X-ray (2–10 keV) bolometric correction vs. bolometric luminosity for the standard population of broad line quasars (slate blue filled circles; Lusso et al. 2020) and the new population of X-ray silent, broad line AGNs discovered by JWST at z >  4 (Maiolino et al. 2025). The latter is shown with red triangles, which represent lower limits to the bolometric correction. The cyan area shows the relation found by Duras et al. (2020) for broad line AGNs with its dispersion. Similarly to the new JWST population, the BiRD is undetected in the X-rays (purple triangle), and its X-ray bolometric correction is at least 30 times larger than expected in standard quasars. The lower limits to the bolometric correction for the Rosetta Stone (in plum) and RUBIES-BLAGN-1 (pink triangle) are also shown for comparison.