Supermassive Dark Stars and their remnants as a possible solution to three recent cosmic dawn puzzles

Cosmin Ilie, Jillian Paulin, Andreea Petric, Katherine Freese

First listed 2025-11-11 | Last updated 2026-01-05

Abstract

The James Webb Space Telescope (JWST) has begun to revolutionize our view of the Cosmos. The discovery of Blue Monsters (i.e., ultra-compact yet very bright high-z galaxies) and the Little Red Dots (i.e., very compact dustless strong Balmer break cosmic dawn sources) pose significant challenges to pre-JWST era models of the assembly of first stars and galaxies. In addition, JWST data further strengthen the problem posed by the origin of the supermassive black holes that power the most distant quasars observed. Stars powered by Dark Matter annihilation (i.e., Dark Stars) can form out of primordial gas clouds during the cosmic dawn era and subsequently might grow via accretion and become supermassive. In this paper we argue that Supermassive Dark Stars (SMDSs) offer natural solutions to the three puzzles mentioned above.

Short digest

This paper argues that Supermassive Dark Stars (SMDSs), powered by dark‑matter annihilation and capable of rapid, dust‑free accretion, can simultaneously explain JWST “Blue Monsters,” Little Red Dots, and the existence of early supermassive black holes. The authors present their strongest observational hint so far: a He II 2511 Å absorption feature in the spectrum of JADES-GS-z13-0. They outline how collapsing SMDSs furnish heavy BH seeds that can plausibly grow into the high‑z quasars (e.g., UHZ1) without prolonged super‑Eddington phases. They also propose that SMDS remnants embedded in dense gas envelopes naturally yield LRD‑like quasi‑stars that are UV‑weak and X‑ray dark, consistent with MIRI/ALMA non‑detections.

Key figures to inspect

• Spectrum of JADES-GS-z13-0 around rest 2511 Å: verify the He II absorption identification, equivalent width, S/N, and continuum shape relative to SMDS model expectations.
• SMDS spectral energy distributions and color tracks: inspect predicted Balmer‑break strength and dust‑free continua versus z>10 galaxy/QSO templates to see how SMDSs reproduce Blue Monster photometry.
• Size–luminosity and comoving number density comparison: check whether SMDS luminosities and compact radii match the observed Blue Monster locus and reported abundances.
• BH growth tracks from SMDS collapse seeds: follow seed masses and accretion assumptions to reach UHZ1, J0313‑1806, J1342+0928, and J1007+2115 by the observed redshifts.
• LRD quasi‑star configuration: look for a schematic or radiative‑transfer result showing a BH plus dense envelope that suppresses UV/X‑ray output and matches MIRI/ALMA non‑detections.