Signals#

Signal utilities: formatting and photon flux.

phise.modules.signals.as_str(signals: ndarray) → str[source]#

Return a compact text representation of a signal vector.

Each complex entry is displayed as amplitude · exp(i·phase) and its intensity abs(s)**2.

Parameters:

signals – Complex amplitudes array, shape (N,) or (N, M).

Returns:

Formatted string listing telescopes and their signals.

phise.modules.signals.photon_flux(
λ: Quantity,
Δλ: Quantity,
f: Quantity,
a: Quantity,
η: float,
m: float,
) → Quantity[source]#

Compute the photon detection rate for a star (photons per second).

Formula: Ṅ ≈ f · a · η · δν · 10^{-m/2.5} / (h c / λ), with δν ≈ c Δλ / λ².

Parameters:

  • λ – Central wavelength (length Quantity, e.g. u.m).

  • Δλ – Spectral width (same length unit as λ).

  • f – Object spectral flux (e.g. W·m⁻²·Hz⁻¹ or compatible).

  • a – Telescope collecting area (area Quantity, e.g. u.m**2).

  • η – Optical throughput (0–1).

  • m – Stellar magnitude (astronomical logarithmic scale).

Returns:

Detection rate in photons / s (Quantity 1 / u.s).