From “The Cliff” to “Virgil”: Mapping the Spectral Diversity of Little Red Dots with JWST/NIRSpec

Abstract One of JWST’s most unexpected discoveries is the emergence of “Little Red Dots” (LRDs), compact sources at z ≳ 3 with blue rest-frame UV continua, red optical slopes, and broad Balmer emission lines that challenge standard models and suggest early, unusual active galactic nuclei (AGNs). Using a comprehensive photometric selection and public NIRSpec/PRISM spectroscopy across six JWST deep fields, we identify a large sample of 118 LRDs with high-signal-to-noise-ratio spectra, enabling a population-wide analysis of their UV–optical continuum and lines. We find clear correlations between rest-frame UV–optical color ([0.3−0.9 μ m]) and slopes; bluer LRDs have blue UV slopes ( β ν ,UV ∼ 0.3) and red optical slopes, while redder LRDs exhibit redder UV slopes ( β ν ,UV ∼ 1.1). The continuum shape shows a similar trend; redder LRDs display prominent Balmer breaks and curvature, while bluer LRDs follow power-law-like optical spectral energy distributions. From literature compilations, ∼60% of known broad-line AGNs satisfy our LRD criteria, and up to 90% of LRDs show broad Balmer lines. Emission line diagnostics reveal a shift from high H α /H β and low [O iii ] λ 5007/H β in redder LRDs to the opposite in bluer ones, along with stronger narrow-line equivalent widths, suggesting a transition from AGN- to host-dominated emission. We fit the spectra with a two-component model combining a gas-enshrouded black hole (BH) and a galaxy host. Redder LRDs require higher-luminosity, unreddened BHs and modestly reddened hosts; bluer LRDs require lower-luminosity, reddened BHs and dust-free galaxies. This framework reproduces the diversity in colors and spectral shape by varying BH luminosity, obscuration, and BH-to-host luminosity ratio.