Pith Number

pith:4TSXQRSO

pith:2025:4TSXQRSOBM63Y7XF2GKXCNJBY3

not attested not anchored not stored refs resolved

Cosmological implications of Bumblebee theory on an FLRW background

Francisco Tello-Ortiz, Grigorios Panotopoulos, Manuel Gonzalez-Espinoza

The Bumblebee model on an FLRW background has one free parameter fixed by supernova data to determine its expansion history and compare to Lambda-CDM.

arxiv:2512.04349 v2 · 2025-12-04 · gr-qc

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\usepackage{pith}
\pithnumber{4TSXQRSOBM63Y7XF2GKXCNJBY3}

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Record completeness

1 Bitcoin timestamp

2 Internet Archive

3 Author claim open · sign in to claim

4 Citations open

5 Replications open

✓ Portable graph bundle live · download bundle · merged state

The bundle contains the canonical record plus signed events. A mirror can host it anywhere and recompute the same current state with the deterministic merge algorithm.

Claims

C1strongest claim

Upon comparison to available supernovae data, the best fit numerical value of the unique free parameter of the model is determined. We show graphically all the cosmological quantities of interest versus red-shift, such as the deceleration parameter, dark energy equation of state parameter, etc. The statefinders and the age of the Universe are also computed. Finally, a comparison to the Λ-CDM model is made as well.

C2weakest assumption

The Bumblebee model possesses a single free parameter whose value can be uniquely determined by fitting background cosmological observables while preserving a consistent FLRW solution and dynamical system structure.

C3one line summary

Bumblebee theory on an FLRW background yields a cosmological model whose single free parameter is fitted to supernovae observations, producing deceleration and dark energy behaviors that are compared to Lambda-CDM.

References

92 extracted · 92 resolved · 52 Pith anchors

[1] It is important to note that at the critical pointa R, the conditions are such that Ωr = 1 and Ωde = 0

[2] S. P. et al., Astrophys. J.517, 565 (1999) 1999

[3] A. G. R. et al., Astron. J.116, 1009 (1998) 1998

[4] V. A. Kostelecky and S. Samuel, Phys. Rev. D39, 683 (1989) 1989

[5] V. A. Kostelecky and S. Samuel, Phys. Rev. D40, 1886 (1989) 1989

Formal links

2 machine-checked theorem links

Receipt and verification

First computed	2026-05-17T23:39:00.646066Z
Builder	pith-number-builder-2026-05-17-v1
Signature	Pith Ed25519 (`pith-v1-2026-05`) · public key
Schema	pith-number/v1.0

Canonical hash

e4e578464e0b3dbc7ee5d195713521c6cde8f993993d8b2ffc1f645a8befe790

Aliases

arxiv: 2512.04349 · arxiv_version: 2512.04349v2 · doi: 10.48550/arxiv.2512.04349 · pith_short_12: 4TSXQRSOBM63 · pith_short_16: 4TSXQRSOBM63Y7XF · pith_short_8: 4TSXQRSO

Agent API

Resolver JSON Graph JSON Events JSON Schema Signing key

Verify this Pith Number yourself

curl -sH 'Accept: application/ld+json' https://pith.science/pith/4TSXQRSOBM63Y7XF2GKXCNJBY3 \
  | jq -c '.canonical_record' \
  | python3 -c "import sys,json,hashlib; b=json.dumps(json.loads(sys.stdin.read()), sort_keys=True, separators=(',',':'), ensure_ascii=False).encode(); print(hashlib.sha256(b).hexdigest())"
# expect: e4e578464e0b3dbc7ee5d195713521c6cde8f993993d8b2ffc1f645a8befe790

Canonical record JSON

{
  "metadata": {
    "abstract_canon_sha256": "b08c57b32bbc8a328f9a3f907a8cdb322afd7cac8bfc5ed6f734332f01ca7094",
    "cross_cats_sorted": [],
    "license": "http://arxiv.org/licenses/nonexclusive-distrib/1.0/",
    "primary_cat": "gr-qc",
    "submitted_at": "2025-12-04T00:45:59Z",
    "title_canon_sha256": "7e2b66e47c634243afcb6a4c427357d16743e5d1ba0181e47dcb24e2b856f651"
  },
  "schema_version": "1.0",
  "source": {
    "id": "2512.04349",
    "kind": "arxiv",
    "version": 2
  }
}