved 2au around the sun and you can measure the angle difference to the star in arcsec, from the pixel movement relative to the background in the 2 images. You have then distance to the star in parsecs.

It is purely a measurement of angle - essentially how many pixels the star moved and how many arcseconds/pixel the camera+telescope is measured to have.

Previously the stars were measured one at a time with a transit telescope so the angle was directly from the encoder on the declination axis (think vertical) and a clock for the right ascension (direction the stars rotate past a fixed point as the Earth turns).

If you have telescope with a very well calibrated angle scale (pixels/arcsec). And you assume the most distance stars are fixed then you can measure how the foreground star appears to move relative to the same background stars in measurements 6months apart. You know the satellite has moved 2au around the sun and you can measure the angle difference to the star in arcsec, from the pixel movement relative to the background in the 2 images. You have then distance to the star in parsecs.

The actual technique used by Hipparcos (and I assume Gaia but I don't know the mission) is interested. The satellite has two telescopes at a fixed angle able to measure pairs of stars approximately that angle apart. As it rotates it sees lots of pairs of stars and records the relative angle. For stars close enough to measure those angles will change through the orbit.

It then performs the "mother of all simultaneous equations" (in the words of the project scientist) to work out which stars moved and which stars are fixed. It also has to solve for the constant angle between the two telescopes because this couldn't be measured well enough on the ground. The measurements are so precise they have to take into account the bending of light by Jupiter as well as the sun.

As an aside, an error during the launch meant that the final booster stage didn't separate - leaving it in the wrong orbit and with several tons of scrap metal stuck to it. The extra mass smoothed the motion of the telescope (reducing the effect of solar wind, micrometeorites etc) and led to more accurate results. A suggestion that they deliberately add several tons of scrap metal to the successor was rejected.

It is purely a measurement of angle - essentially how many pixels the star moved and how many arcseconds/pixel the camera+telescope is measured to have.

Previously the stars were measured one at a time with a transit telescope so the angle was directly from the encoder on the declination axis (think vertical) and a clock for the right ascension (direction the stars rotate past a fixed point as the Earth turns).

Now most are measured with astrometric satellites like Hipparcos and Gaia. These have telescopes with a very well calibrated angle scale (pixels/arcsec). If you assume the most distance stars are fixed then you can measure how the foreground star appears to move relative to the same background stars in measurements 6months apart. You know the satellite has moved 2au around the sun and you can measure the angle difference to the star in arcsec, from the pixel movement relative to the background in the 2 images. You have then distance to the star in parsecs.

(Sorry the previous point about 2 fixed telescopes measuring pairs of stars is an implementation detailed which complicated the answer)

It is purely a measurement of angle - essentially how many pixels the star moved and how many arcseconds/pixel the camera+telescope is measured to have.

Previously the stars were measured one at a time with a transit telescope so the angle was directly from the encoder on the declination axis (think vertical) and a clock for the right ascension (direction the stars rotate past a fixed point as the Earth turns).

If you have telescope with a very well calibrated angle scale (pixels/arcsec). And you assume the most distance stars are fixed then you can measure how the foreground star appears to move relative to the same background stars in measurements 6months apart. You know the satellite has moved 2au around the sun and you can measure the angle difference to the star in arcsec, from the pixel movement relative to the background in the 2 images. You have then distance to the star in parsecs.

It is purely a measurement of angle - essentially how many pixels the star moved and how many arcseconds/pixel the camera+telescope is measured to have.

Previously the stars were measured one at a time with a transit telescope so the angle was directly from the encoder on the declination axis (think vertical) and a clock for the right ascension (direction the stars rotate past a fixed point as the Earth turns).

Now most are measured with astrometric satelites like Hipparcos and Gaia. These have two telescopes at a fixed (and very well known) angle to each other. These measure the angle between multiple combinations pairs of stars repeatedly as the telescope rotates.

It is purely a measurement of angle - essentially how many pixels the star moved and how many arcseconds/pixel the camera+telescope is measured to have.

Previously the stars were measured one at a time with a transit telescope so the angle was directly from the encoder on the declination axis (think vertical) and a clock for the right ascension (direction the stars rotate past a fixed point as the Earth turns).

Now most are measured with astrometric satellites like Hipparcos and Gaia. These have telescopes with a very well calibrated angle scale (pixels/arcsec). If you assume the most distance stars are fixed then you can measure how the foreground star appears to move relative to the same background stars in measurements 6months apart. You know the satellite has moved 2au around the sun and you can measure the angle difference to the star in arcsec, from the pixel movement relative to the background in the 2 images. You have then distance to the star in parsecs.

(Sorry the previous point about 2 fixed telescopes measuring pairs of stars is an implementation detailed which complicated the answer)