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Direct Detection of Dark Photon Dark Matter with the James Webb Space Telescope

Haipeng An, Shuailiang Ge, Jia Liu, Zhiyao Lu

TL;DR

This work proposes a direct search for dark photon dark matter (DPDM) using the James Webb Space Telescope (JWST) by exploiting DPDM-to-photon conversion on metallic optics, yielding monochromatic signals at a frequency $f \approx m_{A'}/(2\pi)$. In the high-frequency limit, the induced field reduces to ray optics via stationary phase, allowing a tractable treatment of surface patches and a patch-dipole model; non-monochromatic DPDM is handled with a finite coherence length that suppresses interpatch interference. The study demonstrates that JWST in space cannot detect the DPDM signal with current configuration, but a ground-based test with modest mirror repositioning can focus DPDM-induced photons onto the detector, enabling competitive sensitivity estimates. Using JWST parameters and archival NIRSpec/MIRI data, the projected 95% C.L. limits on the kinetic-mixing parameter are $\epsilon \sim 10^{-12}-10^{-14}$ over $10-500$ THz, surpassing existing laboratory bounds by 1–2 orders of magnitude, and illustrating the potential of future space telescopes for DPDM searches during ground testing.

Abstract

In this study, we propose an investigation into dark photon dark matter (DPDM) within the infrared frequency band, utilizing highly sensitive infrared light detectors commonly integrated into space telescopes, such as the James Webb Space Telescope (JWST). The presence of DPDM induces electron oscillations in both the reflectors and the interior of the detectors. Consequently, these oscillating electrons can emit monochromatic electromagnetic waves with a frequency almost equivalent to the mass of DPDM. By employing the stationary phase approximation, we can demonstrate that when the size of the reflector significantly exceeds the wavelength of the electromagnetic wave, the contribution to the electromagnetic wave field at a given position primarily stems from the surface unit perpendicular to the relative position vector. This simplification results in the reduction of electromagnetic wave calculations to ray optics. Through a careful analysis of photon generation induced by DPDM on the various optical elements of JWST, we find that the contribution of these photons to the detected signal is negligible. Nevertheless, we propose a modified configuration of the JWST mirrors that would enable the DPDM-induced photons to be focused onto the detector. This approach can be applied to future space telescopes during their ground-testing phases. Using the JWST parameters as a representative example, the achievable upper limits on the DPDM-photon mixing constant are $ε\sim 10^{-12}-10^{-14}$ in the frequency range $10-500$~THz at the 95\% confidence level. This reveals the strong potential of future space telescopes for DPDM detection during ground testing, with sensitivities exceeding current limits by 1 to 2 orders of magnitude compared with the XENON1T result and the solar cooling bound.

Direct Detection of Dark Photon Dark Matter with the James Webb Space Telescope

TL;DR

This work proposes a direct search for dark photon dark matter (DPDM) using the James Webb Space Telescope (JWST) by exploiting DPDM-to-photon conversion on metallic optics, yielding monochromatic signals at a frequency . In the high-frequency limit, the induced field reduces to ray optics via stationary phase, allowing a tractable treatment of surface patches and a patch-dipole model; non-monochromatic DPDM is handled with a finite coherence length that suppresses interpatch interference. The study demonstrates that JWST in space cannot detect the DPDM signal with current configuration, but a ground-based test with modest mirror repositioning can focus DPDM-induced photons onto the detector, enabling competitive sensitivity estimates. Using JWST parameters and archival NIRSpec/MIRI data, the projected 95% C.L. limits on the kinetic-mixing parameter are over THz, surpassing existing laboratory bounds by 1–2 orders of magnitude, and illustrating the potential of future space telescopes for DPDM searches during ground testing.

Abstract

In this study, we propose an investigation into dark photon dark matter (DPDM) within the infrared frequency band, utilizing highly sensitive infrared light detectors commonly integrated into space telescopes, such as the James Webb Space Telescope (JWST). The presence of DPDM induces electron oscillations in both the reflectors and the interior of the detectors. Consequently, these oscillating electrons can emit monochromatic electromagnetic waves with a frequency almost equivalent to the mass of DPDM. By employing the stationary phase approximation, we can demonstrate that when the size of the reflector significantly exceeds the wavelength of the electromagnetic wave, the contribution to the electromagnetic wave field at a given position primarily stems from the surface unit perpendicular to the relative position vector. This simplification results in the reduction of electromagnetic wave calculations to ray optics. Through a careful analysis of photon generation induced by DPDM on the various optical elements of JWST, we find that the contribution of these photons to the detected signal is negligible. Nevertheless, we propose a modified configuration of the JWST mirrors that would enable the DPDM-induced photons to be focused onto the detector. This approach can be applied to future space telescopes during their ground-testing phases. Using the JWST parameters as a representative example, the achievable upper limits on the DPDM-photon mixing constant are in the frequency range ~THz at the 95\% confidence level. This reveals the strong potential of future space telescopes for DPDM detection during ground testing, with sensitivities exceeding current limits by 1 to 2 orders of magnitude compared with the XENON1T result and the solar cooling bound.
Paper Structure (11 sections, 71 equations, 9 figures, 1 table)

This paper contains 11 sections, 71 equations, 9 figures, 1 table.

Table of Contents

  1. Introduction
  2. High Frequency Approximation
  3. Monochromatic DPDM
  4. Non-monochromatic DPDM
  5. The Optical System of JWST
  6. Projected Sensitivity with a Modified JWST Configuration
  7. Summary and Outlook
  8. Detailed derivation of Eq. \ref{['equ:sfull']}
  9. A Brief Proof of Eq. \ref{['equ:approx']}
  10. Ray Transfer Matrix Analysis
  11. Data Analysis Method

Figures (9)

  • Figure 1: The OTE (Optical Telescope Element) of JWST. Here, ISIM stands for 'Integrated Science Instrument Module'. Everything is drawn to scale. Figure taken from Ref. Gardner:2006ky.
  • Figure 2: The optical path inside the detector optics of NISpec onboard JWST. Figure taken from Ref. JWSTUserDocumentation-nir-optics.
  • Figure 3: The OTE of JWST can be simplified to a set of lenses. The configuration comprises two convex lenses, positioned as the first and third lenses, with the second lens being concave and the fourth being flat.
  • Figure 4: Constraints on the kinematic mixing parameter $\epsilon$ between Dark Photon Dark Matter (DPDM) and photons in the randomized polarization scheme. The dashed red curve shows the projected sensitivity for the modified JWST configuration. The left and right sections display constraints derived from NIRSpec and MIRI observation data, respectively. Additionally, we provide a comparison with existing limits, including those from Solar li2023production, XENON1T XENON:2021qze, Lampost Chiles:2021gxk, Mudhi Manenti:2021whp, Funk FUNKExperiment:2020ofv, and Tokyo Suzuki:2015sza.
  • Figure 5: Model-independent 95% C.L. upper limits on a constant monochromatic signal from JWST data. The first figure corresponds to NIRSpec observation data, and the lower one to MIRI. It shows the strongest limit from all the projects at each frequency bin.
  • ...and 4 more figures