This code computes spectral energy distributions (SEDs) for accreting supermassive black holes, with an emphasis on quasars and active galactic nuclei (AGNs). The main goal is to connect the physics of black hole accretion disks to the ionizing continua that illuminate and regulate line-emitting gas in the broad-line region (BLR).
The baseline SED framework follows the AGN disk models of Kubota & Done (2018, 2019), which include emission from the outer disk, warm Comptonizing region, and hot X-ray corona. In this implementation, we modify the underlying effective temperature profile by solving for the slim-disk structure, allowing the SED to capture changes associated with high accretion rates and geometrically thick inner disks.
This model was used in Wu et al. (2026), which studies how slim-disk structure, anisotropic illumination, and self-shadowing affect the BLR size-luminosity relation, especially for high-accretion-rate AGNs.
If you use this code, please cite:
- Wu et al. (2026), arXiv:2606.00992
- Kubota & Done (2018, 2019)