Little red dots (LRDs) at high redshifts are compact sources with V-shaped spectra, broad emission lines, and strong Balmer jumps. The proposed model casts LRDs as supermassive analogues of the microquasar SS 433 observed at high inclination. Super-Eddington accretion, scaled up to supermassive scales, creates a self-screening inflated disk: X-ray weakness, soft optical continuum, apparent sub-Eddington luminosity, and the Balmer jump all emerge naturally. Anisotropic hard radiation from the inner disk ionizes the broad-line region, akin to the W50 nebula around SS 433. The model predicts a correlation between Balmer jump strength and line width, greater line variability relative to the continuum, that LRDs are brighter than observed, and that their low-inclination or less active cousins appear as blue dots. This viewpoint transforms LRDs into laboratories for studying rapid accretion growth at the dawn of galaxy formation.
Like a spotlight: from the side it shines dim red, but head-on it's dazzling white-blue. That's exactly how the mysterious 'little red dots' in the early universe appear—they are giant black holes turned edge-on toward us. The thick disk of scorching gas surrounding them hides the brightest radiation, letting only a soft reddish light and the glow of hydrogen through—as red as a neon sign.
Before, astronomers debated: maybe these are dense clumps of stars or the ultra-bright centers of galaxies. But the spectral fingerprint of their light, stretched by the expansion of space, revealed a familiar signature—the same as a stellar pair in the Milky Way where a black hole devours its neighbor.
🎯 The prototype of the red dots—the SS 433 system in our Galaxy—shoots out plasma jets at a quarter of the speed of light, blowing a bubble hundreds of light-years across.
🎬 In Star Wars, the color of a lightsaber signals your side of the Force; in space, the color of a distant black hole depends on the angle: red when seen edge-on, and blue when staring you straight in the face.