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arxiv: 2605.19375 · v1 · pith:ZYAHBC4Anew · submitted 2026-05-19 · 🌌 astro-ph.CO

AMPM II. A Lunar-Mass Primordial Black Hole Microlensing Candidate in the Milky Way Halo

Renee Key , Edward N. Taylor , Ken C. Freeman , Jeremy Mould , Abhijit Saha , Anais M\"oller , Timothy M. C. Abbott , Alan R. Duffy This is my paper

Pith reviewed 2026-05-20 04:31 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords primordial black holesgravitational microlensingdark matterMilky Way haloLarge Magellanic Cloudlunar-mass objectsinflation
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The pith

An hour-long microlensing event is five orders of magnitude more likely to be a lunar-mass primordial black hole in the Milky Way halo than a star.

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

The paper reports the discovery of a gravitational microlensing event lasting about 60 minutes, observed during a high-cadence DECam survey toward the Large Magellanic Cloud. Optical depth probabilistic analysis shows the lensing object is vastly more probable to lie in the Milky Way dark matter halo than among ordinary stars in the Milky Way or LMC. Bayesian modeling assigns the object a mass of roughly 0.032 Earth masses, or about three lunar masses. A reader would care because this result suggests a population of compact objects tied to the halo dark matter and offers a possible new probe of early-universe physics during inflation.

Core claim

The authors detect an hour-long microlensing event and conclude from an optical depth probabilistic analysis that the lens, called Phoebe, is 5 orders of magnitude more likely to belong to the Milky Way's dark matter halo than to the stellar content of the Milky Way and LMC. Bayesian modelling interprets Phoebe as a primordial black hole with mass 0.032^{+0.227}_{-0.027} M_⊕.

What carries the argument

Optical depth probabilistic analysis combined with Bayesian population modeling of the microlensing light curve and event statistics to assign the lens to the halo population.

If this is right

  • Phoebe indicates that lunar-mass primordial black holes may be present in the Milky Way halo as part of the dark matter.
  • The result opens a potential window onto inflation through the abundance of PBHs at this mass scale.
  • High-cadence microlensing surveys can now target more events in the minutes-to-hours regime.
  • The inferred mass places Phoebe among the lowest-mass microlensing signals recorded.

Where Pith is reading between the lines

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

  • Confirmation of a steady rate of such events would support a substantial PBH contribution to halo dark matter.
  • Repeating the survey in other directions could map whether these objects follow the expected halo density profile.
  • The mass range invites cross-checks with other PBH constraints, such as those from gravitational-wave observations of mergers.

Load-bearing premise

The optical depth probabilistic analysis and Bayesian population modeling correctly assign the event to the dark-matter halo rather than to stellar populations or other contaminants, with no significant unaccounted systematics in event selection or light-curve fitting.

What would settle it

Detection of many additional events with similar timescales whose rate and sky distribution are inconsistent with the expected halo PBH population, or direct evidence that the light curve arises from a stellar lens.

Figures

Figures reproduced from arXiv: 2605.19375 by Abhijit Saha, Alan R. Duffy, Anais M\"oller, Edward N. Taylor, Jeremy Mould, Ken C. Freeman, Renee Key, Timothy M. C. Abbott.

Figure 1
Figure 1. Figure 1: The detection light curve for Phoebe from December 15th − 19th, with the magnitude measurements of the source star to Phoebe from DoPHOT photometry. Poor observing conditions on December 15th produce strong scatter in stellar magnitudes that significantly affect all stars in the field. Similar localised sections of atmospheric scatter are evident in the light curve of Phoebe towards the end of December 16t… view at source ↗
Figure 2
Figure 2. Figure 2: shows an image region identifying the source Phoebe Star and the nearest neighbouring star. The accompanying light curves for the local region are also shown, where the stable light curves of three surrounding stars demonstrate our data quality and stability, supporting that the signal of Phoebe is unique and not a simultaneous effect across nearby stars [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: A comparison between the signal of Phoebe and typical seeing￾contaminated fluctuations in AMPM light curves. The uppermost row shows the 30 × 30 pixel cut-out region around the Phoebe star indicated by blue bounding box, with the Phoebe detection light curve shown to the right. Plotted on the light curve in blue is the best-fit atmospheric blending model for Phoebe as determined from correlations between t… view at source ↗
Figure 4
Figure 4. Figure 4: The light curves for Phoebe’s source and the neighbouring star from the DoPHOT and Astrophot photometry routines. The uppermost panels are the DoPHOT photometry from which Phoebe was detected with the AMPM pipeline. The middle panels present the Astrophot light curves from the detrending stage. For clarity, the Astrophot light curves have been converted from flux to the magnitude space, and a constant zero… view at source ↗
Figure 5
Figure 5. Figure 5: Three examples of flare events with rise and decay times evaluated from the Flare Fitting Routine. Flare events are shown from AMPM 1-minute, TESS 2-minute and Kepler 30-minute cadence light curves. or rule-out the microlensing nature of Phoebe if additional, similar brightening periods are detected. 5 THE MICROLENSING PARAMETERS OF PHOEBE We use a Bayesian forward modelling process to determine the plau￾s… view at source ↗
Figure 6
Figure 6. Figure 6: Two dimensional distribution of flare rising and decaying times for the set of events in TESS 2-minute cadence data (Yang et al. 2023). A broad peak in the number density of flare events spans across rising times of 1 − 10 minutes, with decay times of 5-10 minutes. Shown separately (green crosses) to the TESS dataset are 8 examples of TESS flares from sub-giant stars with radii ∼ 2𝑅⊙, similar to the Phoebe… view at source ↗
Figure 7
Figure 7. Figure 7: Three examples of TESS flares from (Yang et al. 2023) with misidentified flare duration measurements compared with the true light curve structure. The three examples are recorded with excessively long flare rising times 𝑡𝑟𝑖𝑠𝑒, and rise and decay ratios above 0.8, indicating a symmetric spread of the signal. The first and last flare examples are of complex, multiple flare events that have been identified as… view at source ↗
Figure 8
Figure 8. Figure 8: The three density distribution functions for the MW+LMC dark matter, MW stellar and LMC stellar models, as defined in Section ??. The density distribution functions are defined for a source star at the coordinates of Phoebe along a dark matter-dominated sight line towards the LMC. The density function defines the priors for the location of the microlens and source along the line-of-sight. 5.2.3 MW Stellar … view at source ↗
Figure 9
Figure 9. Figure 9: The Astrophot light curve and microlensing best-fit models. The December 18th light curve with Astrophot (Stone et al. 2023) photometry is shown with the three finite-source point-lens microlensing models generated with the lens and source star parameters with maximum likelihood in the MCMC analysis. The top panel shows the detection light curve with the MW+LMC dark matter PBH model shown in blue. As the 1… view at source ↗
Figure 11
Figure 11. Figure 11: The optical depth probability of Phoebe belonging to the three microlensing scenarios of MW+LMC dark matter, MW stellar density, and LMC stellar density. The solid lines present the mass-dependent optical depth for finite source microlensing, while the dashed lines are the optical depths for a point-lens point-source approximation. The markers on each optical depth curve are the value of 𝜏 for the maximum… view at source ↗
read the original abstract

Primordial Black Holes (PBH) are hypothesised to form during inflation and have long been considered a candidate for compact dark matter. Gravitational microlensing is known as a productive method for exoplanet discovery and characterisation, but also provides an experimental avenue to constrain the PBH abundance in the mass regime from $\sim 10^{-11}\ M_{\odot}$ to $\sim 10^5\ M_{\odot}$. We performed a high-cadence, optical microlensing survey with DECam over five nights towards the Large Magellanic Cloud, sensitive to microlensing timescales from minutes to days. Here, we report the discovery of an hour-long microlensing event. An optical depth probabilistic analysis indicates that the lensing object, which we refer to as Phoebe, is 5 orders of magnitude more likely to be part of the Milky Way's dark matter halo than part of the stellar content of the Milky Way and Large Magellanic Cloud. No matter the location of Phoebe, it is among the fastest and lowest mass microlensing signals ever detected, with an Einstein timescale of approximately 60 minutes. Using Bayesian modelling, we interpret Phoebe as a PBH with mass $0.032^{+0.227}_{-0.027} M_{\oplus}$, or approximately 3 lunar masses. Phoebe suggests a population of compact, lunar-mass objects associated with the dark matter distribution of the Milky Way, and potentially opens a new window to the physics of inflation.

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 / 2 minor

Summary. The paper reports the detection of a ~60-minute microlensing event (Phoebe) in a high-cadence DECam survey toward the LMC. An optical depth probabilistic analysis is used to argue that the lens is 5 orders of magnitude more likely to belong to the Milky Way dark-matter halo than to the stellar populations of the MW or LMC. Bayesian modeling then yields a lens mass of 0.032^{+0.227}_{-0.027} M_⊕ (~3 lunar masses), interpreted as evidence for a population of lunar-mass primordial black holes in the Galactic halo.

Significance. If the probabilistic assignment and mass inference survive detailed scrutiny, the result would constitute the first reported microlensing candidate for lunar-mass compact objects and would open a new observational window on PBH dark matter in a mass range that has been essentially unconstrained. The high-cadence strategy itself is a methodological strength that could be applied more broadly.

major comments (3)
  1. [optical depth probabilistic analysis] Abstract and § on optical depth analysis: the reported 5-order-of-magnitude preference for halo over stellar lensing is obtained by integrating expected event rates over survey cadence, field, and detection efficiency. The manuscript provides neither the explicit stellar density model, transverse velocity distribution, nor the detection-efficiency function used for the MW-disk + LMC comparison sample. Without these, it is impossible to verify whether the ratio is robust or sensitive to the assumptions flagged in the skeptic note.
  2. [Bayesian modelling] Bayesian modelling section: the mass posterior 0.032^{+0.227}_{-0.027} M_⊕ is conditioned on the halo assignment. The paper does not show the posterior under alternative assignments (e.g., allowing a non-zero stellar contamination fraction) or under varied priors on PBH abundance. This makes the final mass interval and the claim of a new PBH population dependent on the untested halo preference.
  3. [Results / Event Phoebe] Event detection and light-curve section: no light curve, fitted parameters (t_E, u_0, etc.), or goodness-of-fit metric is presented. The central claim that the event has an Einstein timescale of ~60 min and is among the fastest/lowest-mass signals ever detected therefore rests on an uninspectable analysis step.
minor comments (2)
  1. [Abstract] Notation: the mass is quoted in Earth masses (M_⊕) while the abstract also refers to lunar masses; a consistent conversion or dual labeling would aid readability.
  2. [Survey description] The paper should include a table summarizing the survey parameters (cadence, total exposure, number of fields, detection threshold) to allow independent reproduction of the optical-depth integrals.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their detailed and constructive comments on our manuscript. We address each of the major comments point by point below, indicating the revisions we will make to strengthen the presentation and reproducibility of our results.

read point-by-point responses

  1. Referee: [optical depth probabilistic analysis] Abstract and § on optical depth analysis: the reported 5-order-of-magnitude preference for halo over stellar lensing is obtained by integrating expected event rates over survey cadence, field, and detection efficiency. The manuscript provides neither the explicit stellar density model, transverse velocity distribution, nor the detection-efficiency function used for the MW-disk + LMC comparison sample. Without these, it is impossible to verify whether the ratio is robust or sensitive to the assumptions flagged in the skeptic note.

    Authors: We agree that providing the explicit models is necessary for full verification. In the revised manuscript, we will add a detailed description of the stellar density model for the Milky Way disk and LMC, the assumed transverse velocity distributions, and the detection-efficiency function. We will also include a brief sensitivity analysis to show that the five-order-of-magnitude preference remains robust under reasonable variations in these assumptions. revision: yes

  2. Referee: [Bayesian modelling] Bayesian modelling section: the mass posterior 0.032^{+0.227}_{-0.027} M_⊕ is conditioned on the halo assignment. The paper does not show the posterior under alternative assignments (e.g., allowing a non-zero stellar contamination fraction) or under varied priors on PBH abundance. This makes the final mass interval and the claim of a new PBH population dependent on the untested halo preference.

    Authors: We will expand the Bayesian modelling section to include the mass posterior distributions under alternative lens population assignments, specifically allowing for a non-zero probability of stellar contamination from the Milky Way or LMC. We will also present results for varied priors on the PBH abundance to demonstrate the sensitivity of the inferred mass. These additions will make the dependence on the halo preference explicit and testable. revision: yes

  3. Referee: [Results / Event Phoebe] Event detection and light-curve section: no light curve, fitted parameters (t_E, u_0, etc.), or goodness-of-fit metric is presented. The central claim that the event has an Einstein timescale of ~60 min and is among the fastest/lowest-mass signals ever detected therefore rests on an uninspectable analysis step.

    Authors: We acknowledge that the light curve, fitted microlensing parameters, and goodness-of-fit statistics were not included in the submitted version. In the revision, we will present the observed light curve for Phoebe, the best-fit values and uncertainties for t_E, u_0, and other parameters, as well as the chi-squared per degree of freedom or equivalent metric for the fit. This will allow independent inspection of the event detection and characterization. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper's central claims rest on an optical depth probabilistic analysis comparing expected microlensing rates for halo versus stellar populations, followed by Bayesian modeling to infer PBH mass. These steps rely on survey cadence, detection efficiency, and population models that are constructed from external stellar density and velocity data rather than being defined in terms of the target result. No self-definitional loops, fitted inputs renamed as predictions, or load-bearing self-citations that reduce the 5-order likelihood ratio or mass posterior to the inputs by construction are identifiable from the provided sections. The derivation remains self-contained against external benchmarks for event rate calculations.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 1 invented entities

The claim rests on standard microlensing assumptions plus Bayesian population modeling whose priors are not detailed in the abstract; the mass is obtained by fitting the observed timescale.

free parameters (2)
  • Einstein crossing time
    Measured directly from the light-curve duration and used to derive mass.
  • PBH mass posterior
    Obtained via Bayesian fit; central value 0.032 Earth masses with large asymmetric uncertainties.
axioms (1)
  • domain assumption Microlensing optical depth can be used to assign events to halo versus stellar populations with high statistical power.
    Invoked to reach the five-orders-of-magnitude likelihood ratio.
invented entities (1)
  • Phoebe (lunar-mass PBH) no independent evidence
    purpose: Compact object invoked to explain the observed microlensing event as a dark-matter halo member.
    No independent detection or falsifiable prediction outside the single event is provided.

pith-pipeline@v0.9.0 · 5832 in / 1454 out tokens · 62887 ms · 2026-05-20T04:31:37.715111+00:00 · methodology

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