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Little Red Dots from ultra-strongly self-interacting dark matter
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DOI：10.1088/1475-7516/2026/05/003.png)
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Abstract
En 中文
We investigate the possibility that the recently identified population of highredshift, obscured quasars known as Little Red Dots (LRDs) originates from early black hole seed formation driven by ultra-strongly self-interacting dark matter (uSIDM). In this framework, dark matter halos undergo gravothermal core collapse due to large self-interaction cross sections, resulting in the rapid formation of massive black hole (BH) seeds with masses greater than or similar to 10(5) M-circle dot at redshifts z greater than or similar to 5. We develop a semi-analytic model that tracks the evolution of the dark matter halo population, the redshift of collapse z(coll), and the corresponding BH mass function. Black hole growth is modeled stochastically via a log-normal Eddington ratio distribution and a finite duty cycle. We find that the uSIDM scenario naturally reproduces key observed properties of LRDs, including their abundance, compactness, and characteristic BH masses, while offering a mechanism for early, obscured black hole formation that is difficult to achieve in standard CDM-based models. The predicted SMBH mass function at z similar to 5 shows excellent agreement with LRD observational data and SIDM merger-tree simulations, particularly at the high-mass end (m(BH)greater than or similar to 10(7) M-circle dot). These results suggest that LRDs may serve as powerful observational tracers of exotic dark sector physics and that SMBH formation in the early universe could be significantly shaped by non-gravitational dark matter interactions.
Keywords:
dark matter theory
massive black holes
semi-analytic modeling
Statistical sampling techniques
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