When the signal of a black-hole merger reaches Earth,

it does not arrive as a clean sound or a perfect curve. It appears as a brief, faint disturbance buried inside a much longer stream of detector noise.

Published gravitational-wave results usually summarise an event through quantities such as mass, spin, distance and ringdown frequency. Those measurements are essential, but I wanted to examine what happens before the signal is reduced to a set of numbers.

The Black Hole Waveform Morphology Pipeline is an independent project using public strain data from the Gravitational Wave Open Science Center. Its purpose is to study the observable shape of each merger and preserve as much information as the data genuinely supports.

The basic rule is:

Examine the waveform first. Interpret it afterwards.

What the pipeline does

Each analysis begins by confirming that genuine detector strain has been obtained and that the required science segments are valid. The signals from the available detectors are then aligned and examined separately as well as together.

The pipeline studies the changing shape and frequency of the waveform through the inspiral, merger and ringdown. It also checks whether a possible feature appears in more than one detector, survives changes to the analysis window and remains unusual when compared with nearby noise.

This matters because noise can produce surprisingly convincing oscillations. A precise-looking frequency is not necessarily a real measurement.

Earlier versions of the pipeline repeatedly found apparent clustering near 100 Hz. Other runs produced estimates around 322 Hz with a damping time of about 41 milliseconds. When those results were tested more carefully, they were not stable enough to be treated as properties of the black holes.

They were rejected.

That is a useful result. A trustworthy analysis must be able to discard an attractive number when the evidence does not support it.

Current results

The current V30 pipeline separates quick event screening from deeper analysis. The highest-resolution mode examines the data at 16,384 samples per second and applies expanded detector-consistency, window-stability and noise tests.

One of the latest validated datasets is GW240925_005809, recorded by the H1, L1 and V1 detectors with a reported network signal-to-noise ratio of approximately 31.96. It passed the pipeline’s real-data audit and provides a useful three-detector case for studying waveform agreement.

The printed reports include aligned detector strain, spectrograms, time-frequency structure, merger morphology and stability tests. Rather than forcing a single result from uncertain data, the reports show where the detectors agree, where they differ and which measurements remain unresolved.

The longer-term aim is to build a comparative catalogue of black-hole waveform fingerprints. Repeated structures can then be studied across different detectors, time windows and merger events.

This is not a claim of new physics, a challenge to General Relativity or an attempt to prove the Differential Expansion Framework. Established gravitational-wave physics remains the reference point. Alternative interpretations should only be considered after a feature has survived the observational tests.

Black-hole mergers give us only a fraction of a second of visible motion. Within that fraction may be details that are lost when the waveform is reduced too quickly to a few fitted parameters.

The aim of this project is to keep those details visible for as long as the data allows.

Results, reports and future updates will be published here at imsn.co.uk. Technical criticism and suggestions for improving the pipeline are welcome.