Very interesting Wiki article:

https://en.wikipedia.org/wiki/Extreme_ultraviolet_Imaging_Telescope

Part of the SOHO spacecraft, launched in 1995, the "EIT instrument is sensitive to light of four different wavelengths: 17.1, 19.5, 28.4, and 30.4 nm... The EIT wavelengths are of great interest to solar physicists because they are emitted by the very hot solar corona... EIT was a difficult sell to the scientific funding agencies, as it was not clear in the early 1990s that simple imaging of the corona would be scientifically useful... EIT is credited with a good fraction of the original science to come from SOHO, including the first observations of traveling wave phenomena in the corona, characterization of coronal mass ejection onset, and determination of the structure of coronal holes."

SXUV 100 Ultraviolet/Extreme Ultraviolet (UV/EUV) Photodiodes
https://www.photonicsonline.com/doc/ultravioletextreme-ultraviolet-uveuv-0001

"100% internal quantum efficiency
Photon detection to 1 nm

Opto Diode’s advanced sensor technology devices feature unparalleled quantum efficiency stability and have been successfully used in both European SOHO and Coronas-Photon projects and in American SNOE, SORCE, GOES, TIMED and EOS solar space instrumentation."

Here's my idea, which would utilize similar Extreme Ultraviolet sensors:

The distance to a galaxy 14 billion light years away is taken to be the radius of a circle. Doubling it gives the diameter, and multiplying it by Pi gives the circumference. If we take the diameter of Earth's orbit to be the base of an equilateral triangle whose apex is also at the distant galaxy, then the base of this triangle can be treated as a portion of the circumference of the circle. The angle swept by the diameter of the Earth's orbit is then a fraction of the full 360 degree circle. This first swept angle a = 2.335934E-10 arc-seconds.

For a second galaxy located 100,000 light years closer, the swept angle b = 2.335950E-10 arc-seconds.

To resolve these two objects (as having different distances) requires a precision equal to the difference between the two swept angles, or 1.668536E-15 arc-seconds...

One femto-arcsecond is the required angular precision.

Long-baseline interferometry space telescopes don't exist yet because optical sensors have not been developed that record both amplitude and polarization of incident light, as they do for radio astronomy. If such sensors existed, then space telescopes could be sent to locations millions of kilometers apart, collect light from distant space objects, transmit their data to a ground-based facility, and digitally combined to create a single extreme-high-resolution synthetic image. This would be incredibly useful for astrometrics, such as determining the actual distances to galaxies without using standard candles.

For example, two space telescopes could be placed at the Sun-Saturn L4-L5 Lagrange Points, with 16.474 AU separation. If they have sensors that detect 15 nanometer wavelengths (extreme ultraviolet light), and if they're capable of functioning as an interferometer, recording both amplitude and polarization of incident light, the effective angular resolution would be 1.527 femto-arcseconds.

This space astrometric interferometer constellation would be capable of directly measuring the distances to every galaxy in the visible universe. It would provide accurate distances across the entire range of distances currently estimated using a hodgepodge of methods that are collectively referred to as the "Cosmic Distance Ladder", and that have resulted in multiple estimates of the Cosmological Constant whose error bars do not even overlap. These errors in cosmological data have persisted for over a century, and it is high time effort was made to correct them.