Two telescopes looked at the same patch of sky. They saw almost entirely different stars.
W51 is a giant molecular cloud 17,000 light years away, roughly 350 light years across, where stars started forming within the past million years and are still forming. It contains O-type stars: the rarest class on the main sequence, with surface temperatures above 30,000 kelvin. These stars form deep inside molecular clouds where visible light cannot escape. The evidence existed as radio signatures and theoretical models until the James Webb Space Telescope's infrared cameras showed what had been hiding.
"With optical and ground-based infrared telescopes, we cannot see through the dust to see the young stars. Now we can," Adam Ginsburg, a professor of astronomy at the University of Florida and co-author of the paper, said in a UF press release. Taehwa Yoo, the paper's first author and a doctoral candidate at UF, led the observations. The Near-Infrared Camera (NIRCam) observations ran September 8, 2024; the Mid-Infrared Instrument (MIRI) follow-up ran May 6, 2025. The paper, published in The Astronomical Journal (DOI: 10.3847/1538-3881/ae40b7), lists Yoo as first author and Ginsburg as co-author.
The observations solve one puzzle and create a larger one. Within W51-A, two neighboring protoclusters are in different states. W51-IRS2 appears to be suppressing further gas infall onto itself, essentially choking its own supply of raw material. W51-E is still accreting gas. The same physical process, different outcomes, side by side for the first time.
The larger puzzle is what the telescopes are not agreeing on. Comparing JWST's infrared detections to existing Atacama Large Millimeter/submillimeter Array (ALMA) radio observations, the team found that only 24 sources (roughly 10 percent of ALMA's detections in the same field) appear in both datasets. The rest are too embedded or too cool for JWST's infrared instruments to detect.
This is the number worth sitting with. The two most capable observatories in existence are looking at the same star-forming region and finding almost entirely different stellar populations. They are not seeing the same things through different windows. They are seeing different things because the physical conditions they are sensitive to do not overlap as much as previously assumed. That 10 percent overlap figure is itself a result: it means existing radio catalogs of embedded star-forming regions systematically undercount the full stellar population when cross-referenced with infrared data.
The practical implication is that any single-instrument survey of a star-forming region is capturing a subset, not a census. Both ALMA and JWST are right about what they see. Neither is wrong. But together they reveal how much was missing from viewing the problem through only one lens.
O-type stars eventually explode as supernovae, seeding their surroundings with heavy elements and triggering new rounds of star formation. Watching that process begin is harder than watching it end. JWST, which launched in December 2021 and began science operations in July 2022, has now provided the clearest view yet of where it starts.
The initial signal for this story came via Space.com.