Merge the solar-system branch, so the star catalogue lands on the sky it now shares

Both branches changed the system view's star, the body card's provenance line, the exoplanet
fetch and the ETL's validators. Resolved by keeping both sides:

- The system view's star is the catalogue's (its own radius and temperature, a limb-darkened
  surface in its colour) and turns like a planet when it is the Sun (the solar branch's IAU pole
  and 25.38-day turn), keyed on SUN_STAR_ID, since the catalogue branch dropped the scene's own
  SOL_STAR_ID. Framing takes the outermost thing drawn (an eccentric orbit's aphelion, from the
  solar branch) and the star's radius for a giant (from the catalogue). The solar branch's comment
  about a halo is dropped: there has been none since #33.
- The card's no-temperature sentence is the catalogue's (the host's luminosity or the orbit's size,
  not "not in the catalogue", which holds for 27 planets) and ends with the solar branch's reason
  why no image is used (a point of light for the 101 imaged planets, none for the rest).
- fetchExoplanets reads the composite table and the distance errors (catalogue) and the imaged
  list (solar); build.ts runs both branches' validators.

The data were regenerated by the full ETL on the merged code, from cache (nothing refetched):
stars.bin, stars-meta.bin, stars-index.json and deepsky.json come out byte for byte the catalogue
branch's, bodies.json the solar branch's, and exoplanets.json the catalogue branch's but for the
imaged flag on 101 planets, WASP-108 b not among them. Unit suite 977 passed, the two branches'
870 and 837 over their shared 730, so no test was lost.

Co-Authored-By: Claude Opus 5.5 (1M context) <noreply@anthropic.com>

src/app/shared/models/body.model.ts

@@ -1,7 +1,7 @@
 /**
- * Osculating Keplerian orbital elements at a reference epoch. Positions are derived
- * client-side by propagating these elements forward/backward from `epochJd` (see
- * `shared/astro/kepler.ts`), rather than fetching per-frame positions.
+ * Keplerian orbital elements at a reference epoch. Positions are derived client-side by
+ * propagating these elements forward/backward from `epochJd` (see `shared/astro/kepler.ts`),
+ * rather than fetching per-frame positions.
  */
 export interface OrbitalElements {
   semiMajorAxisAu: number;
@@ -14,29 +14,127 @@ export interface OrbitalElements {
 }
 
 /**
- * A solar-system planet, moon, or dwarf planet, sourced from JPL Horizons/SSD orbital
- * elements. `systemStarId` links back to the HYG star index (the Sun, see `SUN_STAR_ID`).
+ * How a body's mean elements move away from their epoch, per day.
+ *
+ * Mean elements rather than one osculating set, because the map's clock runs decades in minutes.
+ * An osculating orbit is exact at its instant and drifts from then on: fed to Kepler with a mass
+ * ratio, the Moon's went round in 27.70 days instead of 27.32 and was 66 degrees out after a year.
+ * A mean set carries its own measured motion, and the slow turning of its node and periapsis, so
+ * it holds for as long as its source was fit over.
+ */
+export interface MeanElementRates {
+  /**
+   * How fast the body goes round in space, in degrees per day: the rate of its mean longitude.
+   * 360 over this is its sidereal period.
+   */
+  meanMotionDegPerDay: number;
+  longitudeOfAscendingNodeDegPerDay: number;
+  argumentOfPeriapsisDegPerDay: number;
+  semiMajorAxisAuPerDay?: number;
+  eccentricityPerDay?: number;
+  inclinationDegPerDay?: number;
+  /**
+   * Standish's extra terms in the mean anomaly of Jupiter and beyond, `b T² + c cos(f T) +
+   * s sin(f T)` degrees, with T in Julian centuries from the epoch and f in degrees per century:
+   * the great-inequality wobble his 3000 BC to AD 3000 fit needs on top of its linear rates.
+   */
+  meanAnomalyTerms?: { b: number; c: number; s: number; f: number };
+}
+
+/**
+ * A solar-system planet, moon, or dwarf planet: JPL mean orbital elements, and JPL Horizons
+ * physical data. `systemStarId` links back to the HYG star index (the Sun, see `SUN_STAR_ID`).
  */
 export interface BodyRecord {
   id: string;
   systemStarId: number;
   name: string;
   kind: 'planet' | 'moon' | 'dwarf';
+  /** Mean radius: for a triaxial body, the radius of the sphere of its volume, which is how it is drawn. */
   radiusKm: number;
+  /**
+   * A triaxial body's three semi-axes, in km, largest first, where its shape is too far from a
+   * sphere for one radius to say it: Haumea's 1161 x 852 x 513 (Ortiz et al. 2017), whose mean
+   * radius is 798.
+   */
+  semiAxesKm?: readonly [number, number, number];
+  /** Mean elements at `orbit.epochJd`, moving at `rates`. */
   orbit: OrbitalElements;
+  rates: MeanElementRates;
+  /**
+   * The pole of the plane a moon's elements are measured against, where that is its local
+   * Laplace plane or, for Uranus's and Pluto's moons, the planet's equator: right ascension and
+   * declination in the ICRF. The node is then counted from where that plane crosses the ICRF
+   * equator. Absent means the J2000 ecliptic, as for the planets and the Moon.
+   */
+  laplacePole?: { raDeg: number; decDeg: number };
+  /** Where the elements come from and the span they hold over, as the card prints it. */
+  orbitSource: string;
+  /**
+   * The eccentricity the card prints, where it is not the orbit's own: Hyperion's row in the table
+   * its orbit is drawn from gives 0.0232, under a quarter of the 0.105 JPL's current table (SAT441)
+   * and Horizons (0.074 to 0.132 from 1980 to 2100) give. The older row still places Hyperion
+   * nearer where Horizons has it than the same row with 0.105 does, so the orbit keeps it.
+   */
+  measuredEccentricity?: number;
   /**
    * For `kind: 'moon'`, the `id` of the planet it orbits — its `orbit` is expressed
    * relative to that planet, not heliocentrically. Undefined for planets/dwarfs.
    */
   parentBodyId?: string;
+  /**
+   * For a moon heavy enough that it and its planet go round a point outside the planet — Charon,
+   * an eighth of Pluto's mass, puts it 2 100 km from Pluto's centre, 900 km above its surface —
+   * the moon's mass over the planet's, from the GMs on their Horizons pages. The planet's own
+   * elements then place that barycentre, as Standish's "Pluto" does, and both bodies are drawn
+   * going round it. Absent for every other moon.
+   */
+  massRatio?: number;
   /**
    * How the body turns on its own axis: the sidereal rotation period in hours, negative where
    * Horizons gives a negative rate (Venus, Uranus), and the tilt of that axis from its orbital
    * plane — which past 90 degrees already says the turn is retrograde.
    *
-   * Absent where Horizons publishes neither — the view then leaves the body still rather than
-   * spinning it at an invented rate.
+   * For a locked moon the period is its orbit's, from the mean motion that carries it round. Where
+   * the source states none, or one a later measurement overturns, it is the one the body's ETL spec
+   * carries: Nereid's K2 light curve, Eris's lock to Dysnomia. Absent only for Hyperion, which
+   * tumbles — the view leaves it still rather than spinning it at an invented rate.
    */
   rotationPeriodHours?: number;
   obliquityDeg?: number;
+  /**
+   * Where the body's pole points and which way its prime meridian faces at any date, from the IAU
+   * WGCCRE 2015 report (Archinal et al. 2018) as NAIF's `pck00011.tpc` carries it, but that a locked
+   * moon's W, and its pole's terms that turn within 5 per cent of a multiple of its node's rate, turn
+   * at its drawn orbit's rates and Iapetus's pole goes round with its orbit's, so they keep their
+   * faces to their planets, and their poles round their orbits', over the clock's AD 1 to 3000 (see
+   * `lockedToOrbit` in the ETL). The Moon's and Phobos's, whose W has a quadratic, are the IAU's
+   * whole, and so are the terms Ariel's, Umbriel's, Titania's and Oberon's poles go round on, which
+   * turn at none of their nodes' multiples. Where present it alone sets how the body is drawn, and
+   * the ETL checks the period and obliquity above against it. Absent where the report gives none: Hyperion tumbles, and Nereid,
+   * Eris, Haumea and Makemake have no model.
+   */
+  rotationalElements?: RotationalElements;
+}
+
+/**
+ * The IAU's rotational elements for one body: polynomials in time, plus periodic terms.
+ *
+ * The pole's right ascension and declination are in degrees in the ICRF, `[c0, c1, c2]` for
+ * `c0 + c1 T + c2 T²`, T in Julian centuries from J2000.0 TDB. The prime meridian W is the angle
+ * along the body's equator, anticlockwise seen from above that pole, from where the equator rises
+ * through the ICRF equator to the body's longitude 0, `c0 + c1 d + c2 d²` with d in days. A
+ * negative rate turns the body clockwise about the pole the IAU names: Venus, Uranus and its
+ * moons, Triton.
+ */
+export interface RotationalElements {
+  poleRaDeg: number[];
+  poleDecDeg: number[];
+  primeMeridianDeg: number[];
+  /**
+   * Each adds `ra sin θ` to the right ascension, `dec cos θ` to the declination and `pm sin θ` to
+   * W, θ being `angleDeg[0] + angleDeg[1] T + angleDeg[2] T²`. The smallest are left out; see
+   * `parsePckRotationalElements`.
+   */
+  terms?: Array<{ angleDeg: number[]; ra: number; dec: number; pm: number }>;
 }

src/app/shared/models/exoplanet.model.ts

@@ -17,6 +17,11 @@ export interface ExoplanetRecord {
   radiusEarth?: number;
   massEarth?: number;
   discoveryYear?: number;
+  /**
+   * True where the archive flags the planet as detected by imaging (`ima_flag`): photographed as a
+   * point of light beside its star, as HR 8799's four planets were. Absent for every other planet.
+   */
+  imaged?: true;
   /**
    * Measured orbital period in days (`pl_orbper`). Together with the semi-major axis this
    * pins the host star's gravitational parameter exactly, so the planet can be propagated at