JWST NIRSpec/IFU 'Managed Environment' Test — OC ISM Depletion Search

The Omega Centauri Society

🔭 DRAFT RESEARCH PROPOSAL · INFRARED SPECTROSCOPY · JWST NIRSpec / IFU

JWST NIRSpec/IFU "Managed Environment" Test: Searching for Anomalous ISM Depletion in Omega Centauri's Core

A deep spectroscopic mapping program to distinguish natural gas-starvation from artificially managed interstellar medium depletion within 0.5 parsecs of OC's central mass — using chemical tracers of tidal brown-dwarf disruption as the primary discriminant · Working draft · April 2026

The central question: Both the natural null hypothesis (gas-starved quiescent IMBH) and the OCS Macro Transcension hypothesis (actively managed accretion environment) predict electromagnetic silence. This proposal asks: can we tell the difference between "naturally empty" and "artificially managed"? The answer may be yes, through the chemical fingerprints of controlled tidal disruption events.

1. Scientific Rationale

1.1 The Problem: Two Silences Look Identical

Mahida et al. (2025) found zero radio emission from OC's core at ATCA sensitivity (accretion rate < 10⁻¹⁰ Ṁ_Edd). Chen et al. (2025) found no NIRCam/MIRI accretion signature in JWST data. Both studies are consistent with a completely gas-starved, dynamically relaxed environment — which is also what a 12 Gyr stripped dwarf nucleus without ongoing star formation should look like.

The OCS roadmap suggests that a Phase 4 civilisation would deliberately clear its accretion environment and feed the IMBH through controlled tidal disruption events — specifically, disrupting low-mass objects (brown dwarfs, M-dwarfs) at precisely managed rates. This "managed feeding" scenario is thermodynamically identical to a natural quiescent state at the electromagnetic level, but it would leave chemical fingerprints inconsistent with a truly gas-starved environment.

1.2 The Chemical Test: Tidal Disruption Spectral Tracers

The tidal disruption of a brown dwarf (BD) or low-mass M-dwarf near a massive black hole produces characteristic chemical signatures unlike those from normal stellar evolution:

Lithium enrichment: Sub-stellar objects preserve their initial lithium (not depleted by fusion) until disrupted. A controlled series of BD disruptions would produce anomalous Li I λ6708 emission in the immediate environs of the core, well above predictions from the old stellar population
Heavy-element depletion: An artificially "scrubbed" environment would show lower-than-expected refractory dust abundances (Ca, Mg, Fe) in the innermost 0.1 pc compared to 0.3–0.5 pc, because a civilisation feeding the IMBH would need to prevent dust accumulation near the ISCO
Anomalous gas-to-dust ratio: In a naturally gas-starved cluster, the gas-to-dust ratio should be consistent with the cluster's overall metallicity and stellar evolutionary state. An actively managed environment would show a localized deficit of gas relative to dust (or vice versa) that cannot be explained by normal stellar wind dynamics

OCS-specific prediction (Phase 4 "Managed Feeding"): The OCS roadmap describes brown dwarfs as the preferred fuel source for IMBH spin-up in Phase 4 (estimated ~10⁶–10⁷ year duration). A civilisation managing this process would optimise the tidal disruption rate to maintain a steady Eddington-fraction accretion rate. The observable signature would be a non-equilibrium chemical abundance pattern in the inner 0.1 pc that shows periodic or quasi-periodic enrichment inconsistent with a static, equilibrium stellar population model.

1.3 Why JWST NIRSpec/IFU

JWST's NIRSpec Integral Field Unit provides simultaneous spatial and spectral coverage over 3″ × 3″ with R ≈ 1,000–2,700 (medium resolution) or R ≈ 2,700–5,000 (high resolution). At OC's distance of 5.49 kpc, 3″ corresponds to ~0.08 pc — precisely the scale of the innermost region containing the seven fast-moving Häberle stars. This allows spatially resolved spectroscopy of individual stars and diffuse emission from the ISM within the core radius simultaneously.

2. Observation Strategy

2.1 Phase 1: Archival Data Mining

Chen et al. (2025) have already observed OC with NIRCam and MIRI. JWST's multi-cycle GO programs have generated significant OC archival data. Phase 1 requires no new observing time — it is a systematic reanalysis of all existing JWST data for OC:

Extract NIRSpec spectra of all resolved sources in the inner 0.5 pc
Map line-of-sight velocity dispersion and chemical abundances from Ca II, Mg I, Fe I, and Li I features
Construct a gas-to-dust map from NIRCam + MIRI photometry (F150W, F277W, F1800W bands)
Compare abundance ratios against stellar evolution models for 12 Gyr, [Fe/H] = −1.5 populations

2.2 Phase 2: Dedicated NIRSpec/IFU Spectroscopic Mapping

Parameter	Value
Mode	NIRSpec IFU, PRISM/CLEAR (R ≈ 100, 0.6–5.3 µm) for continuum mapping; G140M/F100LP (R ≈ 1,000) for Li I, Ca II features
Field of view	3″ × 3″ per IFU pointing; mosaic of 5×5 pointings to cover inner 0.5 pc (15″ diameter)
Proposed exposure	5h per pointing × 25 pointings = ~125h total JWST time
Line targets	Li I λ1.048µm (NIR), Ca II triplet λ0.85µm, Fe I λ1.189µm, Hα λ0.656µm (diffuse gas), Paα λ1.875µm (ionised gas)
Continuum targets	Broadband SED of diffuse ISM; compare F150W/F277W/F444W flux ratio against model

2.3 Phase 3: Multi-Epoch Transient Search

A synoptic monitoring program (3–4 NIRCam epochs per year) would detect short-duration IR transients consistent with tidal disruption events or accretion flares. Cross-reference any detected transients with KM3NeT/IceCube neutrino burst alerts — a tidal disruption event accompanied by a high-energy neutrino excess would be extraordinary evidence.

3. Falsification Framework

Observable	Natural null result	Consistent with OCS	Inconsistent with OCS
Li I abundance in inner 0.1 pc	Consistent with evolved stellar population (depleted)	Anomalous excess above 12 Gyr model	Consistent with null (no enrichment)
Gas-to-dust ratio vs radius	Smooth gradient matching stellar wind models	Localized deficit in innermost 0.1 pc relative to 0.2–0.5 pc	Gradient consistent with natural depletion
Heavy-element dust abundance in core	Consistent with cluster metallicity	Anomalously low refractory dust in inner 0.1 pc	Normal abundance gradient
IR transient rate	<1 event/yr above JWST detection threshold	Quasi-periodic transients with rates consistent with OCS feeding model	Zero transients or rates inconsistent with any periodic pattern

Epistemic note: Detection of any of the "consistent with OCS" observables would be intriguing but not conclusive — each has plausible natural explanations. The proposal's value is in establishing chemical baselines and constraints. A null result across all channels is the most likely outcome and would itself be scientifically significant, establishing that OC's core is in complete chemical equilibrium with its 12 Gyr age — strongly inconsistent with any recent, active manipulation.

4. Work Plan

Phase	Timeline	Milestone	Deliverable
1 (archival)	Year 1, Q1–Q3	Download and reprocess all existing JWST OC data; stellar abundance extraction	Archival chemical abundance map
1 (archival)	Year 1, Q4	Comparison against 12 Gyr stellar evolution models; flag anomalies	Anomaly report; JWST GO proposal preparation
2 (new obs)	Year 2	JWST Cycle 4/5 GO proposal submission; if approved, IFU spectroscopic mosaic	NIRSpec IFU spectral data cube
2	Year 2–3	Abundance mapping; gas-to-dust ratio spatial analysis; Li I search	Chemical abundance map paper
3 (monitoring)	Year 3–4	NIRCam synoptic monitoring; transient cross-correlation with KM3NeT alerts	Transient rate paper; multi-messenger alert integration

5. Budget

Item	Cost (USD)	Notes
Postdoc (3 years)	180,000	JWST data analysis, stellar spectroscopy expertise required
HPC compute	15,000	Spectral extraction, stellar population modelling, IFU data cubes
JWST observing time	0 (Phase 1) / ~50,000 (Phase 2 est.)	Phase 1 uses existing archival data; Phase 2 requires GO proposal
Travel + publication	12,000	STScI meetings, JWST user conference, two open-access papers
Total (Phase 1 + 2)	~257,000	Phase 1 alone: ~$207,000

6. References

Chen, S., et al. (2025). JWST NIRCam/MIRI constraints on OC IMBH accretion. arXiv:2511.20945
Mahida, A. D., et al. (2025). No evidence for accretion around the IMBH in ω Cen. ApJ, 996, 122. arXiv:2512.09649
Häberle, M., et al. (2024). Fast-moving stars in ω Cen. Nature, 631, 285. arXiv:2405.06015
Bañares-Hernández, A., et al. (2025). New constraints on OC central mass. A&A, 693, A104. doi:10.1051/0004-6361/202451763
Hills, J. G. (1988). Hyper-velocity and tidal stars from binaries disrupted by a massive Galactic black hole. Nature, 331, 687.
Gezari, S. (2021). Tidal Disruption Events. ARA&A, 59, 21. doi:10.1146/annurev-astro-111720-030029
Rebolledo, D., et al. (2023). JWST NIRSpec IFU observations of globular cluster cores. ApJL.
Häberle, M., et al. (2025). oMEGACat VI — kinematic distance. ApJ, 983, 95. arXiv:2503.04903

Working draft · April 2026 · This is the most speculative of the eleven OCS proposals. Phase 1 (archival reanalysis) is low-risk and can be undertaken immediately. Phase 2 and 3 depend on JWST GO proposal acceptance and the results of Phase 1 anomaly mapping. ← Return to omegacentauri.me

Relevant tools

JWST Accretion Limits

IR spectroscopic accretion constraints

BZ–Kardashev Power

Jet power from spinning IMBH

IMBH Constraint Stacker

Joint mass window from all methods

Dark Matter Flux

DM annihilation signatures in OC