Star Profiler v1 and v2

Purpose and expected result

The paired windows use byte-identical copies of one field to compare the detected-star tables and version-specific controls without competing for a single target.

Both Star Profiler windows analyze the image a view shows without modifying it. They draw selectable detections over the image, expose a sortable measurement table, can curate that list, save it for later use, and create a new grey star mask. Both find their stars with one fitted detector: each candidate is fitted with a rotated Gaussian or Moffat profile, and a poor fit is rejected. The two windows differ in what they ask and show:

• v1 asks for a threshold, a roundness tolerance and a size window, and shows thirteen columns, each stated from the fitted star. It reads and writes .anspv1 profiles.
• v2 offers the detector's own controls, shows its fitted figures, places every star on the sky through the image's plate solution and matches it against a configured local Gaia catalog. It reads and writes .anspv2 profiles.

For new measurement and registration work, start with v2. Keep v1 for .anspv1 workflows.

At a glance

Item	Star Profiler v1	Star Profiler v2
Menu path	Process > Star Processing > Star Profiler v1	Process > Star Processing > Star Profiler v2
Input	The image the view shows: a still image, or the frame a sequence view shows.	Same.
Detection data	A colour image's green channel; a grey image's only channel.	Green by default; Use Lightness detects on CIE L*. A grey image's only channel.
Core model	The fitted detector at its defaults, keeping stars whose amplitude stands the threshold above the sky, whose two fitted standard deviations differ by less than the roundness tolerance and whose mean full width lies in the size window.	The fitted detector at the dialog's request: background-noise threshold, candidate scan, rotated Gaussian or free-beta Moffat fit.
Units	Every representation is read as fractions of its full scale, so amplitudes and backgrounds are fractions of full scale.	Same.
Positions	Engine pixel coordinates: the first pixel's centre is at one half.	Same.
Astrometry/catalog	None.	RA/Dec where the image's cards state a plate solution; Gaia matches, zero point and limiting magnitude when a local catalog is configured.
Profile format	JSON schema 1, extension .anspv1, engine v1.	JSON schema 2, extension .anspv2, engine v2.
Interoperability	Refuses a v2 profile by name.	Refuses a v1 profile by name. Profiled Starmask Recombination reads either.
Output	Saved profile or a new grey mask; the image is unchanged.	Same.
Preview/history	No preview and no history step.	Same.

Before you start

1. Use a calibrated, linear image. Strong gradients, hot pixels, clipping, and nonlinear stretching alter detection and fitted widths.
2. Keep display stretch fixed while comparing images; measurements come from the image's samples, not the displayed stretch.
3. Decide whether compatibility requires .anspv1. A profile cannot be converted by renaming its suffix.
4. For v2 astrometry, plate solve the image first. Configure a local Gaia catalog only if catalog matches and the zero point are needed.

Procedure

1. Activate the image and open the required version from Process > Star Processing. The window is bound to that view; there is no target selector.
2. For v2, start with Gaussian, Radius 5, Threshold 1.0, and Roundness Threshold 0.5. On RGB, decide whether green or Use Lightness is the representative detection plane. For v1, start from its four defaults.
3. Click Detect Stars. The detection runs in the background behind a progress window whose Cancel stops it; the application stays responsive. Select rows or click an overlay to cross-highlight a star. Click a column header to sort; enable Center Selected Star only when automatic recentering is useful.
4. Inspect missed stars, hot pixels, saturated cores, and elongated detections. Change one detection control at a time and run detection again.
5. Use Stars Filter for post-detection curation. Preview is non-destructive; OK asks before discarding excluded stars.
6. Save Profile before closing if another process or session needs the list. Use Create Mask when a grey mask is the required output.

Complete parameter and action reference

Star Profiler v1 window

UI label/action	Type and unit	Runtime default	Persisted-default exception	Valid values, step, or constraints	Effect of increasing, decreasing, or selecting	Dependencies and enable/visibility rules	Quality, artifact, runtime, memory, or disk trade-off	Scope: preview/apply, channel, mask, still/sequence	Persistence
Detection Threshold	Fraction of full scale above the sky	0.10	Loaded profiles do not repopulate this control	0.01–1.00; step 0.01	The smallest fitted amplitude a star may have. Higher keeps only brighter stars.	Used on the next Detect Stars.	Low values keep faint stars and the fits of noise; high values miss faint stars.	Green or grey plane	Window lifetime only; Reset/reopen returns 0.10; recorded in saved profiles.
Roundness Tolerance	Pixels	2.00	Loaded profiles do not repopulate this control	0.00–10.00; step 0.01	The largest difference of a star's two fitted standard deviations. Lower requires rounder stars.	Used on the next detection.	High values admit elongated or nonstellar objects; very low values reject real stars.	Detection	Window lifetime; recorded in profiles.
Min Size	Pixels	2	None	0–99; integer	The smallest mean full width kept.	Must not exceed Max Size for useful output; the dialog does not enforce the order.	High values reject small or faint stars; low values admit hot pixels.	After the fit	Window lifetime; recorded in profiles.
Max Size	Pixels	25	None	0–99; integer	The largest mean full width kept.	Must be at least Min Size for useful output.	High values keep large or saturated structures; low values reject large stars.	After the fit	Window lifetime; recorded in profiles.
Detected Stars table	Sortable read-only table	Empty	A loaded profile fills it	Columns: x, y, intensity, percentage, deltaRadius, quality, radius, meanRadius, four axis radii, majorAxisAngle	Select a row to highlight its overlay; click a header to sort, largest first and then smallest. A detection shows the brightest first.	Available after detection or load.	Sorting changes the list's order, not its measurements.	Current curated list	The order is saved, because stars are written in the current order.
Detect Stars	Button	—	—	One detection at a time	Replaces the current list from the view's image using the controls as they were when it was pressed.	Disabled while a detection runs.	Runs on a worker; Cancel, Clear, a Load the window accepts or closing the window stops it and nothing is shown. A Load the window refuses leaves it running.	Analysis only; the image is unchanged	The result remains until replaced, cleared or closed.
Reset	Button	—	—	Click action	Restores the four detection defaults.	Does not clear the stars.	No computation.	Controls only	No preset persistence.

The v1 columns are stated from the fitted star: intensity is the fitted amplitude; quality the brightness-weighted roundness figure C below; radius half the mean full width; meanRadius the radius times 1.5/2.35; the four axis radii half the major and minor full widths; deltaRadius half their difference; majorAxisAngle the fitted position angle; and percentage 1 for every star.

Star Profiler v2 window

UI label/action	Type and unit	Runtime default	Persisted-default exception	Valid values, step, or constraints	Effect of increasing, decreasing, or selecting	Dependencies and enable/visibility rules	Quality, artifact, runtime, memory, or disk trade-off	Scope: preview/apply, channel, mask, still/sequence	Persistence
Radius	Candidate-search half-window; pixels	5	Loaded profiles do not repopulate this control	3–32; integer	Larger requires a candidate to dominate a wider box; smaller separates compact, crowded stars.	Used on the next detection.	Large values merge crowded structures and need a larger frame; small values admit more candidates.	Candidate scan	Window lifetime; saved in profile.
Threshold	Background-noise multiplier	1.00	None	0.01–15.00; step 0.05	The detection threshold is the sky plus 5 × Threshold × background noise.	Used on the next detection.	Lower finds fainter, noisier candidates and costs more; higher misses faint stars.	Selected detection plane	Window lifetime; saved as sigma.
Amplitude Range	Checkable group	Off after initialization/reset	—	Off/On	On rejects fitted amplitudes outside the Minimum/Maximum interval, as fractions of full scale; off applies no amplitude window.	Bounds matter only when checked.	Narrow bounds can remove valid or saturated stars.	Post-fit rejection	Check state window-only; bounds saved when it is on.
Amplitude Range > Minumum	Fraction of full scale; UI spelling	0.00	None	0.00–0.99; step 0.05	Higher removes lower-amplitude fits.	Amplitude Range on.	Suppresses weak candidates and faint stars alike.	Post-fit rejection	Saved as min_A.
Amplitude Range > Maximum	Fraction of full scale	1.00	None	0.01–1.00; step 0.05	Lower removes higher-amplitude fits.	Amplitude Range on; a Maximum below the Minimum refuses the detection with a message.	Can reject bright stars needed for alignment.	Post-fit rejection	Saved as max_A.
Roundness Threshold	Minimum axis ratio	0.50	None	0.01–0.95; step 0.05	Higher requires FWHMy/FWHMx closer to one.	Always used.	High values reject elongated stars but can leave too few.	Post-fit rejection	Saved as roundness.
Roundness Range > Maximum	Optional maximum axis ratio	Group off; value 1.00	None	0.01–1.00; step 0.05	When enabled, lower rejects fits rounder than the bound.	Checkable group; off is a maximum of 1.0.	Usually leave off; a narrow band can empty the list.	Post-fit rejection	Effective maximum saved as max_r.
Convergence	Solver iteration multiplier	1	None	1–3; integer	Multiplies the fit's iteration budget.	Used on the next detection.	Higher can rescue difficult fits at CPU cost.	Per-candidate fit	Saved in profile.
Relax PSF Checks	Checkbox	Off	None	Off/On	Skips the scan's symmetry and local-contrast tests and the width-estimate and residual checks; amplitude, beta, geometry, magnitude and roundness checks remain.	Used on the next detection.	Finds more difficult stars and more blends and poor fits.	Candidate and fit validation	Saved in profile.
Profile Type	Selector	Gaussian	None	Gaussian, Moffat	Gaussian fits exponential wings; Moffat fits power-law wings with a free exponent.	Minimum Beta is enabled only for Moffat.	Moffat has one more parameter.	Per-star model	Saved as gaussian or moffat_bfree.
Minimum Beta	Dimensionless	1.50; disabled for Gaussian	None	0.05–10.00; step 0.05	Higher rejects broad-wing, low-beta fits.	Moffat only.	Too high rejects valid winged stars.	Moffat rejection	Saved in profile.
Use Lightness	Checkbox	Off	Reset does not change it	Off/On	On detects a colour image's stars on CIE L*; off on green. A grey image is always its only channel.	Meaningful for colour images.	L* is less tied to one channel; green may have the best signal on OSC data.	Detection plane	Window lifetime; not stored in .anspv2.
Detected Stars table	Sortable read-only table	Empty	A loaded profile fills it	Columns, in order: x, y, Mag, FWHMx, FWHMy, Ra, Dec, Angle, B, A, Beta, r, RMSE, FWHM, Circularity; the widths are shown in pixels	Select or click an overlay to cross-highlight; click a header to sort. Mag is an instrumental -2.5 log10(background-subtracted box sum), not a calibrated magnitude.	RA/Dec need a plate solution; Beta is - for Gaussian.	—	Current curated list	The order and every field are saved.
Detect Stars	Button	—	—	One detection at a time	Replaces the list, then places it on the sky and matches it against the local Gaia catalog.	Disabled while a detection runs.	Runs on a worker behind a progress window whose Cancel stops it.	Analysis only; the image is unchanged	The result remains until replaced, cleared or closed.
Reset	Button	—	—	Click action	Restores the detection controls and turns both range groups off.	Does not change Use Lightness or clear the stars.	No computation.	Controls only	No preset persistence.

Actions shared by both versions

UI label/action	Type and unit	Runtime default	Persisted-default exception	Valid values, step, or constraints	Effect of increasing, decreasing, or selecting	Dependencies and enable/visibility rules	Quality, artifact, runtime, memory, or disk trade-off	Scope: preview/apply, channel, mask, still/sequence	Persistence
Load Profile	File action	—	Remembers a version-specific folder	v1 reads .anspv1 documents, v2 .anspv2 ones; the schema is read from the document	Reads the document in the background; only once the window accepts it does it replace the list and stop a detection on its way. A document of the other generation, or one that cannot be read, is refused by name and changes nothing: the list stays, and a detection on its way runs on and shows its stars as usual. It does not apply the saved detector settings to the controls or check the document against the image.	Always available.	Bounded to 64 MB and one million stars.	Current window only	The folder persists; the profile comes from the file.
Save Profile	File action	Disabled initially	Remembers a version-specific folder	Requires a nonempty list	Writes the document in the background - the detector settings, the frame's figures and the stars, and in a v1 document the edited-by-hand flag, which the v2 schema does not hold - to a pending file renamed into place when complete.	Enabled after detection or load.	v2 files carry fits, uncertainties, astrometry and catalog fields.	Curated list only; no pixels	The file persists.
Stars Filter	Button/dialog	Disabled initially	—	Requires a populated list	Opens the version-specific filter preview below. It is shown beside the window, not modal.	Enabled after detection or load.	Applying removes excluded stars after confirmation.	Overlay, list, profile, mask input	An applied filter marks the profile edited by hand; save to keep it.
Create Mask	Button/dialog	Disabled initially	—	Requires a populated list	Opens Profiled Mask Generation beside the window, not modal, over the current list.	Enabled after detection or load.	The mask is painted in the background.	New image only	The new view is not saved automatically.
Remove selected star	Icon button	Disabled until a selection	—	One selected row	Removes that star from the list and the overlay and marks the profile edited by hand.	Disabled with no selection.	Deletion does not recalculate the profile's frame figures.	Current list	Save afterward to keep it.
Clear	Button	Disabled initially	—	Confirmation required	Removes every star after Yes, and stops a detection or read on its way.	Enabled for a populated list.	Destructive in memory.	Current list	Reload or redetect to recover.
Detected Stars	Count display	0	—	Read-only	The current list's size.	Always visible.	—	Current list	Not separately persisted.
Center Selected Star	Checkbox	Off; disabled initially	—	Off/On	Centers the view on a selected star.	Enabled for a populated list; enables the zoom factor.	Display only.	Viewer navigation	Window lifetime.
x Zoom	Numeric zoom factor	2	—	1–20	Higher zooms further when centering.	Enabled with Center Selected Star.	Display only.	Viewer navigation	Window lifetime.
Image overlay/click	Viewer interaction	No overlay	Saturated fits are drawn apart	Left-click inside a drawn star selects its row	Each star's fitted ellipse is drawn at its engine pixel coordinate; a click selects the star it lands in, found in the list by its position, so a filter's preview selects the right row.	Populated list required.	Dense fields can be crowded.	Display only	Not saved in the image.
Close	Button/window action	—	—	Confirmation appears whenever the list is nonempty	Closes after confirmation and stops a detection on its way; the window closes once it has landed.	Can be refused with No.	Unsaved curation is lost.	Process window	Saved profiles and new masks survive.

Stars Filter dialog

UI label/action	Type and unit	Runtime default	Persisted-default exception	Valid values, step, or constraints	Effect of increasing, decreasing, or selecting	Dependencies and enable/visibility rules	Quality, artifact, runtime, memory, or disk trade-off	Scope: preview/apply, channel, mask, still/sequence	Persistence
v1 Intensity Min/Max	Data-derived range	Full observed range	—	Current list extrema	Narrows the fitted amplitude kept.	v1 only.	Can remove faint or bright stars.	Current list	Dialog only until OK.
v1 Quality Min/Max	Data-derived range	Full observed range	—	Current list extrema	Narrows the brightness-weighted roundness figure kept.	v1 only.	Combines brightness and shape.	Current list	Dialog only until OK.
v1 Radius Min/Max	Data-derived pixels	Full observed range	—	Current list extrema	Narrows half the mean full width kept.	v1 only.	Excludes hot pixels or very large structures.	Current list	Dialog only until OK.
v2 Mag Min/Max	Data-derived instrumental magnitude	Full observed range, faint end in Min	—	Current list extrema	Keeps the magnitudes between the two ends; a star with no magnitude is not kept.	v2 only.	Uncalibrated box magnitude.	Current list	Dialog only until OK.
v2 FWHMx Min/Max	Data-derived pixels	Full observed range	—	Current list extrema	Narrows the major full width.	v2 only.	Isolates sharp stars or rejects broad fits.	Current list	Dialog only until OK.
v2 FWHMy Min/Max	Data-derived pixels	Full observed range	—	Current list extrema	Narrows the minor full width.	v2 only.	Combine with FWHMx to avoid shape bias.	Current list	Dialog only until OK.
Random selection	Percentage	100%	—	0–100%	Keeps that share of the stars the ranges kept, chosen from a seed the dialog draws when it opens: the same request keeps the same stars until it is opened again.	Both versions.	For sparse masks and testing.	Current list	Dialog only until OK.
Include Neighbors	Checkbox	Off	—	Off/On	Adds the stars whose boxes overlap a kept star's, and so on from them.	Effective when a range or the random share leaves stars out.	Grows the selection in dense fields.	Current list	Dialog only until OK.
Preview	Checkbox	On	—	Off/On	Updates the overlay and count while tuning; closing or Cancel restores the original list.	Both versions.	—	Overlay only until OK	Not persisted.
OK / Reset / Cancel	Buttons	—	—	—	OK replaces the list after confirmation; Reset restores the full ranges and 100%; Cancel restores the original list.	—	—	Current list	Save the profile to keep it.

Profiled Mask Generation dialog

The dialog paints the current list, on a worker, into a new grey 32-bit float mask of the image's size in the unit interval, whatever the source's representation, and opens it beside the view as <source> - STARMASK whether the dialog is still open or not. Binary Areas paints each star's fitted ellipse, scaled by Scale Factor and blurred by Soften Edges, an exact Gaussian; Shaped Areas paints a radial falloff of Shape, its radius multiplied by % Pixel Increase (a multiplier, 0.5 halves it) and grown by Pixel Increase pixels. Its defaults are Binary, scale 1, soften 0, multiplier 0.5, additive 0 and Truncated Bell.

How the algorithm works

The one detector

1. The image is copied and read as fractions of its representation's full scale. Samples the image's validity rule rejects, and samples that hold no number, are left out; the stars are found in a colour image's green channel, or its CIE L* when v2 asks, or a grey image's only channel.
2. The detector measures the sky B, the background noise n and the largest sample, smooths the plane with an exact Gaussian, and scans for candidates above

[ T=B+5sn, ]

where s is v2's Threshold (one for v1). A candidate must dominate a box of Radius (five for v1); symmetry, local contrast, duplicates and saturated plateaus are assessed before fitting. 3. Each candidate is fitted by nonlinear least squares. In rotated coordinates (x',y'), the Gaussian and Moffat models are

[ G=B+A\exp!\left[-\left(\frac{x'^{2}{S_x}+\frac{y'}2}{S_y}\right)\right], ]

[ M=B+A\left(1+\frac{x'^{2}{S_x}+\frac{y'}2}{S_y}\right)^{-\beta}. ]

A position is measured with every sample at its pixel's centre, so the first pixel's centre is at one half. A fit that does not converge, a nonpositive width, poor roundness, an excessive width or residual, an amplitude outside the window and a low Moffat beta are rejected. 4. Per-star metrics are

[ r=\frac{\mathrm{FWHM}_y}{\mathrm{FWHM}_x},\quad \mathrm{FWHM}=\frac{\mathrm{FWHM}_x+\mathrm{FWHM}_y}{2},\quad C=\frac{A}{0.1+|\mathrm{FWHM}_x-\mathrm{FWHM}_y|}. ]

C is Circularity in v2 and quality in v1; it is not a dimensionless shape ratio. The frame's figures are medians, and its quality is count × median roundness / median FWHM over unsaturated stars. 5. v1 then keeps the stars whose amplitude is at least Detection Threshold, whose standard deviations FWHM_x/2.35482 and FWHM_y/2.35482 differ by less than Roundness Tolerance, and whose mean full width lies between Min Size and Max Size.

v2: the sky and the catalog

If the image's header states a plate solution, each star's position is projected through it to RA/Dec. If a configured local Gaia catalog is installed, its stars inside the field, carried to the image's observation epoch - counted in Julian years from J2000.0 (2000-01-01 12:00) - are matched one to one with the stars within five arcseconds, to G magnitude 16. The matched stars' box sums fit the G zero point, and the faintest match is the limiting magnitude.

Parameter interactions and starting points

Combination	Conservative starting point	Too weak looks like	Too strong looks like	Adjustment order
v2 Threshold + Radius	1.0, radius 5	Faint stars missing	Noise, blends, slow fitting	Choose the radius for the field's crowding -> lower the threshold gradually
v2 Roundness + Relax checks	Roundness 0.5, Relax off	Elongated usable stars rejected	Trails, blends, poor fits retained	Tune roundness first -> enable Relax only for a diagnosed rejection
Gaussian + Moffat/beta	Gaussian first	Winged stars show larger RMSE	Free-beta fits rejected	Compare the same stars -> switch to Moffat -> tune minimum beta last
v1 Threshold + Size window	0.10, 2–25	Faint stars missing or large stars excluded	Hot pixels and nebular knots kept	Fix the size window -> lower the threshold
Detection + post-filter	Broad but credible detection, then a narrow filter	Useful stars absent before curation	The filter biases the frame's figures	Fix detection -> inspect the table -> preview the filter -> save

Inputs, outputs, and metadata

• Neither version changes the image or adds a history step. A profile is a JSON file holding measurements, detector parameters and the list's order; it holds no pixels, image size or image identity.
• Positions are engine pixel coordinates; a profile is read and written as it stands, with no half-pixel shift.
• A v1 profile writes every column as the table shows it, except that its radius and meanRadius fields are four times the table's figures. Read back, a v1 window keeps only each star's position, amplitude and mean width: the star is round, of the width it was written with, with quality 1 and no angle.
• A v2 profile holds every fitted figure, the RA/Dec and the catalog match of each star - the entry's identifier, G magnitude, BP-RP colour and separation; the BP and RP magnitudes apart are written as zero - and the frame's figures.
• A loaded profile is drawn over the window's view. Loading another image's profile produces plausible table data with meaningless overlay positions.

Performance

Detection scales with image area and candidate count. A larger Radius, lower Threshold, Moffat, higher Convergence, Relax checks and dense fields cost more; a Gaia match reads only the catalog's tiles inside the field. Detection, loading, saving and mask painting run in the background, so the application stays responsive.

Worked example

• Evidence mode: Source-and-synthetic-test-derived.
• Input and settings: a plate-solved field of round Gaussian stars planted at stated engine pixel coordinates over a speckled sky, with a local Gaia catalog of those stars.
• Expected checkpoint: with either window's defaults every planted star is found within a tenth of a pixel of where it was planted; with v2 each star's RA/Dec is the solution's projection of its position and it matches its catalog entry; a saved profile is read back at the same positions.
• Limitation: no approved acquisition data was run, so no real-image detection completeness, mask quality or timing claim is made.

Warnings and limitations

• A v1 list is the fitted detector's: its columns are figures of the fit.
• A loaded .anspv1 profile keeps each star's position, intensity and radius and reads it as a round star of that radius: its stored quality, four axes, delta radius and angle are not kept, so saving it again writes a round star in their place.
• v2 Mag is uncalibrated. Gaia matches and the zero point do not replace that column with a catalog magnitude.
• The frame's figures are computed before manual deletion or filtering and are not recomputed afterward.
• Profiles do not bind themselves to an image. Verify the image before loading.
• Close does not track whether the list was saved; it asks whenever the list is nonempty.

Troubleshooting

Symptom or exact error	Verified cause/validation path	Recovery	Evidence source
No stars detected	Threshold too high, v1's size window excludes every star, or the chosen v2 plane is weak.	Reset, verify the plane, start at defaults, then lower the threshold or widen the size window.	FirstProfilerWindowTest.TheSizeWindowAndTheThresholdHoldTheStars
Error running Star Profiler	The detector refused the image - a frame too small to search, or a v2 amplitude or roundness range whose maximum is below its minimum.	Use a larger image or correct the range.	ADetectionTheEngineRefusesSaysWhyAndChangesNothing
Many hot pixels or noise detections	Threshold or size too permissive, or Relax checks on.	Raise the threshold; v1 raise Min Size; v2 disable Relax and inspect amplitude and FWHM.	Detector rejection rules
RA/Dec show -	The image's header states no plate solution.	Plate solve the image and detect again.	SecondProfilerWindowTest.AnUnsolvedImageIsProfiledWithoutWorldCoordinates
Gaia fields absent from a saved v2 profile	The image states no plate solution, or the local catalog is not configured, not ready or not readable; a catalog that cannot be read is logged with the reason.	Configure a local Gaia catalog, verify the solution, and detect again.	StarProfilerUnitsTest.WithoutACatalogTheStarsAreStillPlaced
Load Star Profile refusal	Wrong generation, malformed JSON, unsupported schema or a missing v2 field.	Open it in the matching window; restore an unedited profile.	AProfileOfTheOtherGenerationIsRefused, ARefusedReadLeavesTheRunningDetection
Loaded overlays do not align	Profiles carry positions but no image identity.	Load against the original image, or detect again.	Persistence source
Mask too small with % Pixel Increase 0.5	The value is a 0.5× multiplier.	Increase toward 1.0 and/or add Pixel Increase.	Mask creator source

Related workflow steps

Use Plate Solving before v2 when RA/Dec or catalog matches matter. Profiles feed Profiled Starmask Recombination, while generated masks can be used anywhere an image mask is accepted. For a direct mask workflow see Star Mask. Use Image Registration for transforming images rather than measuring detections.

References and provenance

• The fitted detector's candidate scan and fit derive from the Siril star finder and PSF implementation, by Francois Meyer and team free-astro (GPL-3.0-or-later).
• The radial profiles of the generated masks are adapted from DeepSkyStacker's star-mask shapes, under the BSD 3-Clause License of Luc Coiffier and the DeepSkyStacker contributors; Help > About AfterNight credits both works.
• The world coordinates use the image's plate solution and the catalog matches the installed local Gaia DR3 catalog.