Detecting the Axion-Photon Conversion Background
Abstract
The potential to detect axion dark matter through astrophysical processes has shown high promise in recent years. We therefore expand on previous work studying the axion-to-photon conversion efficacy of neutron stars and the interstellar medium (ISM) in this endeavor, respectively. For neutron stars (NS), we examine the possibility of a background signal emanating from all NS magnetospheres in the galaxy. Using a heuristic Galactic model, we find a significant background signal emanating from such magnetospheres in the Milky Way. This signal, while weak in absolute power (≳ 1 mJy sr−1 from the Galactic Center, at 2 GHz), can be detected through new statistical techniques with current instrumentation like the Atacama Large Millimeter Array (ALMA) at high radio frequencies (200 - 950 GHz). These techniques make use of higher order statistics like spectrally-limited (∼ 300 km s−1) increases in confusion noise levels and kurtoses of survey images, and also show promise for general population estimation techniques. For the ISM, we consider Primakoff processes between free electrons and axions, and derive typical signal strengths of 10−15 Jy sr−1 · ma/eV, with a local, cosmological upper bound of 10−8 Jy sr−1 · ma/eV. Hence, we find that any diffuse axion signal from the ISM and other, large-scale, astrophysical plasmas to be too weak to be detected with modern technologies. We therefore find that the best avenue towards detecting a potential quantum chromodynamics (QCD) axion dark-matter particle is through the radio imaging of large swaths of the Galactic Center and other regions where we expect large numbers of pulsars and neutron stars.
Versions
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BibTeX
@misc{weber2026detecting,
title = {{Detecting the Axion-Photon Conversion Background}},
author = {Felix Weber and Vikram Ravi},
howpublished = {arXiv},
year = {2026},
month = may,
doi = {10.48550/arxiv.2605.15175},
eprint = {2605.15175},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2605.15175},
note = {CC BY-NC-ND 4.0},
}
RIS
TY - UNPB
TI - Detecting the Axion-Photon Conversion Background
AU - Felix Weber
AU - Vikram Ravi
PY - 2026
DA - 2026/05/14
PB - arXiv
DO - 10.48550/arxiv.2605.15175
UR - https://arxiv.org/abs/2605.15175
AB - The potential to detect axion dark matter through astrophysical processes has shown high promise in recent years. We therefore expand on previous work studying the axion-to-photon conversion efficacy of neutron stars and the interstellar medium (ISM) in this endeavor, respectively. For neutron stars (NS), we examine the possibility of a background signal emanating from all NS magnetospheres in the galaxy. Using a heuristic Galactic model, we find a significant background signal emanating from such magnetospheres in the Milky Way. This signal, while weak in absolute power (≳ 1 mJy sr^−1 from the Galactic Center, at 2 GHz), can be detected through new statistical techniques with current instrumentation like the Atacama Large Millimeter Array (ALMA) at high radio frequencies (200 - 950 GHz). These techniques make use of higher order statistics like spectrally-limited (∼ 300 km s^−1) increases in confusion noise levels and kurtoses of survey images, and also show promise for general population estimation techniques. For the ISM, we consider Primakoff processes between free electrons and axions, and derive typical signal strengths of 10^−15 Jy sr^−1 · m_a/eV, with a local, cosmological upper bound of 10^−8 Jy sr^−1 · m_a/eV. Hence, we find that any diffuse axion signal from the ISM and other, large-scale, astrophysical plasmas to be too weak to be detected with modern technologies. We therefore find that the best avenue towards detecting a potential quantum chromodynamics (QCD) axion dark-matter particle is through the radio imaging of large swaths of the Galactic Center and other regions where we expect large numbers of pulsars and neutron stars.
ER -