Re-examining the sensitivity of JWST to decaying axion dark matter
Abstract
An eV-scale QCD axion comprising the observed dark matter (DM) abundance is expected to generate a photon line at infrared energies that would be observable or near-observable in data collected by the James Webb Space Telescope (JWST), as might more general axion-like particles (ALPs) over a broader range of masses and couplings. This has motivated a number of efforts to either forecast JWST sensitivities to a QCD axion or realize them through analyses of publicly available datasets. At present, no consensus exists; leading analyses disagree by as much as an order of magnitude in terms of axion-coupling sensitivity, implying an orders-of-magnitude discrepancy in raw flux density sensitivity, and consistency between the analyses and prior forecasts is unclear. We address these outstanding discrepancies with a bespoke data reduction and flexible nonparametric inference procedure that lead to well-controlled and robust limits on the decay of eV-scale axion DM, consistent with previously forecasted sensitivities. We further demonstrate that the strongest previously claimed sensitivities exceed those attainable by any analysis of the datasets from which they were derived. We exclude QCD axion DM for masses between 500 meV and 2.5 eV using NIRSpec data, while setting limits on ALP DM complementary to other astrophysical constraints at masses between 100 meV and 500 meV. However, we find the sensitivities to be systematically limited, and therefore unlikely to be improved upon by ongoing data collection or re-analysis unless instrumental modeling and data reduction pipelines improve considerably.
Related
- Constraints on Decaying Dark Matter with B=1 from Fermi-LAT
- Dynamics of self-gravitating halos with decaying dark matter
- Cosmological constraints on the interacting viscous dark matter and decaying vacuum energy models
- From Axion Detection to Dark Matter Astronomy
- Gravitational Instability of Cold Axion Dark Matter Beyond Minimal Coupling
BibTeX
@misc{gemmell2026reexamining,
title = {{Re-examining the sensitivity of JWST to decaying axion dark matter}},
author = {Caleb Gemmell and Christopher Dessert and Andrea Caputo and Joshua W. Foster},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.10674},
eprint = {2609.10674},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.10674},
}
RIS
TY - UNPB
TI - Re-examining the sensitivity of JWST to decaying axion dark matter
AU - Caleb Gemmell
AU - Christopher Dessert
AU - Andrea Caputo
AU - Joshua W. Foster
PY - 2026
DA - 2026/09/09
PB - arXiv
DO - 10.48550/arxiv.2609.10674
UR - https://arxiv.org/abs/2609.10674
AB - An eV-scale QCD axion comprising the observed dark matter (DM) abundance is expected to generate a photon line at infrared energies that would be observable or near-observable in data collected by the James Webb Space Telescope (JWST), as might more general axion-like particles (ALPs) over a broader range of masses and couplings. This has motivated a number of efforts to either forecast JWST sensitivities to a QCD axion or realize them through analyses of publicly available datasets. At present, no consensus exists; leading analyses disagree by as much as an order of magnitude in terms of axion-coupling sensitivity, implying an orders-of-magnitude discrepancy in raw flux density sensitivity, and consistency between the analyses and prior forecasts is unclear. We address these outstanding discrepancies with a bespoke data reduction and flexible nonparametric inference procedure that lead to well-controlled and robust limits on the decay of eV-scale axion DM, consistent with previously forecasted sensitivities. We further demonstrate that the strongest previously claimed sensitivities exceed those attainable by any analysis of the datasets from which they were derived. We exclude QCD axion DM for masses between 500 meV and 2.5 eV using NIRSpec data, while setting limits on ALP DM complementary to other astrophysical constraints at masses between 100 meV and 500 meV. However, we find the sensitivities to be systematically limited, and therefore unlikely to be improved upon by ongoing data collection or re-analysis unless instrumental modeling and data reduction pipelines improve considerably.
ER -