pith. sign in

arxiv: 2606.29653 · v1 · pith:3A6WQYAHnew · submitted 2026-06-28 · 🌌 astro-ph.HE

Pulsed Infrared Emission from Magnetar 4U 0142+61 Detected by JWST

Jeremy Hare , George G. Pavlov , Bettina Posselt , George Younes , Oleg Kargaltsev This is my paper

Pith reviewed 2026-06-30 07:19 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords magnetarinfrared pulsationsJWST4U 0142+61magnetospheric emissionX-ray comparisonpulsed fractiontiming observations
0
0 comments X

The pith

JWST detects pulsed infrared emission from magnetar 4U 0142+61 at 4.08 microns with a peak that aligns with its hard X-ray pulses.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper reports JWST NIRCam observations of magnetar 4U 0142+61 that measure a flux density of 22.9 ± 0.6 μJy in the F410M filter. Pulsations appear at 115.059 ± 0.035 mHz, matching the known spin period, with a lower limit on the pulsed fraction of 10 percent. The single infrared peak per cycle overlaps the hard X-ray peak recorded by NuSTAR while differing from the soft X-ray profile seen by NICER. This phase match leads the authors to attribute the pulsed infrared light to the magnetosphere rather than a surrounding disk or other external material. The result supplies a new wavelength channel for testing how magnetars generate and beam their radiation.

Core claim

In a 33-minute JWST NIRCam timing-mode observation, the team recorded f_ν = 22.9 ± 0.6 μJy at 4.08 μm and extracted a pulse profile with one peak per rotation at the magnetar spin frequency. The infrared peak coincides with the hard X-ray peak, while the soft X-ray peak is offset, indicating that the pulsed infrared emission originates in the same magnetospheric region responsible for the hard X-rays.

What carries the argument

Phase comparison of the NIRCam-derived infrared pulse profile against archival NICER soft X-ray and NuSTAR hard X-ray profiles to establish spatial coincidence of the emission sites.

If this is right

  • Pulsed infrared emission must be produced inside the magnetosphere together with the hard X-rays.
  • Magnetar emission models are required to generate radiation that remains pulsed from hard X-rays down to at least 4 μm.
  • The lower limit of 10 percent on the pulsed fraction constrains the beaming or viewing geometry of the infrared component.
  • Infrared timing observations can now be used to map magnetospheric structure independently of X-ray absorption.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the phase alignment persists across multiple epochs, it would further rule out a fallback-disk origin for the infrared light.
  • Similar JWST timing observations of other magnetars could reveal whether infrared pulsations are common or tied to specific magnetic-field strengths.
  • The detection implies that infrared data may eventually help separate magnetospheric from surface or crustal contributions in magnetar spectra.

Load-bearing premise

The 115 mHz signal detected in the infrared time series is astrophysical pulsation from the magnetar and the observed phase alignment with hard X-rays indicates they share the same physical emission region.

What would settle it

A later JWST or ground-based infrared observation that either fails to recover significant power at the magnetar spin frequency or places the infrared peak at a different rotational phase from the hard X-ray peak would falsify the shared magnetospheric origin.

Figures

Figures reproduced from arXiv: 2606.29653 by Bettina Posselt, George G. Pavlov, George Younes, Jeremy Hare, Oleg Kargaltsev.

Figure 1
Figure 1. Figure 1: The NIRCam F410M TSO data of the target region. Upper left: The second of the 800 integration ramp images. The white pixels are bad pixels. Upper right: Sum of all 800 ramp images. NaN values for bad pixels are set to 0. No smoothing was applied. Lower left: Same image as upper right, but smoothed. Lower right: WebbPSF for F410M as downloaded from the JWST webpage. No smoothing was applied. Note that the f… view at source ↗
Figure 2
Figure 2. Figure 2: Best-fit absorbed power-law model to the MIRI LRS and NIRCam F140M and F250M photometry and corresponding residuals, ∆χ= (data − model)/error, obtained with more recent and improved detector calibrations. Note that the F070W and F410M fluxes were not used in this fit as the data were obtained at different epochs. The fit is in good agreement with that from Hare et al. 2024. The dereddened best-fit model is… view at source ↗
Figure 3
Figure 3. Figure 3: F410M filter image from a single integration ramp of the timing observation of 4U 0142. The white pixels cor￾respond to known bad pixels which are masked in the cali￾brated images. Red shows the source region, and magenta shows the nine background regions used for the analysis. plicable at the epoch MJD 60540 of the NIRCam tim￾ing observation. A phase-connected timing solution has been provided by Peng et … view at source ↗
Figure 4
Figure 4. Figure 4: Lomb-Scargle periodograms of the source region without background subtraction (top), mean of the back￾ground regions (middle), and source region with background subtracted (bottom). The red solid lines show the magnetar spin peak at ν1 ≃ 115 mHz and the aliased peak ν2 ≃ 168 mHz. The blue horizontal dotted and dashed lines in the bottom panel shows the power corresponding to a 3σ and 5σ trials-corrected si… view at source ↗
Figure 5
Figure 5. Figure 5: Binned phase-folded NIRCam light curve for ν = ν1 (i.e., the spin period of the magnetar). The reference time corresponding to phase 0 is MJD 60540.63881582. The red dashed line shows the time-averaged flux of the source. fold the NICER data using the PINT python package (Luo et al. 2021; Susobhanan et al. 2024). Given that there were differences in the pulse shapes between segments, we split the data into… view at source ↗
Figure 6
Figure 6. Figure 6: Binned phase-folded light curves for JWST NIRCam, NICER, and NuSTAR observations using the timing solution presented in [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Locations of photometry measurement apertures for F410M (left panel) and F070W (right panel). The shown example (maximum size) apertures have radii of 0. ′′25 and 0. ′′17, respectively. North is up, East to the left. A. TIME-AVERAGED PHOTOMETRY In [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
read the original abstract

We report on a JWST observation of the magnetar 4U 0142+61 on 2024 August 18 with the Near-Infrared Camera (NIRCam). NIRCam observed the magnetar for 33~min in timing mode, providing a time resolution of 2.5~s. In the F410M filter (pivot wavelength 4.08 $\mu$m), we measured the flux density $f_\nu = 22.9\pm0.6$ $\mu$Jy and detected pulsations at a frequency of $115.059\pm0.035$ mHz, in agreement with the magnetar's spin period at the epoch of the JWST observation. The observed pulse profile has one peak per period (although this may be due to the poor time resolution), with a lower limit on the pulsed fraction of about 10\%. We compare the IR pulse profile to the NICER and NuSTAR X-ray pulse profiles and find that the IR peak overlaps with the hard X-ray peak, suggesting a magnetospheric origin for the pulsed IR emission.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 1 minor

Summary. The manuscript reports a JWST NIRCam timing-mode observation of magnetar 4U 0142+61 lasting 33 min with 2.5 s sampling in the F410M filter. It measures a flux density of 22.9 ± 0.6 μJy and claims detection of pulsations at 115.059 ± 0.035 mHz, matching the known spin period. The single-peaked IR profile is compared to NICER and NuSTAR X-ray profiles, with the IR peak overlapping the hard X-ray peak; this overlap is interpreted as evidence for a magnetospheric origin of the pulsed IR emission. A lower limit of ~10% is placed on the pulsed fraction.

Significance. If the pulsation detection is statistically robust, the result would constitute the first reported pulsed infrared emission from any magnetar. This would directly constrain the location and mechanism of IR emission relative to the hard X-ray component in the magnetosphere, complementing existing X-ray timing data. The JWST timing-mode measurement itself is technically novel for this source class.

major comments (3)
  1. [Abstract] Abstract: the central claim of a pulsation detection at 115.059 ± 0.035 mHz supplies a formal frequency uncertainty but reports neither peak power, S/N ratio, false-alarm probability, nor the details of the periodicity search (targeted vs. blind, frequency window, number of trials). With only ~226 cycles sampled at 2.5 s cadence, these quantities are required to establish that the signal is not a noise fluctuation or instrumental artifact; their absence is load-bearing for the detection claim.
  2. [Abstract] Abstract, final sentence: the inference that the IR peak overlap with the hard X-ray peak indicates a shared magnetospheric origin rests on a single-epoch alignment. No quantitative test of phase coincidence (e.g., cross-correlation significance or Monte-Carlo phase randomization) is described, weakening the origin argument.
  3. [Abstract] Abstract: the stated lower limit of ~10% on the pulsed fraction does not specify how the limit was derived after accounting for the 2.5 s time resolution and possible aliasing; without this calculation the robustness of the limit cannot be assessed.
minor comments (1)
  1. [Abstract] The parenthetical remark that the single peak 'may be due to the poor time resolution' is appropriate but should be quantified in the main text by showing the expected smearing of a narrower pulse under 2.5 s binning.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their insightful comments, which have helped us improve the presentation of our results. We provide point-by-point responses to the major comments below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim of a pulsation detection at 115.059 ± 0.035 mHz supplies a formal frequency uncertainty but reports neither peak power, S/N ratio, false-alarm probability, nor the details of the periodicity search (targeted vs. blind, frequency window, number of trials). With only ~226 cycles sampled at 2.5 s cadence, these quantities are required to establish that the signal is not a noise fluctuation or instrumental artifact; their absence is load-bearing for the detection claim.

    Authors: We agree that the abstract should include these key statistical measures to support the detection claim. In the revised manuscript, we have incorporated the peak power, S/N ratio, and false-alarm probability into the abstract. The periodicity search was targeted at the known spin frequency, using a narrow frequency window consistent with the spin-down rate, and the number of trials has been accounted for in the FAP. Expanded details are provided in the methods section. revision: yes

  2. Referee: [Abstract] Abstract, final sentence: the inference that the IR peak overlap with the hard X-ray peak indicates a shared magnetospheric origin rests on a single-epoch alignment. No quantitative test of phase coincidence (e.g., cross-correlation significance or Monte-Carlo phase randomization) is described, weakening the origin argument.

    Authors: We recognize that a quantitative assessment of the phase coincidence would strengthen the interpretation. We have added a Monte Carlo phase randomization test in the revised manuscript to evaluate the significance of the observed alignment between the IR and hard X-ray peaks, demonstrating that the overlap is statistically significant. revision: yes

  3. Referee: [Abstract] Abstract: the stated lower limit of ~10% on the pulsed fraction does not specify how the limit was derived after accounting for the 2.5 s time resolution and possible aliasing; without this calculation the robustness of the limit cannot be assessed.

    Authors: We have revised the manuscript to explicitly describe the derivation of the pulsed fraction lower limit, including the effects of the 2.5 s sampling time and aliasing considerations. The limit is obtained by simulating the expected modulation for different intrinsic pulsed fractions folded with the instrument response. revision: yes

Circularity Check

0 steps flagged

No significant circularity; direct observational result compared to external prior period

full rationale

The paper reports a JWST flux measurement (f_ν = 22.9±0.6 μJy) and a detected frequency (115.059±0.035 mHz) that is stated to agree with the independently known spin period from prior X-ray data. No model is fitted to derive the period, no prediction is made from a subset of the same data, and no self-citation chain or ansatz is invoked to justify the central claims. The phase-overlap comparison with X-ray profiles is a post-detection interpretation, not a derivation that reduces to the inputs by construction. The result is self-contained against external benchmarks (known spin period).

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the accuracy of the known spin period from earlier X-ray data and on standard assumptions about JWST instrument calibration and background subtraction in timing mode. No free parameters or invented entities are introduced.

axioms (1)
  • domain assumption The magnetar's spin frequency is independently and accurately known from prior X-ray observations at the epoch of the JWST visit.
    Used to confirm that the detected 115.059 mHz signal matches the spin period.

pith-pipeline@v0.9.1-grok · 5740 in / 1359 out tokens · 30916 ms · 2026-06-30T07:19:32.368754+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

36 extracted references · 35 canonical work pages · 2 internal anchors

  1. [1]

    G., Shibanov, Y., et al.\ 2022, , 924, 128

    Abramkin, V., Pavlov, G. G., Shibanov, Y., et al.\ 2022, , 924, 128. doi:10.3847/1538-4357/ac3a6f

    work page doi:10.3847/1538-4357/ac3a6f 2022

  2. [2]

    F., Kaspi, V

    Archibald, R. F., Kaspi, V. M., Scholz, P., et al.\ 2017, , 834, 2, 163. doi:10.3847/1538-4357/834/2/163

    work page doi:10.3847/1538-4357/834/2/163 2017

  3. [3]

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package

    Astropy Collaboration, Price-Whelan, A. M., Lim, P. L., et al.\ 2022, , 935, 2, 167. doi:10.3847/1538-4357/ac7c74

    work page internal anchor Pith review doi:10.3847/1538-4357/ac7c74 2022

  4. [4]

    M., Sip o cz, B

    Astropy Collaboration, Price-Whelan, A. M., Sip o cz, B. M., et al.\ 2018, , 156, 3, 123. doi:10.3847/1538-3881/aabc4f

    work page doi:10.3847/1538-3881/aabc4f 2018

  5. [5]

    P., Tollerud, E

    Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al.\ 2013, , 558, A33. doi:10.1051/0004-6361/201322068

    work page doi:10.1051/0004-6361/201322068 2013

  6. [6]

    doi:10.5281/zenodo.17515973

    Bushouse, H., Eisenhamer, J., Dencheva, N., et al.\ 2025, Zenodo, 1.20.2. doi:10.5281/zenodo.17515973

    work page doi:10.5281/zenodo.17515973 2025

  7. [7]

    doi:10.3847/1538-4365/ae5655

    Chu, C.-Y., Hu, C.-P., Enoto, T., et al.\ 2026, , 284, 1, 25. doi:10.3847/1538-4365/ae5655

    work page doi:10.3847/1538-4365/ae5655 2026

  8. [8]

    , keywords =

    Dhillon, V. S., Marsh, T. R., Hulleman, F., et al.\ 2005, , 363, 609. doi:10.1111/j.1365-2966.2005.09465.x

    work page doi:10.1111/j.1365-2966.2005.09465.x 2005

  9. [9]

    S., Marsh, T

    Dhillon, V. S., Marsh, T. R., Littlefair, S. P., et al.\ 2009, , 394, 1, L112. doi:10.1111/j.1745-3933.2009.00623.x

    work page doi:10.1111/j.1745-3933.2009.00623.x 2009

  10. [10]

    , keywords =

    Dhillon, V. S., Marsh, T. R., Littlefair, S. P., et al.\ 2011, , The first observation of optical pulsations from a soft gamma repeater: SGR 0501+4516, 416, 1, L16. doi:10.1111/j.1745-3933.2011.01088.x

    work page doi:10.1111/j.1745-3933.2011.01088.x 2011

  11. [11]

    & Kaspi, V

    Dib, R. & Kaspi, V. M.\ 2014, , 784, 37. doi:10.1088/0004-637X/784/1/37

    work page doi:10.1088/0004-637x/784/1/37 2014

  12. [12]

    & van Kerkwijk, M

    Durant, M. & van Kerkwijk, M. H.\ 2006, , 652, 576. doi:10.1086/507605

    work page doi:10.1086/507605 2006

  13. [13]

    S.\ 2004, , 605, 840

    Ertan, \" U ., & Cheng, K. S.\ 2004, , 605, 840. doi:10.1086/382502

    work page doi:10.1086/382502 2004

  14. [14]

    H., Ek s i, K

    Ertan, \"U ., Erkut, M. H., Ek s i, K. Y., et al.\ 2007, , 657, 1, 441. doi:10.1086/510303

    work page doi:10.1086/510303 2007

  15. [15]

    P., Dib, R., & Kaspi, V

    Gavriil, F. P., Dib, R., & Kaspi, V. M.\ 2008, 40 Years of Pulsars: Millisecond Pulsars, Magnetars and More, 983, 234. doi:10.1063/1.2900150

    work page doi:10.1063/1.2900150 2008

  16. [16]

    C., Arzoumanian, Z., Adkins, P

    Gendreau, K. C., Arzoumanian, Z., Adkins, P. W., et al.\ 2016, , The Neutron star Interior Composition Explorer (NICER): design and development, 9905, 99051H. doi:10.1117/12.2231304

    work page doi:10.1117/12.2231304 2016

  17. [17]

    G., Reyes, C., et al.\ 2019, , 874, 2, 175

    Guillot, S., Pavlov, G. G., Reyes, C., et al.\ 2019, , 874, 2, 175. doi:10.3847/1538-4357/ab0f38

    work page doi:10.3847/1538-4357/ab0f38 2019

  18. [18]

    G., et al.\ 2021, , 923, 2, 249

    Hare, J., Volkov, I., Pavlov, G. G., et al.\ 2021, , 923, 2, 249. doi:10.3847/1538-4357/ac30e2

    work page doi:10.3847/1538-4357/ac30e2 2021

  19. [19]

    G., Posselt, B., et al.\ 2024, , 972, 176

    Hare, J., Pavlov, G. G., Posselt, B., et al.\ 2024, , 972, 176. doi:10.3847/1538-4357/ad5ce5

    work page doi:10.3847/1538-4357/ad5ce5 2024

  20. [20]

    A., Craig, W

    Harrison, F. A., Craig, W. W., Christensen, F. E., et al.\ 2013, , 770, 103. doi:10.1088/0004-637X/770/2/103

    work page doi:10.1088/0004-637x/770/2/103 2013

  21. [21]

    H., & Kulkarni, S

    Hulleman, F., van Kerkwijk, M. H., & Kulkarni, S. R.\ 2004, , 416, 1037. doi:10.1051/0004-6361:20031756

    work page doi:10.1051/0004-6361:20031756 2004

  22. [22]

    L., van Dyk, D

    Kashyap, V. L., van Dyk, D. A., Connors, A., et al.\ 2010, , 719, 1, 900. doi:10.1088/0004-637X/719/1/900

    work page doi:10.1088/0004-637x/719/1/900 2010

  23. [23]

    Kaspi, V. M. & Beloborodov, A. M.\ 2017, , 55, 1, 261. doi:10.1146/annurev-astro-081915-023329

    work page doi:10.1146/annurev-astro-081915-023329 2017

  24. [24]

    & Martin, C.\ 2002, , 417, 527

    Kern, B. & Martin, C.\ 2002, , 417, 527. doi:10.1038/417527a

    work page doi:10.1038/417527a 2002

  25. [25]

    doi:10.3847/1538-4357/abe62f

    Luo, J., Ransom, S., Demorest, P., et al.\ 2021, , 911, 1, 45. doi:10.3847/1538-4357/abe62f

    work page doi:10.3847/1538-4357/abe62f 2021

  26. [26]

    doi:10.1093/mnrasl/slw024

    Mu \ n oz-Darias, T., de Ugarte Postigo, A., & Casares, J.\ 2016, , 458, L114. doi:10.1093/mnrasl/slw024

    work page doi:10.1093/mnrasl/slw024 2016

  27. [27]

    Olausen, S. A. & Kaspi, V. M.\ 2014, , 212, 6. doi:10.1088/0067-0049/212/1/6

    work page doi:10.1088/0067-0049/212/1/6 2014

  28. [28]

    G., Kargaltsev, O., Hare, J., & Posselt, B

    Pavlov, G. G., Kargaltsev, O., Hare, J., & Posselt, B. 2021, JWST Proposal. Cycle 1, ID. \#2635

    2021

  29. [29]

    doi:10.3847/1538-4357/ae4007

    Peng, H.-L., Weng, S.-S., Ge, M.-Y., et al.\ 2026, , 999, 1, 85. doi:10.3847/1538-4357/ae4007

    work page doi:10.3847/1538-4357/ae4007 2026

  30. [30]

    J., Kelly, D

    Rieke, M. J., Kelly, D. M., Misselt, K., et al.\ 2023, , 135, 028001. doi:10.1088/1538-3873/acac53

    work page doi:10.1088/1538-3873/acac53 2023

  31. [31]

    W., Kaplan, D

    Shaw, A. W., Kaplan, D. L., Gandhi, P., et al.\ 2025, , 169, 1, 21. doi:10.3847/1538-3881/ad8eb1

    work page doi:10.3847/1538-3881/ad8eb1 2025

  32. [32]

    L., Archibald, A

    Susobhanan, A., Kaplan, D. L., Archibald, A. M., et al.\ 2024, , 971, 2, 150. doi:10.3847/1538-4357/ad59f7

    work page doi:10.3847/1538-4357/ad59f7 2024

  33. [33]

    P., Hasc \"o et, R., Yang, C., et al.\ 2015, , 808, 32

    Tendulkar, S. P., Hasc \"o et, R., Yang, C., et al.\ 2015, , 808, 32. doi:10.1088/0004-637X/808/1/32

    work page doi:10.1088/0004-637x/808/1/32 2015

  34. [34]

    T.\ 2018, , 236, 1, 16

    VanderPlas, J. T.\ 2018, , 236, 1, 16. doi:10.3847/1538-4365/aab766

    work page internal anchor Pith review doi:10.3847/1538-4365/aab766 2018

  35. [35]

    L.\ 2006, , 440, 772

    Wang, Z., Chakrabarty, D., & Kaplan, D. L.\ 2006, , 440, 772. doi:10.1038/nature04669

    work page doi:10.1038/nature04669 2006

  36. [36]

    doi:10.1007/978-3-642-17251-9\_26

    Zane, S., Nobili, L., & Turolla, R.\ 2011, High-Energy Emission from Pulsars and their Systems, 21, 329. doi:10.1007/978-3-642-17251-9\_26

    work page doi:10.1007/978-3-642-17251-9 2011