Galactic constraints on spinning primordial black hole dark matter from interstellar dust heating
Abstract
Primordial black holes (PBHs) are compelling dark matter candidates. PBHs with masses between 1015 and 1018 g can heat interstellar dust via Hawking radiation. Previous studies of this dust heating mechanism mostly neglected PBH spin and adopted a single dark matter halo profile. In this work, we incorporate PBH spin, which substantially enhances the emitted radiation flux, and systematically investigate the dependence of constraints on the dark matter density distribution by considering five different halo models. We compute the complete photon spectra, including both primary and secondary emissions. Our results show that, for a fixed profile and mass function, larger spin parameters yield stronger constraints on the PBH fraction fPBH. Among the halo models, the Isothermal profile gives the most stringent limits, followed by Einasto, then NFW and Moore, while the Burkert profile yields the weakest constraints. For silicate grains, which cool less efficiently than graphite, the upper limits reach 𝒪(10−4) for high spin cases. We consider both monochromatic and lognormal mass functions, and find consistent trends between them. For the lognormal case, larger values of the width σ lead to a broader mass range being excluded, in particular ruling out massive PBHs as the sole dark matter component. Our bounds are generally weaker than other existing limits, but they provide a complementary and independent constraint.
Related
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BibTeX
@misc{hu2026galactic,
title = {{Galactic constraints on spinning primordial black hole dark matter from interstellar dust heating}},
author = {Shaobin Hu and Yupeng Yang and Chengjie Sun and Zihan Li and Jiafan Sun and Yuzhu Tong and Yankun Qu and Shuangxi Yi},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2607.15028},
eprint = {2607.15028},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2607.15028},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Galactic constraints on spinning primordial black hole dark matter from interstellar dust heating
AU - Shaobin Hu
AU - Yupeng Yang
AU - Chengjie Sun
AU - Zihan Li
AU - Jiafan Sun
AU - Yuzhu Tong
AU - Yankun Qu
AU - Shuangxi Yi
PY - 2026
DA - 2026/09/14
PB - arXiv
DO - 10.48550/arxiv.2607.15028
UR - https://arxiv.org/abs/2607.15028
AB - Primordial black holes (PBHs) are compelling dark matter candidates. PBHs with masses between 10^15 and 10^18 g can heat interstellar dust via Hawking radiation. Previous studies of this dust heating mechanism mostly neglected PBH spin and adopted a single dark matter halo profile. In this work, we incorporate PBH spin, which substantially enhances the emitted radiation flux, and systematically investigate the dependence of constraints on the dark matter density distribution by considering five different halo models. We compute the complete photon spectra, including both primary and secondary emissions. Our results show that, for a fixed profile and mass function, larger spin parameters yield stronger constraints on the PBH fraction f_PBH. Among the halo models, the Isothermal profile gives the most stringent limits, followed by Einasto, then NFW and Moore, while the Burkert profile yields the weakest constraints. For silicate grains, which cool less efficiently than graphite, the upper limits reach 𝒪(10^−4) for high spin cases. We consider both monochromatic and lognormal mass functions, and find consistent trends between them. For the lognormal case, larger values of the width σ lead to a broader mass range being excluded, in particular ruling out massive PBHs as the sole dark matter component. Our bounds are generally weaker than other existing limits, but they provide a complementary and independent constraint.
ER -