plesty.pow_pl.viz

Watch a power-PL run — live, replayed, or rendered to a video.

uv run python -m plesty.pow_pl.viz monitor                  # follow the newest run
uv run python -m plesty.pow_pl.viz monitor --replay 2 --record run.mp4
uv run python -m plesty.pow_pl.viz render --run D104-C_QD01_20261012

Everything about watching — which run, where the share is mounted, live or replayed, a window of its own or embedded in the bench console — is plesty.lib.monitor.Viz’s. The manifest names this module as the experiment’s viewer (viz), so the bench opens it on the runs it starts.

Four views follow the run: the newest spectrum; every spectrum so far against the wave-plate angle, in counts per second so the exposures of one angle compare; the excitation power against the angle; and the integrated emission against the power on log–log axes with its running exponent k — the number the analysis after the sweep (analysis) reports for the whole range.

What is this experiment’s own is read_spectrum(): a record names the file the spectrometer wrote, and turning it into columns is the one thing no shared view can do. Watching is passive: the views read committed records and the spectra they point at, and write nothing.

Attributes

`SPIKE_THRESHOLD`
`MIN_POINTS`
`viz`

Classes

`PowerLaw`	Integrated emission against power on log–log axes, with the running exponent.
`RateMap`	The library's map, of every spectrum in counts per second without cosmic rays.

Functions

`remove_spikes`(→ numpy.ndarray)	Replace single-pixel spikes (cosmic rays) by the mean of their neighbours.
`read_spectrum`(→ dict[str, Any])	Turn the file a record names into the columns the views want.
`_band`(→ numpy.ndarray)	Pixels inside band, or every pixel when no band is given.
`integrated`(→ tuple[numpy.ndarray, numpy.ndarray])	Power (µW) and integrated emission (counts/s) of every spectrum so far.

Module Contents

plesty.pow_pl.viz.SPIKE_THRESHOLD = 20.0

plesty.pow_pl.viz.MIN_POINTS = 4

plesty.pow_pl.viz.remove_spikes(counts: numpy.ndarray) → numpy.ndarray

Replace single-pixel spikes (cosmic rays) by the mean of their neighbours.

A spike stands more than SPIKE_THRESHOLD noise levels above the brighter of its two neighbours and more than twice that neighbour; the peak of an emission line fails the second test, so lines pass unchanged.

Parameters:: counts (numpy.ndarray) – One spectrum.
Returns:: The spectrum with single-pixel spikes replaced.
Return type:: numpy.ndarray

plesty.pow_pl.viz.read_spectrum(row: Any, run: Any) → dict[str, Any]

Turn the file a record names into the columns the views want.

Called once per row and cached, so the views load each spectrum once between them.

Parameters:

row (Any) – One committed record.
run (Any) – The run it belongs to; run.local translates the acquiring host’s path onto this machine.

Returns:

wavelength; counts as recorded; rate, the spectrum without cosmic rays in counts per second; and power_uw. Nothing for a row that names no spectrum.

Return type:

dict[str, Any]

plesty.pow_pl.viz._band(wavelength: numpy.ndarray, band: Sequence[float] | None) → numpy.ndarray

Pixels inside band, or every pixel when no band is given.

Parameters:

wavelength (numpy.ndarray)
band (Optional[Sequence[float]])

Return type:

numpy.ndarray

plesty.pow_pl.viz.integrated(data: Any) → tuple[numpy.ndarray, numpy.ndarray]

Power (µW) and integrated emission (counts/s) of every spectrum so far.

The same reduction as the analysis: each spectrum minus its background (the median of analysis.background_nm, or of the whole spectrum), summed over analysis.region_nm (or every pixel).

Parameters:: data (Any) – The run’s RunData.
Returns:: Two arrays, one value per spectrum that has a power.
Return type:: tuple[numpy.ndarray, numpy.ndarray]

class plesty.pow_pl.viz.PowerLaw(title: str = '', *, name: str = '', weight: float | None = None, area: str = '')

Bases: plesty.lib.monitor.Plot

Integrated emission against power on log–log axes, with the running exponent.

Name the view.

Parameters:

title (str) – Overrides the class attribute.
name (str) – Layout key; defaults to the title.
weight (Optional[float]) – Overrides the class attribute.
area (str) – Overrides the class attribute.

title = 'Integrated emission against power'

draw(data: Any) → list[Any]

Every spectrum so far as a point, and the fitted line once there are enough.

Parameters:: data (Any)
Return type:: list[Any]

class plesty.pow_pl.viz.RateMap(values: str = 'counts', row: str = '', *, x: str = 'wavelength', title: str = '', name: str = '', weight: float | None = None, area: str = '', color: str = 'violet', scale: str = 'sqrt', x_label: str = 'Wavelength (nm)', y_label: str = '')

Bases: plesty.lib.monitor.common.SpectrumMap

The library’s map, of every spectrum in counts per second without cosmic rays.

Per second, because each angle may be measured at several exposures; without cosmic rays, because the colour scale runs from the lowest value to the highest and one ray would leave every emission line dark.

Stack values across rows, against row.

Parameters:

values (str) – Field holding each row’s array.
row (str) – Field holding the swept coordinate, for the axis; empty numbers the rows instead.
x (str) – Field holding the sample axis, shared by every row — so the map is drawn in the same units as the spectrum above it. "", or a field no row carries, numbers the samples.
title (str) – What the view is called.
name (str) – Layout key.
weight (Optional[float]) – Relative size.
area (str) – Which side of the window it starts on.
color (str) – Palette token the colour map is built from.
scale (str) – "sqrt" or "linear".
x_label (str) – Axis label of the sample axis.
y_label (str) – Axis label of the swept axis.

block(data: Any) → Any

Stack the per-second spectra rather than the recorded counts.

Parameters:: data (Any)
Return type:: Any

plesty.pow_pl.viz.viz