Pith Number

pith:VVEX5KL2

pith:2026:VVEX5KL2WKDGKVEQ6NZRPCIR43

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Gauge-invariant cosmological perturbations in Type 3 New General Relativity and background-hierarchy bounds

Daniel Blixt, Kyosuke Tomonari, Sebastian Bahamonde

Type 3 New General Relativity permits consistent linear cosmological perturbations only within specific parameter bounds.

arxiv:2605.16869 v1 · 2026-05-16 · gr-qc · astro-ph.CO · hep-th

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Claims

C1strongest claim

We derive the background-hierarchy bounds for the scalar, transverse-vector, and tensor modes around a flat FLRW background, and identify the region of parameter space in which the linear perturbation theory of Type 3 remains viable for cosmological applications.

C2weakest assumption

The central comparison that defines the bound assumes the background spacetime evolution contribution exceeds the quadratic kinetic term in the perturbed Lagrangian; if other higher-order or interaction terms become comparable at the same scale, the identified viability region would no longer guarantee a consistent linear theory.

C3one line summary

Derives background-hierarchy bounds on the two free parameters of Type 3 NGR to ensure linear cosmological perturbation theory remains viable around flat FLRW.

References

78 extracted · 78 resolved · 17 Pith anchors

[1] second-order terms of perturbation fields are included in the torsion and metric tensor,

[2] Our results in the previous work are summarized in Table I

[3] A first-class constraint disappears, giving rise to one new DOF

[4] Pattern II. Two first-class constraints become second-class, giving rise to one new DOF; Patterns I and II occur in modifications or extensions of an original theory, and these two patterns are direct

[5] Gauge choice I.φ ′ = 0,B ′ = 0,C ′ i = 0 (spatially flat gauge)

Formal links

2 machine-checked theorem links

Cited by

1 paper in Pith

Vector modes in Type 3 New GR

Receipt and verification

First computed	2026-05-20T00:03:27.364675Z
Builder	pith-number-builder-2026-05-17-v1
Signature	Pith Ed25519 (`pith-v1-2026-05`) · public key
Schema	pith-number/v1.0

Canonical hash

ad497ea97ab286655490f373178911e6fda5c33b26a159e6b020a812f263cd8c

Aliases

arxiv: 2605.16869 · arxiv_version: 2605.16869v1 · doi: 10.48550/arxiv.2605.16869 · pith_short_12: VVEX5KL2WKDG · pith_short_16: VVEX5KL2WKDGKVEQ · pith_short_8: VVEX5KL2

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Verify this Pith Number yourself

curl -sH 'Accept: application/ld+json' https://pith.science/pith/VVEX5KL2WKDGKVEQ6NZRPCIR43 \
  | 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: ad497ea97ab286655490f373178911e6fda5c33b26a159e6b020a812f263cd8c

Canonical record JSON

{
  "metadata": {
    "abstract_canon_sha256": "9997612e0d98a92694ce23fef48b5864814568450aa4c31939675aa0eacd7cb8",
    "cross_cats_sorted": [
      "astro-ph.CO",
      "hep-th"
    ],
    "license": "http://arxiv.org/licenses/nonexclusive-distrib/1.0/",
    "primary_cat": "gr-qc",
    "submitted_at": "2026-05-16T08:15:03Z",
    "title_canon_sha256": "05729fd18cd43218a4d8d17fc8020e62ef7ab645a8509f1f208360cc2a8af2d5"
  },
  "schema_version": "1.0",
  "source": {
    "id": "2605.16869",
    "kind": "arxiv",
    "version": 1
  }
}