Current master image
DNB + RGB · 3 observing sessions in the archive
DNB · 8 h 10 min · 98 Lights · RGB · 1 h 50 min · 22 Lights
Visual blend of separate masters; RGB and DNB exposure times remain separate.
Catalogue positions on this exact selected master image.
Open full-resolution field image
Catalogue information from SIMBAD/CDS. Labels are reference positions, not new detections or measured object boundaries.
349 saved star coordinates reproduced. Exact projection reproduction after independently held-out Gaia display registration. Presentation only.. Existing reference residual (95%): 0.94 pixels. This is not a precision estimate for diffuse-object centres.
Catalogue reference centres are not object boundaries or new detections. Diffuse-object positions can be approximate. No physical nebula depth is measured. A display-only affine fit passed held-out controls; this does not validate scientific master registration.
Catalogue retrieved 2026-10-27T08:39:28.725664+00:00. 1f329409782a0ee6877faf92fd9fdb9b83b6267b682860098709c73f2c3413a0
Catalogue landmarks on the selected master.
Verified video for this exact saved image; depth is an illustrative display effect.
Saved per-exposure measurements; no universal quality score.
120 of 120 selected input exposures have cached histograms.
Measured curves in 3 of 3 saved image groups. Measurement availability does not establish a transit or a calibrated detection significance.
Each module is checked separately. An unavailable module does not invalidate the saved master; a complete list is not scientific certification.
Selected input exposures
Selected inputs against your whole archive · RGB and DNB remain separate.
Each unique original exposure contributes once per valid saved metric. Arithmetic mean across all objects; RGB and DNB separate. Missing or invalid values are excluded, never zero. This descriptive reference includes the selected exposures and later nights.
Exposure, camera settings, field brightness, sampling and stellar populations may differ. Background and stellar model SNR are not normalized measures of sky quality, master SNR or detection sensitivity. A difference is not a grade.
Stored per-frame medians of stellar fits are averaged; stars are not pooled. SNR requires a positive recorded effective gain and at least five stellar estimates. Units remain separate. Unknown method versions are recorded, not invented. Small, undersampled stars may bias shape measurements.
Archive version ab3717b4ec376ea87d5261c94fe6dbbd42a97237e09422490b5844921d286006
Selected input exposures
Measurements of the selected input exposures, not the finished master.
300.0 s · Gain 100.0 · Archive snapshot 2026-11-09T03:24:34.927460+00:00
Recorded focal length: 612.0 mm · separate header/settings cohorts, not additional observing sessions.
RGB Session 1 · 2026-09-13
300.0 s · Gain 100.0 · Archive snapshot 2026-11-09T03:24:34.927460+00:00
Recorded focal length: 612.0 mm · separate header/settings cohorts, not additional observing sessions.
DNB Session 2 · 2026-09-15 / DNB Session 1 · 2026-09-14
Provisional star fits · stellar SNR is a model estimate, not master SNR.
Provisional stellar models: undersampled stars can bias the measurements. Differences are not quality grades. Stellar SNR is not nebular or master-image SNR.
Planning · model estimate
Based on the actual inputs of this selected master. RGB and DNB are modelled separately.
Current relative SNR = 1.00×. This is a reference level, not a measured master SNR. There is no universal “good” SNR target: it depends on the feature, aperture or region, noise definition and intended use.
8 h 10 min · 98 selected Lights. Sub-exposures: 300 s
One more comparable hour: about 5.9% higher SNR relative to now. Each following hour adds less relative benefit; it does not become useless.
| Relative SNR goal | Additional time | Total time |
|---|---|---|
| 1.25× | 4 h 35 min 38 s | 12 h 45 min 38 s |
| 1.50× | 10 h 12 min 30 s | 18 h 22 min 30 s |
| 2.00× | 24 h 30 min | 32 h 40 min |
1 h 50 min · 22 selected Lights. Sub-exposures: 300 s
One more comparable hour: about 24.3% higher SNR relative to now. Each following hour adds less relative benefit; it does not become useless.
| Relative SNR goal | Additional time | Total time |
|---|---|---|
| 1.25× | 1 h 01 min 52 s | 2 h 51 min 52 s |
| 1.50× | 2 h 17 min 30 s | 4 h 07 min 30 s |
| 2.00× | 5 h 30 min | 7 h 20 min |
Detail visibility is not angular resolution. More integration can reveal fainter structures. Seeing, optics, sampling, focus and guiding limit sharpness; this curve does not predict smaller or rounder stars.
Same target region, filter, camera, sub-exposure mix, throughput and sky conditions; independent random noise and comparable stacking weights. Fixed-pattern noise, calibration errors, gradients, correlated noise, changing conditions and rejected data can reduce the realised gain. Total exposure is not an effective per-pixel weight or an HDR-core coverage map.
Relative SNR = √((current time + additional time) / current time). Required extra time = current time × (goal² − 1). No numerical floor or absolute master SNR has been fitted; no per-frame star-SNR median is substituted.
Time means usable integration in the stack, excluding overheads, rejected frames and nights with unsuitable conditions. The curve is a planning scenario, not a measured progress history.
Verified session image, not the combined complete image · DNB · 2026-09-15
565 verified identities; 13 spatially distributed highlights. Query: G < 16, at most 5000 sources; fainter neighbours may be absent.
Scheinbare Kataloghelligkeit, kein HR-Diagramm; Staub und Distance wirken mit.
Holdout residual: median 0.26402355851491244 px; 95 % 0.75894494977569 px. G<16; fainter neighbours may be absent. Historical solver training set is unknown.
Temperature, mass and radius are catalogue model estimates, not stellar parameters measured from this photograph.
Exact catalogue values and geometryExperimental photometry · no confirmed transit. 1 unresolved technical review items.
DNB · 98/98 original exposures measured.
RGB · 22/22 original exposures measured.
ADU · decoded digital value · Pixel count per bin; not a wavelength spectrum.
All saved bins, including negative values.
ADU · decoded digital value · Pixel count per bin; not a wavelength spectrum.
All saved bins, including negative values.
8-bit display values · nonlinear · Pixel count per bin; not a wavelength spectrum.
All saved bins, including negative values.
Searched · technical review pending
1 unresolved technical review items · 25 Gaia IDs searched · 2730 tested windows. Windows are not independent events.
No confirmed transit. Short artifact clusters and time-correlated errors can pass this screening. Real periodic search: insufficient coverage; no globally calibrated false-alarm probability is available.
Gaia 2178585194128110080 · 23.78 % relative depth · 15 min · cause unresolved.
Individual native exposures, independent of the final display/HDR image. Conditional measurement errors include the comparison ensemble; shared systematics remain outside that model.
measured diagnostics · 22 timed frames; 0 timing exclusions.
Separate segment 9c7c2898: 1.92 h span · 303.4 s median cadence · duty unavailable · 1 large gap(s); 1 overlapping recorded intervals (bins unavailable when present).
Brightness comparison is observational: sources share sky and calibration; points are not independent trials.
22/22 valid epochs · robust scatter 4.49% · median conditional error 1.27%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
22/22 valid epochs · robust scatter 3.62% · median conditional error 1.26%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
0/22 valid epochs · robust scatter — · median conditional error —. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
22/22 valid epochs · robust scatter 4.44% · median conditional error 1.13%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
12/22 valid epochs · robust scatter 4.65% · median conditional error 0.85%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
16/22 valid epochs · robust scatter 1.29% · median conditional error 0.83%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
22/22 valid epochs · robust scatter 2.69% · median conditional error 1.46%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
22/22 valid epochs · robust scatter 4.33% · median conditional error 1.11%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
6/22 valid epochs · robust scatter 3.37% · median conditional error 0.71%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
20/22 valid epochs · robust scatter 2.92% · median conditional error 0.89%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/22 valid epochs · robust scatter 3.84% · median conditional error 0.71%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
22/22 valid epochs · robust scatter 3.42% · median conditional error 1.20%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
14/22 valid epochs · robust scatter 2.91% · median conditional error 0.77%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
21/22 valid epochs · robust scatter 3.59% · median conditional error 0.86%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
22/22 valid epochs · robust scatter 3.49% · median conditional error 1.35%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
22/22 valid epochs · robust scatter 2.36% · median conditional error 1.01%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
Recommended next acquisition: characterize unsaturated stars with matched short-exposure Darks and same-session Flats, then keep one exposure/filter configuration through a dedicated known-host event and its before/after baseline. There is no real 60/120 s improvement demonstrated here.
measured diagnostics · 32 timed frames; 0 timing exclusions.
Separate segment c94925ef: 2.96 h span · 303.5 s median cadence · 90.2% exposure duty · 1 large gap(s); 0 overlapping recorded intervals (bins unavailable when present).
Brightness comparison is observational: sources share sky and calibration; points are not independent trials.
32/32 valid epochs · robust scatter 4.94% · median conditional error 5.05%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 4.90% · median conditional error 5.65%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 8.25% · median conditional error 5.60%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 4.68% · median conditional error 4.00%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
0/32 valid epochs · robust scatter — · median conditional error —. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 10.73% · median conditional error 7.05%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 3.08% · median conditional error 4.24%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 6.34% · median conditional error 5.15%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 6.34% · median conditional error 4.81%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 7.20% · median conditional error 6.69%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 9.75% · median conditional error 6.87%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 3.99% · median conditional error 4.98%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 6.53% · median conditional error 5.83%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 4.23% · median conditional error 5.28%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 8.03% · median conditional error 3.65%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
32/32 valid epochs · robust scatter 5.65% · median conditional error 5.40%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
Recommended next acquisition: characterize unsaturated stars with matched short-exposure Darks and same-session Flats, then keep one exposure/filter configuration through a dedicated known-host event and its before/after baseline. There is no real 60/120 s improvement demonstrated here.
measured diagnostics · 66 timed frames; 0 timing exclusions.
Separate segment d8c7fd7d: 0.99 h span · 303.1 s median cadence · 84.4% exposure duty · 1 large gap(s); 0 overlapping recorded intervals (bins unavailable when present).
Separate segment 479095b3: 5.14 h span · 303.5 s median cadence · 90.9% exposure duty · 2 large gap(s); 0 overlapping recorded intervals (bins unavailable when present).
Brightness comparison is observational: sources share sky and calibration; points are not independent trials.
10/10 valid epochs · robust scatter 6.37% · median conditional error 6.72%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 5.46% · median conditional error 7.20%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 8.09% · median conditional error 4.54%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 3.47% · median conditional error 3.66%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 2.94% · median conditional error 3.01%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 7.14% · median conditional error 4.30%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 4.27% · median conditional error 3.01%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
0/10 valid epochs · robust scatter — · median conditional error —. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 4.14% · median conditional error 3.21%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 6.33% · median conditional error 6.13%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 10.94% · median conditional error 9.32%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 6.12% · median conditional error 6.62%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 2.48% · median conditional error 3.21%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 4.43% · median conditional error 5.48%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 6.85% · median conditional error 5.80%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
10/10 valid epochs · robust scatter 3.59% · median conditional error 3.83%. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 8.88% · median conditional error 6.88%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 7.18% · median conditional error 7.23%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 4.29% · median conditional error 4.61%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 3.14% · median conditional error 3.60%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 3.59% · median conditional error 3.00%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 5.42% · median conditional error 4.20%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 3.69% · median conditional error 3.06%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
0/56 valid epochs · robust scatter — · median conditional error —. measured, not suitable for search.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 3.08% · median conditional error 3.19%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 6.54% · median conditional error 5.91%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 9.35% · median conditional error 9.09%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 6.47% · median conditional error 6.31%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 3.36% · median conditional error 3.30%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 5.32% · median conditional error 5.54%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 5.08% · median conditional error 5.69%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
56/56 valid epochs · robust scatter 3.58% · median conditional error 3.75%. single-event diagnostics only.
1.4826 × median absolute deviation divided by median. Nonoverlapping bins never split an exposure; boundary crossings remain in the native curve. Sparse bins do not establish a precision improvement.
Recommended next acquisition: characterize unsaturated stars with matched short-exposure Darks and same-session Flats, then keep one exposure/filter configuration through a dedicated known-host event and its before/after baseline. There is no real 60/120 s improvement demonstrated here.
Could a more robust reference ensemble improve these light curves? This controlled experiment reuses the original native fluxes. Your published scientific curves and event results remain unchanged.
Insufficient contiguous data or independent references for the blocked comparison.
Overlapping or unordered timestamps; no guessed cadence
Scientific baseline retained. No promotion from scatter alone; independent control observations and a calibrated uncertainty model are still required.
Median held-out scatter ratio 1.011 (robust / equal-weight reference). Below 1 means less scatter in this diagnostic, not a better transit measurement. 1 source/segments improve by more than 10%; 4 worsen by more than 10%. These are correlated samples, not independent experiments.
1 contiguous blocks are too short; no test is forced across the gap.
2 contiguous blocks are too short; no test is forced across the gap.
First eligible Gaia ID in deterministic order: 2178322720084600832. Held-out points; no connecting lines.
Scientific baseline retained. No promotion from scatter alone; independent control observations and a calibrated uncertainty model are still required.
Insufficient contiguous data or independent references for the blocked comparison.
2 contiguous blocks are too short; no test is forced across the gap.
Scientific baseline retained. No promotion from scatter alone; independent control observations and a calibrated uncertainty model are still required.
Four contiguous held-out folds per sufficiently long uninterrupted block, with one purged epoch on each side. Reference medians are learned only from training epochs; each target is excluded from its references. Fixed Huber cutoff 1.5, at least six references. No hyperparameter search or target-based refitting.
2026-09-13 · RGB · Gaia 2178322342127309056. First available session and source ID; not selected for apparent variability.
2026-09-13 02:00:37 CEST (UTC+0200) → 2026-09-13 03:55:40 CEST (UTC+0200)
4.3% Moon illumination · saved calculation
Altitude -49.7°Target separation —Mitte des Aufnahmezeitraums
Time assumption: DATE-OBS interpreted as UTC because TIMESYS is missing. Astronomical context is provisional.
Moon altitude is approximate; local Earth-orientation data may be incomplete.
Geometric Moon altitude, without terrain or refraction; site elevation assumed to be 0 m.
2026-09-15 01:06:27 CEST (UTC+0200) → 2026-09-15 04:03:52 CEST (UTC+0200)
16.2% Moon illumination · saved calculation
Altitude -58.4°Target separation —Mitte des Aufnahmezeitraums
Time assumption: DATE-OBS interpreted as UTC because TIMESYS is missing. Astronomical context is provisional.
Moon altitude is approximate; local Earth-orientation data may be incomplete.
Geometric Moon altitude, without terrain or refraction; site elevation assumed to be 0 m.
2026-09-15 21:57:27 CEST (UTC+0200) → 2026-09-16 04:52:04 CEST (UTC+0200)
23.8% Moon illumination · saved calculation
Altitude -47.1°Target separation —Mitte des Aufnahmezeitraums
Time assumption: DATE-OBS interpreted as UTC because TIMESYS is missing. Astronomical context is provisional.
Moon altitude is approximate; local Earth-orientation data may be incomplete.
Geometric Moon altitude, without terrain or refraction; site elevation assumed to be 0 m.
Saved time assumptions are unchanged. Site and weather are shown on the session pages.
Comparison with your current archive: each physical observing session has equal weight. Valid per-exposure values are first averaged within each session, then the session means are averaged. Later sessions and the exposures shown here may be included. This is neither an independent test nor a formal quality grade.
Selected data use the exact input IDs of this product. RGB and DNB, methods, units, sampling and recorded acquisition settings remain separate. Unknown setup metadata do not establish physical compatibility. A few sessions form only a small descriptive reference. Missing values do not count as zero.
FWHM and star shape are saved medians of the stellar fits in each exposure; the display averages these per-exposure values. Stellar SNR is the saved median of model estimates from at least five stars per exposure. Model: source Poisson noise, background variance and uncertainty in the mean local sky. Circular aperture radius 3, sky annulus 5–7 sampling pixels, 3σ clipping. EGAIN in electrons/ADU is required. Different star selections remain a limitation even within the same field.
Background and scatter are raw green-grid ADU under compatible acquisition conditions. Field emission, gradients and stellar populations limit comparison. These are not measurements of pure seeing, nebular SNR or transit sensitivity. The previous grading rule requiring eight other nights has not changed.
RGB · Background: 22/22 valid selected exposures; archive 52/52 frames, 2 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
RGB · Star shape: 22/22 valid selected exposures; archive 52/52 frames, 2 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
DNB · Star shape: 98/98 valid selected exposures; archive 139/139 frames, 4 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
DNB · Star width (FWHM): 98/98 valid selected exposures; archive 139/139 frames, 4 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
DNB · Stellar SNR: 98/98 valid selected exposures; archive 98/98 frames, 2 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
DNB · Background scatter: 98/98 valid selected exposures; archive 139/139 frames, 4 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
RGB · Background scatter: 22/22 valid selected exposures; archive 52/52 frames, 2 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
RGB · Star width (FWHM): 22/22 valid selected exposures; archive 52/52 frames, 2 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
RGB · Stellar SNR: 22/22 valid selected exposures; archive 22/22 frames, 1 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
DNB · Background: 98/98 valid selected exposures; archive 139/139 frames, 4 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
Archive version ab3717b4ec376ea87d5261c94fe6dbbd42a97237e09422490b5844921d286006. This export is a frozen snapshot; it does not update without a new export.
All measurements and frozen archive comparison
16 selected frames worth reviewing · 110/120 inputs have enough same-session support. All frames remain selected exactly as before.
Separate raw measurements, compared with the median of the same session and recorded setup. No overall score, automatic rejection or diagnosis.
| Saved header time / input ID | Measurement | This frame | Session median | Why review? |
|---|---|---|---|---|
| 2026-09-15T22:24:51.008145 ed247b9862bd | Star width (FWHM) | 4.279 sensor pixels | 3.124 | Broader than this session; inspect focus, tracking and sampling. The cause is not identified. |
| 2026-09-16T02:01:03.537004 aed49c12ae94 | Background level | 546 ADU | 540 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-16T02:06:06.737446 e0833a1216e0 | Background level | 546 ADU | 540 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-16T02:11:20.195469 ddb1b4dd52bf | Background level | 547 ADU | 540 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-16T02:16:23.154696 bef9201c707d | Background level | 547 ADU | 540 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-16T02:16:23.154696 bef9201c707d | Detected sources | 2071 sources | 3024 | Fewer detected sources; clouds, focus, framing and detection thresholds are possible causes. |
| 2026-09-16T02:21:26.234403 ea890226a86e | Background level | 548 ADU | 540 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-16T02:21:26.234403 ea890226a86e | Detected sources | 1828 sources | 3024 | Fewer detected sources; clouds, focus, framing and detection thresholds are possible causes. |
| 2026-09-16T02:21:26.234403 ea890226a86e | Stellar SNR estimate | 50.37 dimensionless | 124.5 | Lower model SNR in the sampled stars; changing star selection may contribute. |
| 2026-09-16T02:26:43.757869 28e52093f4c1 | Background level | 548 ADU | 540 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-16T02:26:43.757869 28e52093f4c1 | Background scatter | 15.19 ADU | 14.02 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-16T02:31:47.845276 fc9a0e08a15b | Background level | 549 ADU | 540 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-16T02:31:47.845276 fc9a0e08a15b | Background scatter | 15.23 ADU | 14.02 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-16T02:31:47.845276 fc9a0e08a15b | Detected sources | 2034 sources | 3024 | Fewer detected sources; clouds, focus, framing and detection thresholds are possible causes. |
| 2026-09-16T02:31:47.845276 fc9a0e08a15b | Stellar SNR estimate | 88.01 dimensionless | 124.5 | Lower model SNR in the sampled stars; changing star selection may contribute. |
| 2026-09-16T02:36:51.247743 8ac2db8fe488 | Background level | 550 ADU | 540 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-16T02:36:51.247743 8ac2db8fe488 | Background scatter | 15.37 ADU | 14.02 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-16T02:42:00.761306 644750354c8b | Background level | 550 ADU | 540 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-16T02:42:00.761306 644750354c8b | Background scatter | 15.43 ADU | 14.02 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-16T02:42:00.761306 644750354c8b | Stellar SNR estimate | 87.74 dimensionless | 124.5 | Lower model SNR in the sampled stars; changing star selection may contribute. |
| 2026-09-16T02:47:04.894169 67352681f298 | Background level | 552 ADU | 540 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-16T02:47:04.894169 67352681f298 | Background scatter | 15.58 ADU | 14.02 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-13T01:25:07.172448 0b1321b0d7f1 | Background level | 869 ADU | 814 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-13T01:25:07.172448 0b1321b0d7f1 | Background scatter | 40.65 ADU | 38.91 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-13T01:30:10.282039 b7ed0fea7238 | Background level | 872 ADU | 814 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-13T01:30:10.282039 b7ed0fea7238 | Background scatter | 40.64 ADU | 38.91 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-13T01:35:13.324373 bd535d60eeac | Background level | 885 ADU | 814 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-13T01:35:13.324373 bd535d60eeac | Background scatter | 40.99 ADU | 38.91 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-13T01:50:40.840909 47a4429ce8b5 | Background level | 852 ADU | 814 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-13T01:50:40.840909 47a4429ce8b5 | Background scatter | 40.49 ADU | 38.91 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-13T01:50:40.840909 47a4429ce8b5 | Star width (FWHM) | 2.795 sensor pixels | 2.661 | Broader than this session; inspect focus, tracking and sampling. The cause is not identified. |
| 2026-09-13T01:50:40.840909 fc63e2d7d0c3 | Background level | 852 ADU | 814 | Different background level; sky, gradients and real field emission can all contribute. |
| 2026-09-13T01:50:40.840909 fc63e2d7d0c3 | Background scatter | 40.48 ADU | 38.91 | Higher saved background scatter; this is not pure detector noise. |
Review distance = (value − session median) / (1.4826 × MAD). The threshold 3.5 is an advisory rule, not statistical significance. At least 12 valid frames and 75% coverage are required; zero MAD is unavailable. SNR requires the existing gain and star-count checks. Background changes are flagged in either direction.
Shared tracking/focus problems can affect an entire night without producing an outlier. No independent validation labels exist yet. Raw-green sampling and changing star populations limit interpretation. RGB/DNB, exposure, method and recorded orientation remain separate; unknown metadata do not establish compatibility.
DNB · 300.0 s · session acq_5e32c08a: Background level 10/10: too few valid session frames; Background scatter 10/10: too few valid session frames; Detected sources 10/10: too few valid session frames; Star eccentricity 10/10: too few valid session frames; Star width (FWHM) 10/10: too few valid session frames; Stellar SNR estimate 10/10: too few valid session frames. Unknown: device_id, filter, optical_configuration, readout_mode.
DNB · 300.0 s · session acq_e2cac882: Background level 32/32: zero or numerically unresolved MAD; no relative flag; Background scatter 32/32; Detected sources 32/32; Star eccentricity 32/32; Star width (FWHM) 32/32; Stellar SNR estimate 32/32. Unknown: device_id, filter, optical_configuration, readout_mode.
RGB · 300.0 s · session acq_b98cd89d: Background level 22/22; Background scatter 22/22; Detected sources 22/22; Star eccentricity 22/22; Star width (FWHM) 22/22; Stellar SNR estimate 22/22. Unknown: device_id, filter, optical_configuration, readout_mode.
DNB · 300.0 s · session acq_5e32c08a: Background level 56/56; Background scatter 56/56; Detected sources 56/56; Star eccentricity 56/56; Star width (FWHM) 56/56; Stellar SNR estimate 56/56. Unknown: device_id, filter, optical_configuration, readout_mode.
Method session-quality-assistant-1. Saved measurements and existing archive comparisons are unchanged.
Literature context, checked 3 November 2026; not measured from these images. Distances are approximate and depend on the adopted source.
Barnard's 1893 photograph records the larger IC 1396 region; a separate first-discovery date for the Elephant's Trunk (IC 1396A) is not established here. Distance follows NASA/WISE's approximate value for the nebula, not a new Gaia fit.
