Selected by you
DNB · 1 observing sessions in the archive
DNB · 2 h 35 min · 31 Lights
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.
569 saved star coordinates reproduced. Exact projection reproduction after independently held-out Gaia display registration. Presentation only.. Existing reference residual (95%): 1.27 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.
31 of 31 selected input exposures have cached histograms.
Measured curves in 1 of 1 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.
DNB Session 1 · 2026-09-29
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.
DNB · 2 h 35 min · 31 Lights
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.
2 h 35 min · 31 selected Lights. Sub-exposures: 300 s
One more comparable hour: about 17.8% 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 27 min 11 s | 4 h 02 min 11 s |
| 1.50× | 3 h 13 min 45 s | 5 h 48 min 45 s |
| 2.00× | 7 h 45 min | 10 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 image · DNB · 2026-09-29
584 verified identities; 12 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 0.5692565529249214 px; 95 % 1.2145060181409268 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. 0 unresolved technical review items.
DNB · 31/31 original exposures measured.
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 · no flagged review item
0 unresolved technical review items · 16 Gaia IDs searched · 816 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.
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 · 31 timed frames; 0 timing exclusions.
Separate segment 3e7ad407: 2.91 h span · 303.5 s median cadence · 88.7% 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.
31/31 valid epochs · robust scatter 4.38% · median conditional error 5.76%. 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.
31/31 valid epochs · robust scatter 5.01% · median conditional error 4.63%. 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.
31/31 valid epochs · robust scatter 3.41% · median conditional error 4.63%. 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.
31/31 valid epochs · robust scatter 5.26% · median conditional error 4.17%. 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.
31/31 valid epochs · robust scatter 2.22% · median conditional error 3.62%. 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.
31/31 valid epochs · robust scatter 3.72% · median conditional error 4.47%. 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.
31/31 valid epochs · robust scatter 6.49% · median conditional error 4.52%. 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.
31/31 valid epochs · robust scatter 2.79% · median conditional error 3.68%. 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.
31/31 valid epochs · robust scatter 2.36% · median conditional error 4.19%. 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.
31/31 valid epochs · robust scatter 3.52% · median conditional error 4.23%. 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.
31/31 valid epochs · robust scatter 6.29% · median conditional error 6.20%. 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.
31/31 valid epochs · robust scatter 3.76% · median conditional error 3.79%. 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.
31/31 valid epochs · robust scatter 2.59% · median conditional error 3.09%. 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.
31/31 valid epochs · robust scatter 2.88% · median conditional error 4.02%. 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.
31/31 valid epochs · robust scatter 3.88% · median conditional error 5.32%. 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.
31/31 valid epochs · robust scatter 5.54% · median conditional error 5.90%. 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.
3 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.
2026-09-29 · DNB · Gaia 423548410359174784. First available session and source ID; not selected for apparent variability.
2026-09-29 21:51:48 CEST (UTC+0200) → 2026-09-30 00:46:38 CEST (UTC+0200)
87.5% Moon illumination · saved calculation
Altitude 35.9°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.
DNB · Star shape: 31/31 valid selected exposures; archive 139/139 frames, 4 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
DNB · Star width (FWHM): 31/31 valid selected exposures; archive 139/139 frames, 4 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
DNB · Background scatter: 31/31 valid selected exposures; archive 139/139 frames, 4 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
DNB · Stellar SNR: 31/31 valid selected exposures; archive 31/31 frames, 1 Sessions. Unknown properties: device_id, readout_mode, optical_configuration, filter.
DNB · Background: 31/31 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
5 selected frames worth reviewing · 31/31 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? |
|---|---|---|---|---|
| 2026-09-29T19:51:48.407618 b43cc74da1cf | Background scatter | 23.61 ADU | 23.13 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-29T20:01:54.629931 9f3376f436d5 | Background scatter | 23.54 ADU | 23.13 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-29T20:07:12.288030 ea5de9307f18 | Background scatter | 23.54 ADU | 23.13 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-29T20:22:36.458787 1fca65d7fdb3 | Background scatter | 23.54 ADU | 23.13 | Higher saved background scatter; this is not pure detector noise. |
| 2026-09-29T22:41:38.007691 95374a1b97b4 | Star width (FWHM) | 3.321 sensor pixels | 2.956 | Broader than this session; inspect focus, tracking and sampling. The cause is not identified. |
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_4fd2500f: Background level 31/31; Background scatter 31/31; Detected sources 31/31; Star eccentricity 31/31; Star width (FWHM) 31/31; Stellar SNR estimate 31/31. 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.
The history follows the research notes citing Barnard's original discovery reports. The discovery year is shown without assigning a disputed exact day; publication dates are not the observing date.
