Nearly full Moon — rays across ancient seas
A few hours before full, the Moon loses its shadows — and shows its second map. At 99.9 percent illumination the Sun, seen from the center of the lunar disk, stands almost exactly behind us: the relief is as if switched off, craters and mountains lose their modeling. What remains is the albedo, the brightness of the ground itself. Whatever is bright now is bright material, not an illuminated slope.
That turns the nearly full Moon into a geological map. The dark plains — Oceanus Procellarum, Mare Imbrium, Serenitatis, Tranquillitatis and Crisium — are giant impact basins filled with basalt, flooded with lava in several episodes; their subtle differences in shade still reveal the individual flows today. Over them lie, like brushstrokes applied last, the bright ray systems of the youngest craters.
Two of them supply the timescale: Tycho, whose rays cover half the southern hemisphere, is by NASA dating about 110 million years old — on the Moon, almost the present day. Copernicus, at nearly a billion years, is markedly older and still radiates. On a world without weather, water and plate tectonics, fading simply takes eons.
The image was taken on October 29, 2012; the file stamp reads 13:15, and a few hours later the full phase was exactly reached. Together with the three-quarter Moon of October 7 it forms a pair: the same landscape, two illuminations — topography there, material here. Precisely this contrasting pair is the exhibit of the Moon article in the knowledge section.
All labels are computed, not placed by eye: the image was geometrically registered against the NASA reference for the same hour of exposure, and the names follow the official USGS/IAU nomenclature. Details are given under "Capture and processing".
Crops
Tycho & highlands
Tycho and the southern highlands — young rays over ancient crust
Tycho is no giant at about 85 kilometers — but with the Sun high it is the unmissable focal point of the south. Its rays run across everything: across the cratered walled plains of Deslandres, Maurolycus and Stöfler, across Pitatus at the edge of the mare, all the way to Clavius and Schiller.
Precisely this running-across is the information: whatever lies on top of everything else came last. The rays are the topmost page in the layered book of the highlands — at about 110 million years, almost the present day on a crust four billion years old.
Reiner Gamma & Kepler
Reiner Gamma — a swirl without relief
The bright, curving structure is not a crater: Reiner Gamma is a lunar swirl — a pure albedo pattern without relief of its own, tied to a local magnetic anomaly that apparently shields the solar wind there and lets the ground darken more slowly. Exactly how that works is still a matter of research today.
Beside it the ray crater Kepler and the dark basalt of Mare Insularum — three kinds of bright and dark in one field: swirl, ejecta and lava. Only the comparison makes it clear that “bright” on the Moon can tell quite different stories.
Aristarchus
Aristarchus — the brightest mark in the darkest sea
Aristarchus is among the brightest formations on the entire lunar near side, and in almost full light it becomes a pure beacon: no cast shadow, no relief — only freshly excavated material that has not yet had time to darken under the particle bombardment of the solar wind.
The contrast with the surrounding Oceanus Procellarum could hardly be greater: young, bright ejecta on old, dark basalt. The three-quarter Moon entry shows the same crater with Vallis Schroteri right beside it.
Humorum & Gassendi
Mare Humorum and Gassendi — a broken ring at the basin rim
On the northern rim of the dark Mare Humorum sits Gassendi like a ring set on top: central peaks, fractured floor, fine rilles. Its interior was lifted and broken up by rising magma — a classic “floor-fractured” crater, of the kind that cluster at basin rims.
The arcuate Rimae Hippalus trace the stress lines along which the crust gave way under the load of the basin lava. Letronne, Billy and Hansteen accompany the field to the west, where nearness to the limb draws all shapes increasingly out into length.
Crisium & Serenitatis
Crisium, Serenitatis, Tranquillitatis — three seas, three lava histories
Three seas in one view: the limb-near, ovally foreshortened Mare Crisium, the great Mare Serenitatis and Mare Tranquillitatis, where the first Moon landing touched down in 1969. Their basalt surfaces are tinted differently — every shade an eruptive episode of its own, still readable billions of years later.
Along the northern edge stand Cleomedes, Atlas and Hercules, farther south Taruntius and the sunken ghost crater Lamont, together with Rima and Rupes Cauchy as fine tectonic strokes in the basalt. In almost full light the relief is nearly gone — what remains is the material map.
Nectaris & Fecunditatis
Theophilus, Langrenus, Vendelinus — a staircase of ages in three craters
Between Mare Nectaris and Mare Fecunditatis stand three large craters that together form a staircase of ages: the sharp-edged, young Theophilus with its central peaks, the imposing Langrenus — and beside it the almost melted-away, far older Vendelinus, from which time has taken rampart and contour.
The small Mare Spumans sets a dark dab into the transition. With the Sun high, age is read not from shadows but from sharpness and brightness: the fresher the impact, the brighter and crisper the rims.
Copernicus & Insularum
Copernicus — the spoked wheel above Mare Insularum
Copernicus is here the hub of a spoked wheel: its rays reach far out across Mare Insularum and cross everything older — including Stadius, of which the lava has left only a low, gap-ridden ring, a true ghost crater.
Eratosthenes and the Montes Carpatus lead over to Mare Imbrium; to the west Kepler and Aristarchus set their own bright centers. Along the southern edge lies the old hill country around Fra Mauro — ejecta from the Imbrium impact, in which Apollo 14 landed.
Lunar north
Mare Frigoris, Plato and Sinus Iridum — the compressed north
The narrow Mare Frigoris, the “Sea of Cold”, draws a dark band across the north. South of it: the strikingly dark floor of Plato, the Montes Alpes with Vallis Alpes, and farther west the elegant arc of Sinus Iridum, framed by the Montes Jura and Promontorium Laplace.
Everything here belongs to the northern rim of the Imbrium basin — and everything appears compressed, because we are looking at a shallow angle across the lunar globe. The “Bay of Rainbows” is in truth an almost circular crater remnant, half swallowed by the Imbrium lava.
Schickard & Schiller
Schickard and Schiller — the limb makes ellipses
At the southwestern limb the perspective tips over: the 212-kilometer walled plain Schickard becomes a narrow ellipse, and in full light its floor shows a conspicuous pattern of lighter and darker zones — different surface layers that the flat relief alone would never reveal.
The strangely elongated Schiller is one of the Moon's more puzzling shapes; an extremely oblique impact or several merged craters are under discussion. The three-quarter Moon entry shows the same area in grazing light — there with the lava-filled Wargentin in between.
Imbrium in full light
Imbrium in high light — the same landscape, without shadows
The same region that the three-quarter Moon entry shows in grazing light — Plato, the Alpine Valley, Archimedes, the Apennines — here with the Sun nearly overhead. The relief is as if switched off: no shadows, hardly any modeling. What remains is the Moon's second layer of information, the albedo — the brightness difference of the ground itself: dark mare basalts, bright highlands, the dark floor of Plato.
The direct comparison with the three-quarter Moon entry is the best demonstration that a lunar photograph can show two completely different things — topography or material — and that the illumination decides which.
Moretus & southern limb
Moretus and the southern limb — where even the full Moon has shadows
Right at the southern limb even the nearly full Moon keeps its drama: here the sunlight strikes the surface at a shallow angle even at full phase, and the ramparts of the crowded highland craters still cast shadows. Moretus with its central peak stands in the middle of this crush.
Added to that is the extreme foreshortening: a round crater appears at the limb as a narrow ellipse. The limb zones are the reason the Moon can never quite be photographed “to completion” — libration tips this edge toward us a little differently from month to month.
Farther toward the limb the overlays mark Drygalski and the near-polar Cabeus. NASA's LCROSS mission struck there deliberately in 2009; the analyzed ejecta plume provided the detection of water in the permanently shadowed south polar region.
Acquisition and processing
The image comes from this gallery's early Newtonian period: a GSO 8″ f/4 Newtonian of 800 mm focal length, extended by a Tele Vue 2.5× Barlow, with an ALCCD full-HD planetary camera in front of it. The Moon was recorded as video sequences; lucky imaging was used to pick out and average the sharpest moments, and the individual fields were then assembled in Adobe Photoshop into this panorama of 2,091 × 2,160 pixels. The AVIF version was output in 2026 from Photoshop/Camera Raw as a 10-bit HDR image in Rec. 2020 PQ.
The overlay uses the NASA reference for October 29, 2012 at 12:00 UT, with matching phase, libration and axis orientation. 207 geometrically consistent image matches register it directly onto the panorama, with a median residual of 2.39 pixels; the official coordinates from the USGS/IAU Gazetteer of Planetary Nomenclature are then projected into the image. The procedure serves reliable naming — it is not a photogrammetric height measurement.