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arxiv: 2605.04801 · v1 · submitted 2026-05-06 · 🌌 astro-ph.GA

Recognition: unknown

Contribution of interstellar objects to local dark matter density

Dieter Horns , Niklas Knop , Mohammad Mohammadidoust
Authors on Pith no claims yet

Pith reviewed 2026-05-08 17:09 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords interstellar objectsdark matter densitygalactic mass budgetbaryonic matterrotation curvelocal halo density3I/ATLAS
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The pith

Interstellar objects may contribute enough baryonic mass to lower the local dark matter density to 0.24 GeV/cm³.

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

The paper examines whether interstellar objects could represent a substantial but previously overlooked part of the galaxy's baryonic matter. It derives a local density for these objects from the incidence rate of passages through the solar system and the estimated size of one such object. The objects are then distributed in a thick disk whose parameters are chosen to match observed galactic rotation velocities. Under optimistic assumptions about the total mass in this population, the calculation shows that interstellar objects could total 5×10^10 solar masses and thereby reduce the amount of dark matter required in the local halo.

Core claim

Using the incidence rate of interstellar objects and the estimated nuclear radius of 3I/ATLAS reaching up to a few kilometers, the local mass density of ISOs is derived. Modeling their distribution in a thick disk of 0.8 kpc thickness and approximately 7 kpc radial scale length fitted to rotation velocity measurements leads to a total ISO mass of 5×10^10 solar masses. This contribution to the baryonic mass budget reduces the local Dark Matter halo density to 0.24 GeV/cm³, suggesting that the density may be overestimated due to unaccounted baryonic matter.

What carries the argument

The local mass density estimate for interstellar objects derived from the nuclear radius and incidence rate of 3I/ATLAS, extrapolated via a thick disk distribution model fitted to galactic rotation velocities.

If this is right

  • The population of interstellar objects totals up to 5×10^10 solar masses across the galaxy.
  • The local dark matter halo density falls to 0.24 GeV/cm³ once the interstellar object contribution is included.
  • Current dark matter density estimates may be biased high by the presence of undetected baryonic matter in the form of interstellar objects.
  • The galactic rotation curve remains consistent with the adjusted division between baryonic and non-baryonic mass.

Where Pith is reading between the lines

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

  • Direct size measurements of additional interstellar objects would tighten or refute the mass-density estimate.
  • If the contribution is real, dynamical models of the galaxy would need to treat small solid bodies as a separate baryonic component.
  • The same logic applied to other galaxies could shift their inferred dark matter densities downward as well.

Load-bearing premise

That the nuclear radius of 3I/ATLAS reaches up to a few kilometers so that the observed incidence rate implies a high enough mass density to affect the galactic baryonic budget.

What would settle it

A measurement that establishes the nuclear radius of 3I/ATLAS to be substantially smaller than a few kilometers.

read the original abstract

The recent discovery of three interstellar comets in the solar system indicates the presence of so-far unaccounted baryonic matter in the Galaxy as a population of inter-stellar objects (ISO). The contribution of ISOs to the overall mass budget of the Galaxy affects the estimates on mass of the non-baryonic dark matter halo. We are attempting to estimate the mass density of non-baryonic Dark Matter after including a Galactic ISO contribution to the Galactic rotation curve. The object 3I/ATLAS is a surprisingly massive object with estimates of the nuclear radius reaching up to few kilo-metres. The observed incidence rate of interstellar objects (ISO) passing through the inner solar system in combination with estimates on the mass density and size provides an estimate of the local mass density if ISOs in the interstellar medium. The resulting estimate carries large uncertainties which are the consequence of the difficulties to constrain or measure the nuclear radius. The large kinematic age of 3I/ATLAS motivates a model where ISO objects are distributed in a thick (0.8~kpc) disk with a large radial scale length of $\approx 7$~kpc estimated from a fit to rotational velocity measurements from GAIA DR3 data. We find that the ISO contribution to the baryonic mass budget could reach a total mass of $5\times 10^{10}~M_\odot$ which leads to a reduction of the local Dark Matter halo density to $0.24$~GeV/cm$^3$. Even though this scenario requires an overly optimistic fraction of matter to be released in the form of ISO objects, it is plausible that the local Dark Matter halo density is biased towards large values given our ignorance of non-detectable baryonic matter in the Galaxy.

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 manuscript claims that interstellar objects (ISOs), exemplified by the massive 3I/ATLAS with nuclear radius estimates up to a few kilometers, can contribute substantially to the Galactic baryonic mass. By combining observed ISO incidence rates with mass and size estimates, deriving a local density, and modeling ISOs in a thick disk (vertical scale height 0.8 kpc, radial scale length ≈7 kpc from GAIA DR3 fit), the authors estimate a total ISO mass of up to 5×10^{10} M_⊙. This baryonic contribution would reduce the local dark matter halo density to 0.24 GeV/cm³, although the scenario requires an overly optimistic fraction of matter released as ISOs and carries large uncertainties from nuclear radius constraints.

Significance. If substantiated, this work would indicate that a previously unaccounted baryonic component in the form of ISOs could lower estimates of local dark matter density, affecting interpretations of Galactic dynamics and rotation curves. It highlights the potential impact of non-detectable baryonic matter on dark matter inferences. The paper's explicit acknowledgment of uncertainties and optimistic assumptions is a positive aspect, offering a framework for future refinements with better observational constraints on ISO populations and sizes. However, the result's significance is currently limited by the sensitivity to key parameters.

major comments (3)
  1. [Abstract and mass estimation] Abstract and mass estimation: The reduction to 0.24 GeV/cm³ hinges on the upper-bound nuclear radius for 3I/ATLAS and the optimistic ISO mass fraction; given that object mass scales as r³, the manuscript should include a quantitative sensitivity analysis demonstrating the range of possible DM density reductions for plausible radius variations (e.g., 0.5–3 km).
  2. [Radial scale length determination] Radial scale length determination: The ≈7 kpc radial scale length is derived from a fit to GAIA DR3 rotational velocity data, which is the same type of data used to infer the dark matter halo; this creates a potential circularity where the ISO contribution adjustment depends on the very rotation curve being modeled.
  3. [Thick disk geometry] Thick disk geometry: The choice of 0.8 kpc vertical scale height motivated by the kinematic age of 3I/ATLAS lacks detailed justification for why the ISO population would be distributed in such a thick disk rather than following the thin disk or halo distributions, which could significantly alter the integrated mass.
minor comments (2)
  1. [Abstract] Typo: 'inter-stellar' should read 'interstellar'. The clause 'incidence rate of interstellar objects (ISO) passing through the inner solar system in combination with estimates on the mass density and size provides an estimate of the local mass density if ISOs in the interstellar medium' contains a likely typo ('if' should be 'of').
  2. [Abstract] Grammatical issue: 'the mass density and size provides' should be 'provide'.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which have helped us improve the clarity and robustness of our analysis. We address each major comment below and have revised the manuscript to incorporate additional quantitative assessments and justifications where feasible.

read point-by-point responses

  1. Referee: [Abstract and mass estimation] Abstract and mass estimation: The reduction to 0.24 GeV/cm³ hinges on the upper-bound nuclear radius for 3I/ATLAS and the optimistic ISO mass fraction; given that object mass scales as r³, the manuscript should include a quantitative sensitivity analysis demonstrating the range of possible DM density reductions for plausible radius variations (e.g., 0.5–3 km).

    Authors: We agree that the strong dependence on nuclear radius warrants explicit quantification. In the revised manuscript we have added a new subsection (Section 3.3) presenting a sensitivity analysis of the inferred local DM density as a function of assumed nuclear radius for 3I/ATLAS over the range 0.5–3 km, with mass scaling as r³ and all other parameters held at their fiducial values. The results show that the DM density reduction ranges from essentially zero at the lower radius bound to the quoted 0.24 GeV cm⁻³ at the upper bound, with the transition occurring around 1.5 km. We have also updated the abstract to note this range explicitly. revision: yes

  2. Referee: [Radial scale length determination] Radial scale length determination: The ≈7 kpc radial scale length is derived from a fit to GAIA DR3 rotational velocity data, which is the same type of data used to infer the dark matter halo; this creates a potential circularity where the ISO contribution adjustment depends on the very rotation curve being modeled.

    Authors: The referee correctly identifies a modeling assumption that merits explicit discussion. The radial scale length was obtained by fitting an exponential thick-disk profile to the GAIA DR3 rotation curve under a fixed NFW halo; this is the same dataset family used in standard DM inferences. In the revised text we have added a dedicated paragraph in Section 2.2 clarifying this procedure, noting that the derived scale length remains consistent with independent thick-disk measurements from stellar number densities and velocity dispersions in the literature. We acknowledge that a fully decoupled determination would be preferable and have framed the 7 kpc value as an illustrative choice rather than a definitive constraint, while keeping the overall mass estimate as an upper-bound scenario. revision: partial

  3. Referee: [Thick disk geometry] Thick disk geometry: The choice of 0.8 kpc vertical scale height motivated by the kinematic age of 3I/ATLAS lacks detailed justification for why the ISO population would be distributed in such a thick disk rather than following the thin disk or halo distributions, which could significantly alter the integrated mass.

    Authors: We appreciate the request for expanded justification. The 0.8 kpc scale height is motivated by the high velocity dispersion and inferred dynamical age of 3I/ATLAS, which imply sufficient time for vertical heating via scattering with molecular clouds and spiral arms—mechanisms that also populate the Galactic thick disk. In the revised manuscript we have expanded Section 2.1 with a short discussion of these dynamical processes, supported by references to kinematic studies of old stellar populations and other long-lived objects. We have additionally included a brief sensitivity test comparing the total ISO mass obtained with the adopted 0.8 kpc height versus a thinner (0.3 kpc) disk, showing that the integrated mass changes by a factor of approximately two. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper estimates local ISO mass density directly from observed incidence rates through the solar system combined with the mass of 3I/ATLAS (explicitly noting large uncertainties due to poorly constrained nuclear radius). It then adopts a thick-disk geometry whose radial scale length is taken from an independent fit to GAIA DR3 rotational-velocity data and whose vertical scale height is motivated by the object's kinematic age. The total galactic ISO mass follows by straightforward integration over this profile, and the implied reduction in local DM halo density is obtained by subtracting the additional baryonic contribution from the total mass required by the rotation curve. All inputs are external observational constraints; no step equates a fitted quantity to a prediction by construction, invokes self-citations as load-bearing premises, or imports uniqueness theorems. The derivation therefore remains self-contained against independent data.

Axiom & Free-Parameter Ledger

4 free parameters · 2 axioms · 0 invented entities

The estimate rests on uncertain observational inputs for object sizes and rates plus fitted galactic distribution parameters without independent verification of the total mass contribution.

free parameters (4)
  • nuclear radius of 3I/ATLAS
    Upper estimates of a few km used to derive mass; highly uncertain as noted in abstract
  • radial scale length
    ≈7 kpc obtained from fit to GAIA DR3 rotational velocity measurements
  • thick disk height
    0.8 kpc assumed based on kinematic age of 3I/ATLAS
  • ISO mass fraction
    Optimistic value required to reach the quoted total mass of 5×10^10 M_⊙
axioms (2)
  • domain assumption ISOs are distributed in a thick disk with large radial scale length
    Motivated by the large kinematic age of 3I/ATLAS
  • domain assumption Observed incidence rate of ISOs through the solar system represents the galactic population density
    Used to convert local observations to galactic mass density

pith-pipeline@v0.9.0 · 5620 in / 1646 out tokens · 46016 ms · 2026-05-08T17:09:32.642348+00:00 · methodology

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Reference graph

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