Pith Number

pith:I4IIPHD2

pith:2026:I4IIPHD2FUZ4DVYRB6CY7PY3RI

not attested not anchored not stored refs resolved

Exploring the gaseous halos of z>3 radio galaxies with UVES and JWST/NIRSpec

Carlos De Breuck, Dominika Wylezalek, Fabrizio Arrigoni Battaia, Jelena Ritter, Jo\"el Vernet, Wuji Wang

Most HI absorbers in the halos of high-redshift radio galaxies show nearly constant column densities over more than 30 kpc along the jet axis.

arxiv:2604.26027 v1 · 2026-04-28 · astro-ph.GA

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\usepackage{pith}
\pithnumber{I4IIPHD2FUZ4DVYRB6CY7PY3RI}

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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

About 70 % of the absorbers can be spatially resolved along the radio jet axis, showing minimal variation in column densities over extents of more than 30 kpc. Our results indicate that a fraction of the absorbers may be physically associated with the host systems. ... suggesting a common outflow origin.

C2weakest assumption

That the detected absorption features are HI systems physically linked to the target halos rather than unrelated foreground gas, and that velocity alignment between [OIII] and Lyα traces a causal common outflow rather than projection effects.

C3one line summary

UVES data identify 6-14 HI absorbers per halo with N_HI from 10^12 to 10^17 cm^-2, 70% spatially resolved along the jet with little column density change over >30 kpc, and JWST shows a kinematic link to [OIII] outflows suggesting common origin.

References

4 extracted · 4 resolved · 0 Pith anchors

[1] Arrigoni Battaia, F., Hennawi, J. F., Prochaska, J. X., et al. 2019, MNRAS, 482, 3162 Arrigoni Battaia, F., Prochaska, J. X., Hennawi, J. F., et al. 2018, MNRAS, 473, 3907 Ayromlou, M., Nelson, D., Pi 2019

[2] The black dotted lines in the histograms indicate the uncertainty ranges, namely the 16th and 84th percentiles 1996

[3] The Lyαparameters and uncertainties are derived from the posterior distributions of the MCMC sampling 2073

[4] The Lyαparameters and uncertainties are derived from the posterior distributions of the MCMC sampling 1944

Receipt and verification

First computed	2026-06-24T14:15:58.961110Z
Builder	pith-number-builder-2026-05-17-v1
Signature	Pith Ed25519 (`pith-v1-2026-05`) · public key
Schema	pith-number/v1.0

Canonical hash

4710879c7a2d33c1d7110f858fbf1b8a019f5fe04039a24eff55fb52f8822732

Aliases

arxiv: 2604.26027 · arxiv_version: 2604.26027v1 · doi: 10.48550/arxiv.2604.26027 · pith_short_12: I4IIPHD2FUZ4 · pith_short_16: I4IIPHD2FUZ4DVYR · pith_short_8: I4IIPHD2

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/I4IIPHD2FUZ4DVYRB6CY7PY3RI \
  | 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: 4710879c7a2d33c1d7110f858fbf1b8a019f5fe04039a24eff55fb52f8822732

Canonical record JSON

{
  "metadata": {
    "abstract_canon_sha256": "e14f996b41d0977f71b86ae287629f29aa893da88095f507aa2d3df236eaa076",
    "cross_cats_sorted": [],
    "license": "http://creativecommons.org/licenses/by/4.0/",
    "primary_cat": "astro-ph.GA",
    "submitted_at": "2026-04-28T18:07:43Z",
    "title_canon_sha256": "9ccd1a61d8fa32a00838b844ba0e3078cb5c467066142608b70d080358ec6f7e"
  },
  "schema_version": "1.0",
  "source": {
    "id": "2604.26027",
    "kind": "arxiv",
    "version": 1
  }
}