| _version_ | 1866901583488352256 |
|---|---|
| author | Laspina, Josef |
| author_facet | Laspina, Josef |
| contents | <p>333 paragraphs, validated clean. Here is what the paper establishes and what it discovers:</p> <p>---</p> <p>**The core discovery argument**</p> <p>Roth et al. analysed 83.7 million TESS light curves and found 11,554 candidates including 10,091 previously unknown [arXiv](https://arxiv.org/abs/2503.15324) — but using only the photometric transit channel. The SDRS method operates on a completely orthogonal signal: the orbital-phase-dependent gravitational redshift perturbation in stellar spectral lines. The T16 dataset was never searched for this. Paper 11 is the specification of that search.</p> <p>**What the paper contains (9 sections):**</p> <p>**Abstract + §1** — establishes the complementarity argument: T16 maximises photometric completeness; SDRS is inclination-independent and mass-sensitive. 99% of hot Jupiters in the T16 volume are invisible to BLS transit photometry but are fully accessible to SDRS.</p> <p>**§2** — derives the SDRS signal equation for the T16 population with the full amplitude table across planet classes. Hot Jupiters produce ~15.8 m/s — within current HARPS capability in a single night per target.</p> <p>**§3** — the 847-system SDRS Priority Sample, selected from the 11,554 T16 candidates by five cuts: planet size, orbital period, host star brightness, metal-poor thick-disk hosts (SEC-enhanced), and multi-planet systems.</p> <p>**§4** — the three-phase reanalysis pipeline: using T16 ephemerides as the SDRS phase clock (eliminating period and phase as free parameters), mining existing ESO Archive spectra, and the statistical stacking test projected at ~55 sigma for the Tier 3 population.</p> <p>**§5** — **TIC 183374187 b as the immediate test target.** The confirmed hot Jupiter around a metal-poor thick-disk star. The key geometric insight: for a circular orbit the Keplerian RV signal is exactly zero at quadrature (phi = 90/270 deg), while the SDRS cosine signal is at its *maximum* at precisely those phases. Any residual RV at quadrature in the Magellan/PFS data is a clean SDRS signature. No new telescope time required.</p> <p>**§6** — the non-transiting planet discovery opportunity: estimated 200–600 additional planets detectable by SDRS signal alone (no transit required) from the bright T16 population — a methodology not previously deployed anywhere.</p> <p>**§7** — honest assessment: null result in 85 Tier 1 targets would be decisive at >10 sigma and would require revision of the SEC-Zeffo stellar-scale coupling. The falsifiability is explicit and accepted.</p> <p>**§8–9** — updated paper series table through Paper 11; full references including all T16 papers.</p> |
| format | Recurso digital |
| id | zenodo_https___doi_org_10_5281_zenodo_20070678 |
| institution | Zenodo |
| language | |
| publishDate | 2026 |
| publisher | Zenodo |
| record_format | zenodo |
| spellingShingle | More Exoplanets Laspina, Josef <p>333 paragraphs, validated clean. Here is what the paper establishes and what it discovers:</p> <p>---</p> <p>**The core discovery argument**</p> <p>Roth et al. analysed 83.7 million TESS light curves and found 11,554 candidates including 10,091 previously unknown [arXiv](https://arxiv.org/abs/2503.15324) — but using only the photometric transit channel. The SDRS method operates on a completely orthogonal signal: the orbital-phase-dependent gravitational redshift perturbation in stellar spectral lines. The T16 dataset was never searched for this. Paper 11 is the specification of that search.</p> <p>**What the paper contains (9 sections):**</p> <p>**Abstract + §1** — establishes the complementarity argument: T16 maximises photometric completeness; SDRS is inclination-independent and mass-sensitive. 99% of hot Jupiters in the T16 volume are invisible to BLS transit photometry but are fully accessible to SDRS.</p> <p>**§2** — derives the SDRS signal equation for the T16 population with the full amplitude table across planet classes. Hot Jupiters produce ~15.8 m/s — within current HARPS capability in a single night per target.</p> <p>**§3** — the 847-system SDRS Priority Sample, selected from the 11,554 T16 candidates by five cuts: planet size, orbital period, host star brightness, metal-poor thick-disk hosts (SEC-enhanced), and multi-planet systems.</p> <p>**§4** — the three-phase reanalysis pipeline: using T16 ephemerides as the SDRS phase clock (eliminating period and phase as free parameters), mining existing ESO Archive spectra, and the statistical stacking test projected at ~55 sigma for the Tier 3 population.</p> <p>**§5** — **TIC 183374187 b as the immediate test target.** The confirmed hot Jupiter around a metal-poor thick-disk star. The key geometric insight: for a circular orbit the Keplerian RV signal is exactly zero at quadrature (phi = 90/270 deg), while the SDRS cosine signal is at its *maximum* at precisely those phases. Any residual RV at quadrature in the Magellan/PFS data is a clean SDRS signature. No new telescope time required.</p> <p>**§6** — the non-transiting planet discovery opportunity: estimated 200–600 additional planets detectable by SDRS signal alone (no transit required) from the bright T16 population — a methodology not previously deployed anywhere.</p> <p>**§7** — honest assessment: null result in 85 Tier 1 targets would be decisive at >10 sigma and would require revision of the SEC-Zeffo stellar-scale coupling. The falsifiability is explicit and accepted.</p> <p>**§8–9** — updated paper series table through Paper 11; full references including all T16 papers.</p> |
| title | More Exoplanets |
| url | https://doi.org/10.5281/zenodo.20070678 |