2 colour previews: one per pointing, and enough wavelength combinations that every band below appears in at least one.
S/N > 10 in every band shown, and a measurement in all 4 - 130,941 of 399,846 catalogue sources. Vega magnitudes. Catalogue from v1.7-2026.09.
Files are served from the JWST root Globus collection; downloading requires a free Globus login. Checksums and full provenance are in MANIFEST.json.
wget -i / curl after authenticating.Mosaic images (resampled onto a sky grid)
| Filter | Type | Iteration | Version | Size | Download |
|---|---|---|---|---|---|
| F162M 1.62µm | Science mosaic | v1.7-2026.09 | 1.6GB | download | |
| PSF residual | resbgsub_m7 | v1.7-2026.09 | 1.6GB | download | |
| PSF model | resbgsub_m7 | v1.7-2026.09 | 1.6GB | download | |
| F210M 2.1µm | Science mosaic | v1.7-2026.09 | 1.6GB | download | |
| PSF residual | resbgsub_m7 | v1.7-2026.09 | 1.6GB | download | |
| PSF model | resbgsub_m7 | v1.7-2026.09 | 1.6GB | download | |
| F360M 3.6µm | Science mosaic | v1.7-2026.09 | 333.0MB | download | |
| PSF residual | resbgsub_m7 | v1.7-2026.09 | 333.0MB | download | |
| PSF model | resbgsub_m7 | v1.7-2026.09 | 333.0MB | download | |
| F480M 4.8µm | Science mosaic | v1.7-2026.09 | 333.1MB | download | |
| PSF residual | resbgsub_m7 | v1.7-2026.09 | 333.1MB | download | |
| PSF model | resbgsub_m7 | v1.7-2026.09 | 333.1MB | download |
Catalogs
| Catalog | Filter | Iteration | Version | Size | Download |
|---|---|---|---|---|---|
| Merged catalog (full) (fits) | — | resbgsub_m8 | v1.7-2026.09 | 358.9MB | download |
| Per-filter vetted (fits) | F162M | resbgsub_m7 | v1.7-2026.09 | 56.9MB | download |
| Per-filter vetted (fits) | F210M | resbgsub_m7 | v1.7-2026.09 | 52.3MB | download |
| Per-filter vetted (fits) | F360M | resbgsub_m7 | v1.7-2026.09 | 28.9MB | download |
| Per-filter vetted (fits) | F480M | resbgsub_m7 | v1.7-2026.09 | 26.7MB | download |
Detector-frame exposures
The 160 individual exposures (17.5GB) the mosaics above were drizzled from, in the original detector frame, carrying the full distortion solution and this pipeline's astrometry as it stood before the images were resampled onto a sky grid. Each group holds exactly the frames behind the matching mosaic, taken from the record that mosaic itself carries of what went into it. Use these to re-drizzle, re-fit, or chase a per-exposure systematic.
The last detector-frame product differs by field and filter: _crf is the Stage-3 outlier/CR-flagged frame where one was written, otherwise the _destreak / _align / _cal frame the mosaic was drizzled from directly. These are the pipeline's live products rather than frozen copies, so a re-reduction writes a new file beside them and a frame here can become an older generation than the pipeline now holds; they are not covered by CHECKSUMS.sha256. Each file records its own provenance in the keywords below, so a downloaded frame can be identified without reference to this page.
How these frames were produced — command, versions, and the Stage-1 settings that change what is in them
NIRCampython jwst_gc_pipeline/reduction/PipelineRerunNIRCAM-LONG.py -p <proposal> -d <field> -f <FILTER> -m nrca,nrcb,merged
Stage-1 (Detector1Pipeline) is re-run from _uncal rather than taken from the archive, with these overrides:
ramp_fit: suppress_one_group=False— a 1-group ramp is FIT rather than discarded, so the brightest stars (whose later groups saturate) keep a measurement instead of a hole. Set on every instrument pathrefpix: use_side_ref_pixels=True— set on every instrument path
jump runs at its pipeline defaults — in particular expand_large_events (snowball expansion) is NOT disabled, despite a comment in the source suggesting otherwise.
Astrometric provenance
Pointing corrections: Offsets_JWST_Brick2092_VIRAC2locked.csv (16KB, modified 2026-08-27T20:04:05)
sha256 13b45b163c10680c19f5d4fff8c6b4ccf9d3a543c541b1d8f2da92acc16b8b05
The table ships as a frozen, checksummed copy; the detector frames do not, because a re-reduction rewrites their headers in place. This table, not the FITS, is what makes this version's astrometry reconstructible after the frames have moved on.
| Filter | vs Gaia (sparse) | vs VIRAC2 (dense) | Quote | Measured |
|---|---|---|---|---|
| F162M | 4.26 mas (contrast 14) | 10.75 mas (contrast 17) | dense highest-contrast leg within tolerance (contrast 17) | 2026-08-29 |
| F210M | 3.94 mas (contrast 16) | 11.62 mas (contrast 6) | sparse highest-contrast leg within tolerance (contrast 16) | 2026-08-29 |
| F360M | 2.75 mas (contrast 43) | 8.23 mas (contrast 68) | dense highest-contrast leg within tolerance (contrast 68) | 2026-08-29 |
| F480M | 1.14 mas (contrast 72) | 8.23 mas (contrast 174) | dense highest-contrast leg within tolerance (contrast 174) | 2026-08-29 |
Where the two references differ, which one to believe is decided per filter by the contrast of the measurement rather than by a fixed preference — a sparse reference can have too few stars to place a peak at all. The bolded value is the one to quote. “neither” means the measurement is either too weak to cite or too large to be an accuracy figure, and the reason says which. Both columns are bulk offsets; a per-star error bar is a separate quantity.