siderust 0.7.0

High-precision astronomy and satellite mechanics in Rust.
Documentation 
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// SPDX-License-Identifier: AGPL-3.0-or-later
// Copyright (C) 2026 Vallés Puig, Ramon

//! Frame rotation implementations targeting [`ICRS`](crate::coordinates::frames::ICRS).
//!
//! ## Scientific scope
//!
//! The **International Celestial Reference System (ICRS)** is the IAU's
//! primary celestial reference system, realised by the International Celestial
//! Reference Frame (ICRF) from extragalactic radio-source positions. It
//! supersedes the older equinox-based frames and serves as the hub through
//! which all modern frame transformations are routed.
//!
//! This module implements two inverse rotation chains targeting ICRS:
//!
//! - **EclipticMeanJ2000 → ICRS**: inverse of `icrs_to_ecliptic_j2000`.
//! - **EquatorialMeanJ2000 → ICRS**: inverse frame bias `rb⁻¹`.
//!
//! ## Technical scope
//!
//! Both impls apply fixed 3×3 rotations from [`bias`]:
//!
//! - `ecliptic_j2000_to_icrs()` = `(Rx(ε₀) · rb)⁻¹`.
//! - `frame_bias_j2000_to_icrs()` = `rb⁻¹`.
//!
//! Spherical types are handled by the blanket impl in the parent module via
//! a Cartesian round-trip.
//!
//! ## References
//!
//! - Ma, C. et al. (1998). *Astronomical Journal*, 116, 516 — ICRF definition.
//! - SOFA routine `iauBp06`.

use super::bias;
use super::TransformFrame;
use crate::coordinates::{cartesian::Position, centers::ReferenceCenter, frames};
use crate::qtty::LengthUnit;

// Implement Transform trait for EclipticMeanJ2000 -> ICRS
impl<C: ReferenceCenter, U: LengthUnit> TransformFrame<Position<C, frames::ICRS, U>>
    for Position<C, frames::EclipticMeanJ2000, U>
{
    fn to_frame(&self) -> Position<C, frames::ICRS, U> {
        let rot = bias::ecliptic_j2000_to_icrs();
        let [x, y, z] = rot * [self.x(), self.y(), self.z()];
        Position::from_array(self.center_params().clone(), [x, y, z])
    }
}

// Implement Transform trait for EquatorialMeanJ2000 -> ICRS (frame bias inverse)
impl<C: ReferenceCenter, U: LengthUnit> TransformFrame<Position<C, frames::ICRS, U>>
    for Position<C, frames::EquatorialMeanJ2000, U>
{
    fn to_frame(&self) -> Position<C, frames::ICRS, U> {
        let rot = bias::frame_bias_j2000_to_icrs();
        let [x, y, z] = rot * [self.x(), self.y(), self.z()];
        Position::from_array(self.center_params().clone(), [x, y, z])
    }
}

#[cfg(test)]
mod tests {
    use super::*;
    use crate::coordinates::centers::Barycentric;
    use crate::macros::assert_cartesian_eq;
    use crate::qtty::AstronomicalUnit;

    #[test]
    fn ecliptic_roundtrip_through_icrs_preserves_vector() {
        let ecl = Position::<Barycentric, frames::EclipticMeanJ2000, AstronomicalUnit>::new(
            0.0, 1.0, 1.0,
        );
        let icrs: Position<_, frames::ICRS, AstronomicalUnit> = ecl.to_frame();
        let back: Position<_, frames::EclipticMeanJ2000, AstronomicalUnit> = icrs.to_frame();

        assert_cartesian_eq!(ecl, back, 1e-12);
    }

    #[test]
    fn equatorial_mean_j2000_to_icrs_is_bias_only() {
        let eq = Position::<Barycentric, frames::EquatorialMeanJ2000, AstronomicalUnit>::new(
            1.0, -2.0, 0.5,
        );
        let icrs: Position<_, frames::ICRS, AstronomicalUnit> = eq.to_frame();
        let back: Position<_, frames::EquatorialMeanJ2000, AstronomicalUnit> = icrs.to_frame();

        assert_cartesian_eq!(eq, back, 1e-12);
    }
}