Photographing black holes
You cannot see a black hole directly. You can photograph its shadow — if you build a telescope the size of the planet.
A black hole is a region where gravity bends spacetime so severely that nothing escapes — not even light. What astronomers can observe is the brilliantly hot gas trapped around it and the dark silhouette that gas outlines: the shadow of the event horizon.
Imaging that shadow requires angular resolution far beyond any single dish. The trick is interferometry at radio wavelengths: roughly eight observatories worldwide catch the same wavefront of light at the same moment, as if the Earth were one receiving dish. The Event Horizon Telescope is that array. Combined data from South Pole to Spain, synchronized with atomic clocks, produced the first shadow image of M87* and later Sagittarius A* at the center of the Milky Way.
Seeds big enough to grow
The supermassive black holes those images target — billions of solar masses — could not have formed fast enough if every seed had to come from collapsing stars that merged over cosmic time. Direct collapse offers an alternative: in the dense early universe, giant gas cores skip the star stage and collapse straight into black-hole seeds that then accrete and merge. That chain is theory constrained by timing, not a photograph.
Earth-sized interferometry turned a mathematical prediction — black holes exist, horizons are real — into a picture on a press release slide. The EHT is the entity; the shadow is the evidence; the direct-collapse story is how some of the targets got there in the first place.