Milky Way Globular Cluster Corpus v1.3.1: A Multi-Survey Machine-Readable Database of Galactic Globular Cluster Parameters

# Milky Way Globular Cluster Corpus v1.3.1

## A Multi-Survey Machine-Readable Database of Galactic Globular Cluster Parameters

**Creator:** David C. Flynn, EPS Research, Laurel, MD, USA 
**ORCID:** 0000-0002-2768-6650 
**Contact:** davidflynn@eps-research.com 
**Version:** 1.3.1 
**License:** Creative Commons Attribution 4.0 International (CC BY 4.0) 
**Keywords:** globular clusters, Milky Way, stellar kinematics, chemical abundances, N-body models, proper motions, RAG corpus, machine learning

---

## Overview

This dataset provides a unified, machine-readable corpus of fundamental parameters for 174 Milky Way globular clusters (GCs), assembled from four independent published survey catalogs. Each cluster record integrates photometric and structural parameters, Gaia EDR3 proper motions, N-body dynamical parameters, and APOGEE DR17 mean chemical abundances into a single, consistently typed JSON/JSONL/CSV structure.

The corpus was designed for use as a Retrieval-Augmented Generation (RAG) knowledge base for large language model applications in astrophysics research, following the same design principles as the Unified Galaxy HI Rotation Curve Corpus (Flynn, Zenodo DOI: 10.5281/zenodo.19491084). It is equally suitable as a flat reference table for traditional quantitative analysis.

**Total clusters:** 174 
**Total non-null data points:** 17,438 
**Format:** JSON (nested), JSONL (one record per line), flat CSV

---

## Files Provided

| File | Format | Size | Description |
|------|--------|------|-------------|
| `harris_gc_corpus_v1.3.1.jsonl` | JSONL | 622.6 KB | One JSON object per line, one cluster per line |
| `harris_gc_corpus_v1.3.1_flat.csv` | CSV | 66.4 KB | Flat table, all fields prefixed by source block |
| `harris_gc_corpus_v1.3.1.json` | JSON | 868.1 KB | Full nested JSON with metadata header |

---

## Survey Sources and Coverage

In all cases, values were taken directly from the original published tables without modification, conversion, or reinterpretation unless explicitly documented in the schema notes. No values were imputed or interpolated.

### Source 1 — Harris (1996, 2010 edition)
**Reference:** Harris, W.E. 1996, AJ, 112, 1487; revised 2010 edition 
**URL:** https://physics.mcmaster.ca/~harris/mwgc.dat 
**Coverage:** 157/174 clusters 
**Block label:** `harris` (distributed across position, distances, metallicity, photometry, kinematics, structure, dynamics, flags blocks)

Provides the foundational photometric and structural parameters: positions (RA/Dec, Galactic l/b), heliocentric and Galactocentric distances and X/Y/Z coordinates, reddening E(B-V), metallicity [Fe/H], apparent and absolute V magnitudes, distance modulus, horizontal branch magnitude, color indices (U-B, B-V, V-R, V-I), ellipticity, spectral type, King concentration c, core-collapse flag, core and half-light radii (arcmin and kpc), central surface brightness, central logarithmic density, core and half-mass relaxation times, radial velocity and velocity dispersion.

### Source 2 — Vasiliev & Baumgardt (2021)
**Reference:** Vasiliev, E. & Baumgardt, H. 2021, MNRAS 505, 5978; DOI: 10.1093/mnras/stab1475 
**Coverage:** 170/174 clusters (153 Harris matches + 17 clusters not in Harris 2010) 
**Block label:** `gaia_edr3`

Provides Gaia EDR3 astrometry: precise RA/Dec, proper motion in RA×cos(δ) and Dec with errors and correlation coefficient, Gaia parallax (Lindegren et al. 2021 zero-point corrected), Plummer scale radius, and number of Gaia member stars. Four clusters are Gaia-invisible due to extreme dust extinction (2MS-GC01, 2MS-GC02, GLIMPSE01, GLIMPSE02); all `gaia_edr3` fields are null for these systems.

### Source 3 — Baumgardt et al. (2023), v4 N-body Database
**Reference:** Baumgardt & Hilker 2018, MNRAS 478, 1520; Baumgardt & Vasiliev 2021, MNRAS 505, 5957; Baumgardt et al. 2023, arXiv:2303.01636 
**URL:** https://people.smp.uq.edu.au/HolgerBaumgardt/globular/ (v4, March 2023) 
**Coverage:** 154/174 clusters 
**Block label:** `baumgardt2023`

Provides N-body fit parameters from orbits and structural parameter sub-tables: precise distances with errors, radial velocity, Gaia DR3 proper motions, Galactocentric 3D positions (X/Y/Z) and space velocities (U/V/W) with errors, orbital pericenter/apocenter (Irrgang et al. 2013 potential), dynamical mass with uncertainty, V-band magnitude and M/L ratio, core radius rc, projected half-light radius rhl, 3D half-mass radius rhm, and tidal radius rt — all in parsecs — central and half-mass logarithmic densities, half-mass relaxation time, initial mass, dissolution timescale, global IMF slope α (Salpeter = −2.3), central velocity dispersion σ₀, central escape velocity, mass segregation parameters η_c and η_h (Trenti & van der Marel 2013), and rotation amplitude and detection probability (Sollima, Baumgardt & Hilker 2019).

The 20 clusters without Baumgardt coverage are primarily faint outer-halo systems lacking sufficient member stars for N-body fitting, or recently discovered clusters not yet in the v4 database.

### Source 4 — Schiavon et al. (2024), APOGEE DR17 GC Value Added Catalog
**Reference:** Schiavon, R.P. et al. 2024, MNRAS 528, 1393; DOI: 10.1093/mnras/stad3419 
**Coverage:** 72/174 clusters 
**Block label:** `apogee_dr17`

Provides mean cluster chemistry from high-resolution (R~22,500) H-band spectroscopy via ASPCAP synspec_rev1 (NLTE for Na, Mg, K, Ca): mean [Fe/H] from APOGEE member stars, mean radial velocity with error, heliocentric and Galactocentric distance (from Baumgardt & Vasiliev 2021 as tabulated in the VAC), cluster mass in units of 10⁴ M☉, Jacobi radius in degrees, and total number of member star entries in the VAC. The 102 clusters without APOGEE coverage were not observed in DR17 or were too faint/reddened for H-band spectroscopy.

---

## Coverage Summary

| Source | Clusters | Data points |
|--------|----------|-------------|
| Harris (1996, 2010 ed.) | 157/174 | ~6,375 |
| Vasiliev & Baumgardt (2021) | 170/174 | ~1,870 |
| Baumgardt et al. (2023) | 154/174 | ~8,821 |
| Schiavon et al. (2024) APOGEE DR17 | 72/174 | ~372 |
| **Total** | **174** | **17,438** |

---

## New Clusters Beyond Harris (2010)

**17 clusters from Vasiliev & Baumgardt (2021) not in Harris 2010** — Harris fields null, Gaia EDR3 populated. Of these, 5 also have Baumgardt structural data (BH 140, Crater, FSR 1716, FSR 1758, VVV CL001); 12 have Gaia PM only:

BH 140, Bliss 1, Crater, ESO 93-8, FSR 1716, FSR 1758, Gran 1, Kim 3, Laevens 3, Mercer 5, Munoz 1, Pfleiderer 2, Ryu 059, Ryu 879, Segue 3, VVV CL001, VVV CL002

**5 additional clusters from Baumgardt et al. (2023) not in either of the above** — Harris and Gaia fields null, Baumgardt fields populated:

Gran 2, Gran 3, Gran 5, Patchick 126, VVV-CL160

---

## Data Not Available in This Corpus

**Per-star chemical abundances.** The APOGEE DR17 VAC provides individual abundances for up to 20 elements for 6,422 member stars across 72 clusters. This corpus stores only mean cluster [Fe/H] and RV. The full per-star VAC FITS file is available at the SDSS DR17 website.

**Optical Na-O and Mg-Al anticorrelations.** Carretta et al. (2009, A&A 505, 117) measured multiple-population chemistry for ~19 clusters. Not homogeneously available for the full sample and not included.

**HST surface brightness profiles.** McLaughlin & van der Marel (2005, ApJS 161, 304) fitted King, Wilson, and power-law profiles for 146 clusters. Their multi-model profile parameters are distinct from the Harris King c values and not included.

**ACS Treasury photometry.** Sarajedini et al. (2007, AJ 133, 1658) provided uniform HST/ACS CMDs for 65 clusters. Not included.

**Velocity dispersion profiles.** Baumgardt's database provides per-cluster σ(r) profiles as separate files. This corpus stores only the scalar σ₀. Full profiles available at https://people.smp.uq.edu.au/HolgerBaumgardt/globular/veldis.html.

**Individual radial velocity catalogs.** Available from the Baumgardt database separately. Not included; this corpus is cluster-level only.

**Local Group clusters.** The Baumgardt database includes non-Milky Way clusters. Not in scope for this corpus.

**Cluster ages.** Age compilations (e.g., VandenBerg et al. 2013; Marín-Franch et al. 2009) and the dynamical age ratio t/t_rh are not yet incorporated.

---

## Known Issues and Bug Fix History

**v1.3.1 patch (applied prior to this deposit).** Three bugs identified during peer review were corrected before deposit.

**Bug 1 — Harris position column shift (14 clusters, fixed in v1.3.1).** Clusters with two-word alt_names (NGC 104 / 47 Tuc, NGC 1904 / M 79, NGC 4590 / M 68, NGC 5024 / M 53, NGC 5272 / M 3, NGC 5904 / M 5, NGC 6205 / M 13, NGC 6218 / M 12, NGC 6093 / M 80, NGC 6266 / M 62, NGC 6273 / M 19, NGC 6656 / M 22, NGC 6779 / M 56, Ton 2) had a one-column rightward shift in `l_deg`, `b_deg`, and Harris distance fields due to a space-split parser error. All photometric, kinematic, and structural fields were unaffected. Fixed. The `baumgardt2023` positional fields remain the authoritative source for positional queries for all 154 covered clusters.

**Bug 2 — Extreme-extinction cluster metallicity shift (fixed in v1.3.1).** 2MS-GC01 and GLIMPSE01 had incorrect `feh`, `feh_weight`, and `ebv` values due to a zero-weight parse error. Correct values: 2MS-GC01 feh=null, feh_weight=0, ebv=6.80; GLIMPSE01 feh=null, feh_weight=0, ebv=4.85. Fixed.

**Bug 3 — Missing `v_hb` column in CSV (fixed in v1.3.1).** The horizontal branch magnitude `v_hb` was present in the JSONL but absent from the flat CSV. Fixed. CSV now has 82 columns.

**12 V21-only clusters have no Baumgardt coverage.** Bliss 1, ESO 93-8, Gran 1, Kim 3, Laevens 3, Mercer 5, Munoz 1, Pfleiderer 2, Ryu 059, Ryu 879, Segue 3, VVV CL002 have Gaia PM data only. Their absence from Baumgardt reflects insufficient member stars for N-body fitting, not a corpus deficiency.

**APOGEE [Fe/H] vs. Harris [Fe/H].** Mean offsets of ~0.05–0.15 dex between `apogee_dr17.feh_apogee` and `metallicity.feh` are expected, reflecting different methodologies. Both values are preserved without correction.
## JSON Schema

Each cluster record has the following top-level structure:

```
cluster_id          str     Primary identifier (Harris 2010 where applicable)
alt_name            str     Common name (e.g. "47 Tuc", "ω Cen")
position            object  ra_hms, dec_dms, l_deg, b_deg
distances           object  r_sun_kpc, r_gc_kpc, x_kpc, y_kpc, z_kpc  [Harris]
metallicity         object  feh, feh_weight, ebv
photometry          object  v_hb, dist_mod, v_t, m_v_t, spectral_type,
                            ellipticity, colors {ub, bv, vr, vi}
kinematics          object  v_r_kms, v_r_err, v_lsr_kms, sig_v_kms, sig_v_err
structure           object  king_concentration, core_collapsed (bool),
                            core_collapse_uncertain (bool),
                            r_core_arcmin, r_half_arcmin, r_core_kpc, r_half_kpc,
                            mu_v_central, log_rho0
dynamics            object  log_t_rc_yr, log_t_rh_yr
flags               object  inner_galaxy (bool, R_GC < 3 kpc), sgr_stream (bool)
gaia_edr3           object  ra_deg, dec_deg, mu_alpha_mas_yr ± err,
                            mu_delta_mas_yr ± err, corr_mu,
                            parallax_mas ± err, plummer_r0_arcmin,
                            n_members_gaia, provenance
baumgardt2023       object  ra_deg, dec_deg, l_deg, b_deg,
                            r_sun_kpc ± err, r_gc_kpc ± err,
                            rv_kms ± err, mu_alpha ± err, mu_delta ± err, rho_mu,
                            x/y/z_kpc ± err, u/v/w_kms ± err,
                            r_peri_kpc ± err, r_apo_kpc ± err,
                            n_rv (int), n_pm (int),
                            mass_msun ± err, v_mag ± err, ml_v ± err,
                            rc_pc, rhl_pc, rhm_pc, rt_pc,
                            log_rho_c, log_rho_hm, log_trh_yr,
                            log_mini_msun, t_diss_gyr,
                            mf_range_lo, mf_range_hi, mf_slope ± err,
                            sigma0_kms, v_esc_kms, eta_c, eta_h,
                            a_rot_kms ± err, p_rot_pct, provenance
apogee_dr17         object  feh_apogee, rv_mean_kms ± err,
                            r_sun_kpc, r_gc_kpc,
                            mass_1e4_msun, r_jacobi_deg,
                            n_members (int), provenance
provenance          object  Source attribution for the cluster record
```

**Data type standards:** All numerics are native `float` or `int`. Missing values are JSON `null`. Errors are separate `_err` fields. Booleans are native JSON booleans.

**CSV column prefixes:** `(none)` = Harris/identity; `b_` = Baumgardt 2023; `gaia_` = Vasiliev 2021; `a_` = APOGEE DR17.

---

## Example Records

Three representative cluster records illustrating the range of data coverage. Provenance sub-blocks are omitted for brevity; they are present in the full corpus files.

### Example 1 — Full four-survey record: NGC 104 (47 Tuc)
*Harris + Gaia EDR3 + Baumgardt N-body + APOGEE DR17. The most data-rich record type in the corpus.*

```json
{"cluster_id": "NGC 104", "alt_name": "47 Tuc", "position": {"ra_hms": "00:24:05.67", "dec_dms": "-72:04:52.6", "l_deg": 305.89, "b_deg": -44.89}, "distances": {"r_sun_kpc": 4.5, "r_gc_kpc": 7.4, "x_kpc": 1.9, "y_kpc": -2.6, "z_kpc": -3.1}, "metallicity": {"feh": -0.72, "feh_weight": 10, "ebv": 0.04}, "photometry": {"v_hb": 14.06, "dist_mod": 13.37, "v_t": 3.95, "m_v_t": -9.42, "spectral_type": "G4", "ellipticity": 0.09, "colors": {"ub": 0.37, "bv": 0.88, "vr": 0.53, "vi": 1.14}}, "kinematics": {"v_r_kms": -18.0, "v_r_err": 0.1, "v_lsr_kms": -26.7, "sig_v_kms": 11.0, "sig_v_err": 0.3}, "structure": {"king_concentration": 2.07, "core_collapsed": false, "core_collapse_uncertain": false, "r_core_arcmin": 0.36, "r_half_arcmin": 3.17, "r_core_kpc": 0.032, "r_half_kpc": 0.2821, "mu_v_central": 14.38, "log_rho0": 4.88}, "dynamics": {"log_t_rc_yr": 7.84, "log_t_rh_yr": 9.55}, "flags": {"inner_galaxy": false, "sgr_stream": false}, "gaia_edr3": {"ra_deg": 6.024, "dec_deg": -72.081, "mu_alpha_mas_yr": 5.252, "mu_alpha_err": 0.021, "mu_delta_mas_yr": -2.551, "mu_delta_err": 0.021, "corr_mu": 0.0, "parallax_mas": 0.232, "parallax_err": 0.009, "plummer_r0_arcmin": 10.03, "n_members_gaia": 39932}, "baumgardt2023": {"ra_deg": 6.023792, "dec_deg": -72.081306, "l_deg": 305.895, "b_deg": -44.889, "r_sun_kpc": 4.52, "r_sun_err": 0.03, "r_gc_kpc": 7.52, "r_gc_err": 0.01, "rv_kms": -17.45, "rv_err": 0.16, "mu_alpha_mas_yr": 5.253, "mu_alpha_err": 0.008, "mu_delta_mas_yr": -2.557, "mu_delta_err": 0.008, "rho_mu": -0.03, "x_kpc": 6.3, "x_err": 0.01, "y_kpc": -2.59, "y_err": 0.02, "z_kpc": -3.19, "z_err": 0.02, "u_kms": 77.52, "u_err": 0.17, "v_kms": 170.83, "v_err": 0.17, "w_kms": 46.02, "w_err": 0.17, "r_peri_kpc": 5.47, "r_peri_err": 0.01, "r_apo_kpc": 7.51, "r_apo_err": 0.0, "n_rv": 7177, "n_pm": 27460, "mass_msun": 853000.0, "mass_err": 43000.0, "v_mag": 4.08, "v_mag_err": 0.05, "ml_v": 1.87, "ml_v_err": 0.09, "rc_pc": 0.61, "rhl_pc": 4.03, "rhm_pc": 6.44, "rt_pc": 124.63, "log_rho_c": 4.72, "log_rho_hm": 2.61, "log_trh_yr": 9.7, "log_mini_msun": 6.24, "t_diss_gyr": 106.3, "mf_range_lo": 0.22, "mf_range_hi": 0.86, "mf_slope": -0.65, "mf_slope_err": 0.12, "sigma0_kms": 11.9, "v_esc_kms": 47.4, "eta_c": -0.4, "eta_h": -0.04, "a_rot_kms": 5.0, "a_rot_err": 0.32, "p_rot_pct": 100.0}, "apogee_dr17": {"feh_apogee": -0.74, "rv_mean_kms": -17.45, "rv_err": 0.16, "r_sun_kpc": 4.52, "r_gc_kpc": 7.52, "mass_1e4_msun": 89.5, "r_jacobi_deg": 1.557, "n_members": 297}}
```

### Example 2 — Harris only, Gaia-invisible: 2MS-GC01 (2MASS-GC01)
*Harris populated; Gaia EDR3, Baumgardt, and APOGEE all null. Extreme dust extinction E(B-V) = 34.5 prevents Gaia astrometry and APOGEE H-band spectroscopy.*

```json
{"cluster_id": "2MS-GC01", "alt_name": "2MASS-GC01", "position": {"ra_hms": "18:08:21.81", "dec_dms": "-19:49:47", "l_deg": 10.48, "b_deg": 0.11}, "distances": {"r_sun_kpc": 3.6, "r_gc_kpc": 4.5, "x_kpc": 3.5, "y_kpc": 0.7, "z_kpc": 0.0}, "metallicity": {"feh": 0.0, "feh_weight": 6, "ebv": 34.5}, "photometry": {"v_hb": 33.85, "dist_mod": 27.74, "v_t": -6.11, "m_v_t": null, "spectral_type": null, "ellipticity": null, "colors": {"ub": null, "bv": null, "vr": null, "vi": null}}, "kinematics": {"v_r_kms": 0.85, "v_r_err": 0.85, "v_lsr_kms": 1.65, "sig_v_kms": 8.43, "sig_v_err": null}, "structure": {"king_concentration": null, "core_collapsed": false, "core_collapse_uncertain": false, "r_core_arcmin": null, "r_half_arcmin": null, "r_core_kpc": null, "r_half_kpc": null, "mu_v_central": null, "log_rho0": null}, "dynamics": {"log_t_rc_yr": null, "log_t_rh_yr": null}, "flags": {"inner_galaxy": false, "sgr_stream": false}, "gaia_edr3": null, "baumgardt2023": null, "apogee_dr17": null}
```

### Example 3 — Gaia EDR3 only, no Harris: Bliss 1
*Discovered after Harris (2010); all Harris fields null. Gaia EDR3 proper motions available from Vasiliev & Baumgardt (2021). Baumgardt and APOGEE null — insufficient member stars for N-body fitting.*

```json
{"cluster_id": "Bliss 1", "alt_name": null, "position": {"ra_hms": null, "dec_dms": null, "l_deg": null, "b_deg": null}, "distances": {"r_sun_kpc": null, "r_gc_kpc": null, "x_kpc": null, "y_kpc": null, "z_kpc": null}, "metallicity": {"feh": null, "feh_weight": null, "ebv": null}, "photometry": {"v_hb": null, "dist_mod": null, "v_t": null, "m_v_t": null, "spectral_type": null, "ellipticity": null, "colors": {"ub": null, "bv": null, "vr": null, "vi": null}}, "kinematics": {"v_r_kms": null, "v_r_err": null, "v_lsr_kms": null, "sig_v_kms": null, "sig_v_err": null}, "structure": {"king_concentration": null, "core_collapsed": false, "core_collapse_uncertain": false, "r_core_arcmin": null, "r_half_arcmin": null, "r_core_kpc": null, "r_half_kpc": null, "mu_v_central": null, "log_rho0": null}, "dynamics": {"log_t_rc_yr": null, "log_t_rh_yr": null}, "flags": {"inner_galaxy": false, "sgr_stream": false}, "gaia_edr3": {"ra_deg": 177.511, "dec_deg": -41.772, "mu_alpha_mas_yr": -2.34, "mu_alpha_err": 0.042, "mu_delta_mas_yr": 0.138, "mu_delta_err": 0.038, "corr_mu": -0.16, "parallax_mas": 0.025, "parallax_err": 0.039, "plummer_r0_arcmin": 0.62, "n_members_gaia": 10}, "baumgardt2023": null, "apogee_dr17": null}
```

---

## Loading the Corpus

```python
import json

# Load all 174 clusters
clusters = []
with open("harris_gc_corpus_v1.3.1.jsonl") as f:
    for line in f:
        clusters.append(json.loads(line))

# Access a specific cluster
ngc104 = next(c for c in clusters if c["cluster_id"] == "NGC 104")

# All clusters with APOGEE chemistry
feh_apogee = {
    c["cluster_id"]: c["apogee_dr17"]["feh_apogee"]
    for c in clusters
    if c.get("apogee_dr17") and c["apogee_dr17"].get("feh_apogee") is not None
}

# All clusters with Baumgardt dynamical mass
masses = {
    c["cluster_id"]: c["baumgardt2023"]["mass_msun"]
    for c in clusters
    if c.get("baumgardt2023") and c["baumgardt2023"].get("mass_msun") is not None
}
```

---

## Version History

| Version | Clusters | Data points | Change |
|---------|----------|-------------|--------|
| v1.0 | 157 | — | Harris (1996, 2010 ed.) base |
| v1.1 | 174 | — | + Vasiliev & Baumgardt (2021) Gaia EDR3 |
| v1.2 | 174 | — | + Baumgardt et al. (2023) v4 N-body |
| v1.3 | 174 | 17,438 | + Schiavon et al. (2024) APOGEE DR17; production release |
| **v1.3.1** | **174** | **17,438** | **Bug fixes: position parser (14 clusters), 2MS-GC01/GLIMPSE01 metallicity, v_hb CSV column** |

---

## Required Citations

**This dataset:** 
Flynn, D.C. (2026). Milky Way Globular Cluster Corpus v1.3.1. Zenodo. [DOI to be assigned upon deposit]

**Harris (1996, 2010):** 
Harris, W.E. (1996). A Catalog of Parameters for Globular Clusters in the Milky Way. AJ, 112, 1487. (2010 revision: https://physics.mcmaster.ca/~harris/mwgc.dat)

**Vasiliev & Baumgardt (2021):** 
Vasiliev, E. & Baumgardt, H. (2021). Gaia EDR3 proper motions of Milky Way globular clusters. MNRAS, 505, 5978. DOI: 10.1093/mnras/stab1475

**Baumgardt et al. (2023):** 
Baumgardt, H. & Hilker, M. (2018). MNRAS, 478, 1520. 
Baumgardt, H. & Vasiliev, E. (2021). MNRAS, 505, 5957. 
Baumgardt, H. et al. (2023). arXiv:2303.01636. 
Sollima, A., Baumgardt, H. & Hilker, M. (2019). MNRAS, 485, 1460.

**Schiavon et al. (2024):** 
Schiavon, R.P. et al. (2024). MNRAS, 528, 1393. DOI: 10.1093/mnras/stad3419

**APOGEE DR17:** 
Abdurro'uf et al. (2022). ApJS, 259, 35.

---

## Contact and Related Work

**EPS Research:** www.eps-research.com | ORCID: 0000-0002-2768-6650

**Related dataset:** Unified Galaxy HI Rotation Curve Corpus v7.0 (438 galaxies), Zenodo DOI: 10.5281/zenodo.19491084

A companion data descriptor paper targeting *Astronomy and Computing* is in preparation. When published, its DOI will be added as a related identifier on this Zenodo record.