AC32
Star cluster colours and populations
Trace one population from component masses to light. Add companions, change the physical field and inspect native-model support before interpreting a broad colour diagram.
L1
Same birthday, different stars
Unequal masses, unresolved pairs and a finite field can broaden a coeval colour diagram. Follow the light before assigning an age spread.
L1
Draw masses before counting stars
Turn a component IMF into finite draws and native-node weights, then distinguish components from unresolved systems.
L2
Two stars, one point
Add component light within each band, then carry the same system through its actual distance and observing cone.
L3
An age comparison needs a model
Check native ages, phases, passbands, interpolation failures and boundary minima before treating a diagram comparison as an age statement.
L3
A fixed patch of M67
Fetch a named Gaia cone and native models locally, rerun selections and comparisons, and build verified twelve-age import files.
L4
A concentrated core is not a clock
Read fixed simulation and abundance papers to distinguish mass segregation, formation history, finite samples and chemical populations.
Drag the aperture and follow the same light
Sources and calculation scope
- Reyes et al. (2024), a precise M67 isochrone; native ISOA data
The original ISOA file supplies one 3.95 Gyr age. Our CC BY 4.0slice uses98 monotonic rows with central hydrogen fraction above0.001; its native absolute magnitudes areGaia DR2, notEDR3.
- Kroupa (2001), On the variation of the initial mass function
Read the distinction between a component mass distribution and unresolved systems. The finite0.1–8 solar-mass family in our local model is a stated teaching truncation, not a fittedM67IMF.
- PARSEC/CMD3.8 official input help and phase labels
PinnedPARSEC 1.2S, solar-scaled composition, OBC andGaia EDR3Vega, native returned ages andAvnodes. Source labels are approximate; our equal-phase rule prevents bridging labelled boundaries but does not certify continuous evolutionary branches.
- MIST official isochrone interface and user documentation
The local comparison usesMIST 1.2, MESA 7503, nonrotating, solar iron abundance, Av 0, and the originalGaia EDR3columns. Full original numerical hashes identify the twelve-node file; code licensing does not establish table redistribution permission.
- Gaia DR3 documentation and archive
Astrometric reference epoch2016.0 is not a universal epoch for mean photometry. The tutorial uses a fixed cone and explicit astrometric cuts; source rows and real point plots are made only on the reader computer.
- Official Gaia data license
The dedicated data-license page specifiesCC BY-NC 3.0 IGO. This package supplies a named upstream recipe, not a rehostedGaia catalogue, individual-source derivative table or real-source scatter plot.
- Polak et al., arXiv2408.14592v2 (16 September2025)
Sections2–4, Figures2–4 and AppendixA. Separate ongoing formation, dynamical rearrangement, ejections and wind-driven mass-rank changes; inspect which stars define each mass-segregation statistic.
- Huang et al. (2024), arXiv2401.17584v1
SectionIII/Figure3/Table2 and SectionIV/Figure4/Table3. Eight giant-star abundances and the conditional population-selection argument concern chemical multiple populations, not an unresolved-binary ridge.