Bridge to AstroSpectro
AstroSpectro classifies stellar spectra (LAMOST DR5 × Gaia DR3); AstroVision classifies galaxy images (Galaxy10 DECaLS). They share a design philosophy — reproducible runs, interpretability, explicit leakage and limitation tracking — but they operate on different objects: stars in the Milky Way and extragalactic systems. No AstroSpectro number applies to AstroVision, and vice versa.
Status of the bridge
The "images × spectra" link is a research direction. It has not produced a result yet.
What exists
| Element | Where | Status |
|---|---|---|
| Photometric proxy for star formation (u−r populations, g−r) | crossmatcher.py, notebook 05 | Done, from SDSS DR16 — see SDSS Cross-match |
| Plot helpers for morphology × spectral properties | spectral_viz.py | Code in place (CMD, colour by class, UMAP by property, BPT proxy) |
Cross-match with LAMOST DR7 (VizieR V/156) | synthesis.py (attempt_lamost_xmatch), notebook 07 | Failed: the table was not available on the CDS XMatch server; no [Fe/H] was obtained for Galaxy10 galaxies |
| Spectroscopic redshifts | SDSS zsp | Available for 5,652 galaxies; used to compute absolute magnitudes |
What would make the bridge real
- A spectroscopic catalogue overlapping the Galaxy10 footprint (the notebook mentions LAMOST DR7 as the next attempt).
- A definition of the shared quantity — for galaxies, integrated spectral indices; for stars, atmospheric parameters — since [Fe/H] of a star is not the metallicity of a galaxy.
- A common evaluation protocol, so that comparisons are made on matched objects only.
Until then, the physical link used in AstroVision is photometric: SDSS colours and population labels (see Physical Interpretation).
Related pages