Before the advent of telescopic photography, eight moons of Saturn were discovered by direct observation using optical telescopes. Saturn's largest moon, Titan, was discovered in 1655 by Christiaan Huygens using a 57-millimeter (2.2 in) objective lens^[13] on a refracting telescope of his own design.^[14] Tethys, Dione, Rhea and Iapetus (the "Sidera Lodoicea") were discovered between 1671 and 1684 by Giovanni Domenico Cassini.^[15] Mimas and Enceladus were discovered in 1789 by William Herschel.^[15] Hyperion was discovered in 1848 by W. C. Bond, G. P. Bond^[16] and William Lassell.^[17]

The use of long-exposure photographic plates made possible the discovery of additional moons. The first to be discovered in this manner, Phoebe, was found in 1899 by W. H. Pickering.^[18] In 1966 the tenth satellite of Saturn was discovered by Audouin Dollfus, when the rings were observed edge-on near an equinox.^[19] It was later named Janus. A few years later it was realized that all observations of 1966 could only be explained if another satellite had been present and that it had an orbit similar to that of Janus.^[19] This object is now known as Epimetheus, the eleventh moon of Saturn. It shares the same orbit with Janus—the only known example of co-orbitals in the Solar System.^[20] In 1980, three additional Saturnian moons were discovered from the ground and later confirmed by the Voyager probes. They are trojan moons of Dione (Helene) and Tethys (Telesto and Calypso).^[20]

The study of the outer planets has since been revolutionized by the use of uncrewed space probes. The arrival of the Voyager spacecraft at Saturn in 1980–1981 resulted in the discovery of three additional moons—Atlas, Prometheus and Pandora—bringing the total to 17.^[20] In addition, Epimetheus was confirmed as distinct from Janus. In 1990, Pan was discovered in archival Voyager images.^[20]

The Cassini mission,^[21] which arrived at Saturn in July 2004, initially discovered three small inner moons: Methone and Pallene between Mimas and Enceladus, and the second trojan moon of Dione, Polydeuces. It also observed three suspected but unconfirmed moons in the F Ring.^[22] In November 2004 Cassini scientists announced that the structure of Saturn's rings indicates the presence of several more moons orbiting within the rings, although only one, Daphnis, had been visually confirmed at the time.^[23] In 2007 Anthe was announced.^[24] In 2008 it was reported that Cassini observations of a depletion of energetic electrons in Saturn's magnetosphere near Rhea might be the signature of a tenuous ring system around Saturn's second largest moon.^[25] In March 2009, Aegaeon, a moonlet within the G Ring, was announced.^[26] In July of the same year, S/2009 S 1, the first moonlet within the B Ring, was observed.^[27] In April 2014, the possible beginning of a new moon, within the A Ring, was reported.^[28] (related image)

Study of Saturn's moons has also been aided by advances in telescope instrumentation, primarily the introduction of digital charge-coupled devices which replaced photographic plates. For the 20th century, Phoebe stood alone among Saturn's known moons with its highly irregular orbit. Then in 2000, a team of astronomers led by Brett J. Gladman discovered twelve irregular moons of Saturn using various ground-based telescopes around the world.^[29][30] The discovery of these irregular moons revealed orbital groupings within Saturn's irregular moon population, which provided the first insights into the collisional history of Saturn's irregular moons.^[30]

In 2003, a team of astronomers including Scott Sheppard, David Jewitt, and Jan Kleyna began using the Subaru 8.2 m telescope at Mauna Kea Observatory to search for irregular moons around Saturn, and discovered Narvi.^[30] Because of the Subaru telescope's very large aperture size alongside its camera's large field of view, it is capable of detecting extremely faint moons, hence Sheppard's team continued using the Subaru telescope for further moon searches.^[30] In 2005, Sheppard's team announced the discovery of twelve more small outer moons from their Subaru observations.^[31][32] Sheppard's team announced nine more irregular moons in 2006^[33] and three more moons in 2007, where Tarqeq (S/2007 S 1) was announced in April 2007 and S/2007 S 2 and S/2007 S 3 were announced one month after.^[34] No new irregular moons of Saturn were reported until 2019, when Sheppard's team identified twenty more irregular satellites of Saturn in archives of their 2004–2007 Subaru observations. This brought Saturn's moon count to 82, which resulted in Saturn overtaking Jupiter as the planet with the most known moons for the first time since 2000.^[12][2]

In 2019, researchers Edward Ashton, Brett Gladman, and Matthew Beaudoin conducted a survey of Saturn's Hill sphere using the 3.6-meter Canada–France–Hawaii Telescope (CFHT) and discovered about 80 new Saturnian irregular moons, which were reported to the Minor Planet Center (MPC) for announcement.^[4][35] Follow-up observations of these new moons took place over 2019–2021, eventually leading to S/2019 S 1 being announced in November 2021 and an additional 62 moons being announced from 3–16 May 2023.^[36][37] These discoveries brought Saturn's total number of confirmed moons up to 145, making it the first planet known to have over 100 moons.^[36][38] Yet another moon, S/2006 S 20, was announced on 23 May 2023, bringing Saturn's total count moons to 146.^[37]

All of these new moons are small and faint, with diameters over 3 km (2 mi) and apparent magnitudes of 25–27.^[4] These extremely dim moons could only be seen via the shift-and-add technique, where multiple long-exposure images are overlaid, shifted to follow the motion of Saturn in the sky, and then additively combined to bring out the signal of faint moons that follow Saturn in the sky.^[4] The researchers found that the Saturnian irregular moon population is more abundant at smaller sizes, suggesting that they are likely fragments from a collision that occurred a few hundred million years ago. The researchers extrapolated that the true population of Saturnian irregular moons larger than 2.8 km (1.7 mi) in diameter amounts to 150±30, which is approximately three times as many Jovian irregular moons down to the same size. If this size distribution applies to even smaller diameters, Saturn would therefore intrinsically have more irregular moons than Jupiter.^[4]

On 11 March 2025, 128 moons of Saturn were simultaneously announced by the MPC,^[1] bringing the total number of confirmed moons to 274 and making it the first planet known to have over 200 moons.^[39][40][41] These moons were found by Ashton, Gladman, Mike Alexandersen, and Jean-Marc Petit using the CFHT in 2023, as a continuation of their 2019–2021 survey for Saturnian irregular moons.^[40] Ashton's team also searched for moons in CFHT images taken by a separate team consisting of Wesley Fraser, Samantha Lawler, and John Kavelaars,^[1] who coincidentally imaged close to Saturn while searching for trans-Neptunian objects.^[39] Like the other faint Saturnian irregular moons previously discovered by Ashton's team, these 128 moons were discovered via the shift-and-add technique on the CFHT images.^[39][40] Many of these moons were traced back to earlier observations from 2004 to 2021, which corresponds to these moons' discovery dates.^[1]

Discovery of outer planet moons

The modern names for Saturnian moons were suggested by John Herschel in 1847.^[15] He proposed to name them after mythological figures associated with the Roman god of agriculture and harvest, Saturn (equated to the Greek Cronus).^[15] In particular, the then known seven satellites were named after Titans, Titanesses and Giants – brothers and sisters of Cronus.^[18] The idea was similar to Simon Marius' scheme for naming moons of Jupiter after children of Zeus.^[42]

As Saturn devoured his children, his family could not be assembled around him, so that the choice lay among his brothers and sisters, the Titans and Titanesses. The name Iapetus seemed indicated by the obscurity and remoteness of the exterior satellite, Titan by the superior size of the Huyghenian, while the three female appellations [Rhea, Dione, and Tethys] class together the three intermediate Cassinian satellites. The minute interior ones seemed appropriately characterized by a return to male appellations [Enceladus and Mimas] chosen from a younger and inferior (though still superhuman) brood. [Results of the Astronomical Observations made ... at the Cape of Good Hope, p. 415]

In 1848, Lassell proposed that the eighth satellite of Saturn be named Hyperion after another Titan.^[17][42] When in the 20th century the names of Titans were exhausted, the moons were named after different characters of the Greco-Roman mythology or giants from other mythologies.^[43] All the irregular moons (except Phoebe, discovered about a century before the others) are named after Inuit, and Gallic gods, and after Norse ice giants.^[44] The International Astronomical Union's (IAU) Committee for Planetary System Nomenclature, which oversees the naming of Solar System moons, rules that Saturnian moons that are smaller than 3 km in diameter (absolute magnitude H_V > 16.5)^[a] should only be named if it is of scientific interest.^[45]

Some asteroids share the same names as moons of Saturn: 55 Pandora, 106 Dione, 577 Rhea, 1809 Prometheus, 1810 Epimetheus, and 4450 Pan. In addition, three more asteroids would share the names of Saturnian moons but for spelling differences made permanent by the IAU: Calypso and asteroid 53 Kalypso; Helene and asteroid 101 Helena; and Gunnlod and asteroid 657 Gunlöd.

Saturn's satellite system is very lopsided: one moon, Titan, comprises more than 96% of the mass in orbit around the planet. The six other planemo (ellipsoidal) moons constitute roughly 4% of the mass, and the remaining small moons, together with the rings, comprise only 0.04%.^[b] Seven moons are large enough to have collapsed into a relaxed, ellipsoidal shape, though only one or two, Titan and possibly Rhea, are currently in hydrostatic equilibrium.

Although the boundaries may be somewhat vague, Saturn's moons can be divided into nine groups according to their orbital characteristics. Many of them, such as Pan and Daphnis, orbit within Saturn's ring system and have orbital periods only slightly longer than the planet's rotation period.^[49] The innermost moons and most regular satellites all have mean orbital inclinations ranging from less than a degree to about 1.5 degrees (except Iapetus, which has an inclination of 7.57 degrees) and small orbital eccentricities.^[2] On the other hand, irregular satellites in the outermost regions of Saturn's moon system, in particular the Norse group, have orbital radii of millions of kilometers and orbital periods lasting several years. The moons of the Norse group also orbit in the opposite direction to Saturn's rotation.^[44]

During late July 2009, a moonlet, S/2009 S 1, was discovered in the B Ring, 480 km from the outer edge of the ring, by the shadow it cast.^[27] It is estimated to be 300 m in diameter. Unlike the A Ring moonlets (see below), it does not induce a 'propeller' feature, probably due to the density of the B Ring.^[50]

In 2006, four tiny moonlets were found in Cassini images of the A Ring.^[51] Before this discovery only two larger moons had been known within gaps in the A Ring: Pan and Daphnis. These are large enough to clear continuous gaps in the ring.^[51] In contrast, a moonlet is only massive enough to clear two small—about 10 km across—partial gaps in the immediate vicinity of the moonlet itself creating a structure shaped like an airplane propeller.^[52] The moonlets themselves are tiny, ranging from about 40 to 500 meters in diameter, and are too small to be seen directly.^[3]

In 2007, the discovery of 150 more moonlets revealed that they (with the exception of two that have been seen outside the Encke gap) are confined to three narrow bands in the A Ring between 126,750 and 132,000 km from Saturn's center. Each band is about a thousand kilometers wide, which is less than 1% the width of Saturn's rings.^[3] This region is relatively free from the disturbances caused by resonances with larger satellites,^[3] although other areas of the A Ring without disturbances are apparently free of moonlets. The moonlets were probably formed from the breakup of a larger satellite.^[52] It is estimated that the A Ring contains 7,000–8,000 propellers larger than 0.8 km in size and millions larger than 0.25 km.^[3] In April 2014, NASA scientists reported the possible consolidation of a new moon within the A Ring, implying that Saturn's present moons may have formed in a similar process in the past when Saturn's ring system was much more massive.^[28]

Similar moonlets may reside in the F Ring.^[3] There, "jets" of material may be due to collisions, initiated by perturbations from the nearby small moon Prometheus, of these moonlets with the core of the F Ring. One of the largest F Ring moonlets may be the as-yet unconfirmed object S/2004 S 6. The F Ring also contains transient "fans" which are thought to result from even smaller moonlets, about 1 km in diameter, orbiting near the F Ring core.^[53]

One recently discovered moon, Aegaeon, resides within the bright arc of G Ring and is trapped in the 7:6 mean-motion resonance with Mimas.^[26] This means that it makes exactly seven revolutions around Saturn while Mimas makes exactly six. The moon is the largest among the population of bodies that are sources of dust in this ring.^[54]

Shepherd satellites are small moons that orbit within, or just beyond, a planet's ring system. They have the effect of sculpting the rings: giving them sharp edges, and creating gaps between them. Saturn's shepherd moons are Pan (Encke gap), Daphnis (Keeler gap), Prometheus (F Ring), Janus (A Ring), and Epimetheus (A Ring).^[22][26] Atlas and Pandora orbit on the outside edge of the A Ring and F Ring respectively, and were long thought to be shepherds as well, until more recent studies began to indicate otherwise. These moons probably formed as a result of accretion of the friable ring material on preexisting denser cores. The cores with sizes from one-third to one-half the present-day moons may be themselves collisional shards formed when a parental satellite of the rings disintegrated.^[49]

Janus and Epimetheus are co-orbital moons.^[20] They are of similar size, with Janus being somewhat larger than Epimetheus.^[49] They have orbits with less than a 100-kilometer difference in semi-major axis, close enough that they would collide if they attempted to pass each other. Instead of colliding, their gravitational interaction causes them to swap orbits every four years.^[55]

The innermost large moons of Saturn orbit within its tenuous E Ring, along with three smaller moons of the Alkyonides group.

• Mimas is the smallest and least massive of the inner round moons,^[47] although its mass is sufficient to alter the orbit of Methone.^[55] It is noticeably ovoid-shaped, having been made shorter at the poles and longer at the equator (by about 20 km) by the effects of Saturn's gravity.^[56] Mimas has a large impact crater one-third its diameter, Herschel, situated on its leading hemisphere^[57] Mimas has no known past or present geologic activity and its surface is dominated by impact craters, though it does have a water ocean 20–30 km beneath the surface.^[58] The only tectonic features known are a few arcuate and linear troughs, which probably formed when Mimas was shattered by the Herschel impact.^[57]
• Enceladus is one of the smallest of Saturn's moons that is spherical in shape—only Mimas is smaller^[56]—yet is the only small Saturnian moon that is currently endogenously active, and the smallest known body in the Solar System that is geologically active today.^[59] Its surface is morphologically diverse; it includes ancient heavily cratered terrain as well as younger smooth areas with few impact craters. Many plains on Enceladus are fractured and intersected by systems of lineaments.^[59] The area around its south pole was found by Cassini to be unusually warm and cut by a system of fractures about 130 km long called "tiger stripes", some of which emit jets of water vapor and dust.^[59] These jets form a large plume off its south pole, which replenishes Saturn's E ring^[59] and serves as the main source of ions in the magnetosphere of Saturn.^[60] The gas and dust are released with a rate of more than 100 kg/s. Enceladus may have liquid water underneath the south-polar surface.^[59] The source of the energy for this cryovolcanism is thought to be a 2:1 mean-motion resonance with Dione.^[59] The pure ice on the surface makes Enceladus one of the brightest known objects in the Solar System—its geometrical albedo is more than 140%.^[59]
• Tethys is the third largest of Saturn's inner moons.^[47] Its most prominent features are a large (400 km diameter) impact crater named Odysseus on its leading hemisphere and a vast canyon system named Ithaca Chasma extending at least 270° around Tethys.^[57] The Ithaca Chasma is concentric with Odysseus, and these two features may be related. Tethys appears to have no current geological activity. A heavily cratered hilly terrain occupies the majority of its surface, while a smaller and smoother plains region lies on the hemisphere opposite to that of Odysseus.^[57] The plains contain fewer craters and are apparently younger. A sharp boundary separates them from the cratered terrain. There is also a system of extensional troughs radiating away from Odysseus.^[57] The density of Tethys (0.985 g/cm³) is less than that of water, indicating that it is made mainly of water ice with only a small fraction of rock.^[46]
• Dione is the second-largest inner moon of Saturn. It has a higher density than the geologically dead Rhea, the largest inner moon, but lower than that of active Enceladus.^[56] While the majority of Dione's surface is heavily cratered old terrain, this moon is also covered with an extensive network of troughs and lineaments, indicating that in the past it had global tectonic activity.^[61] The troughs and lineaments are especially prominent on the trailing hemisphere, where several intersecting sets of fractures form what is called "wispy terrain".^[61] The cratered plains have a few large impact craters reaching 250 km in diameter.^[57] Smooth plains with low impact-crater counts are also present on a small fraction of its surface.^[62] They were probably tectonically resurfaced relatively later in the geological history of Dione. At two locations within smooth plains strange landforms (depressions) resembling oblong impact craters have been identified, both of which lie at the centers of radiating networks of cracks and troughs;^[62] these features may be cryovolcanic in origin. Dione may be geologically active even now, although on a scale much smaller than the cryovolcanism of Enceladus. This follows from Cassini magnetic measurements that show Dione is a net source of plasma in the magnetosphere of Saturn, much like Enceladus.^[62]

Three small moons orbit between Mimas and Enceladus: Methone, Anthe, and Pallene. Named after the Alkyonides of Greek mythology, they are some of the smallest moons in the Saturn system. Anthe and Methone have very faint ring arcs along their orbits, whereas Pallene has a faint complete ring.^[63] Of these three moons, only Methone has been photographed at close range, showing it to be egg-shaped with very few or no craters.^[64]

Trojan moons are a unique feature only known from the Saturnian system. A trojan body orbits at either the leading L₄ or trailing L₅ Lagrange point of a much larger object, such as a large moon or planet. Tethys has two trojan moons, Telesto (leading) and Calypso (trailing), and Dione also has two, Helene (leading) and Polydeuces (trailing).^[22] Helene is by far the largest trojan moon,^[56] while Polydeuces is the smallest and has the most chaotic orbit.^[55] These moons are coated with dusty material that has smoothed out their surfaces.^[65]

These moons all orbit beyond the E Ring. They are:

• Rhea is the second-largest of Saturn's moons. It is even slightly larger than Oberon, the second-largest moon of Uranus.^[56] In 2005, Cassini detected a depletion of electrons in the plasma wake of Rhea, which forms when the co-rotating plasma of Saturn's magnetosphere is absorbed by the moon.^[25] The depletion was hypothesized to be caused by the presence of dust-sized particles concentrated in a few faint equatorial rings.^[25] Such a ring system would make Rhea the only moon in the Solar System known to have rings.^[25] Subsequent targeted observations of the putative ring plane from several angles by Cassini's narrow-angle camera turned up no evidence of the expected ring material, leaving the origin of the plasma observations unresolved.^[66]

Otherwise Rhea has rather a typical heavily cratered surface,^[57] with the exceptions of a few large Dione-type fractures (wispy terrain) on the trailing hemisphere^[67] and a very faint "line" of material at the equator that may have been deposited by material deorbiting from present or former rings.^[68] Rhea also has two very large impact basins on its anti-Saturnian hemisphere, which are about 400 and 500 km across.^[67] The first, Tirawa, is roughly comparable to the Odysseus basin on Tethys.^[57] There is also a 48 km-diameter impact crater called Inktomi^[69] at 112°W that is prominent because of an extended system of bright rays,^[70] which may be one of the youngest craters on the inner moons of Saturn.^[67] No evidence of any endogenic activity has been discovered on the surface of Rhea.^[67]

• Titan, at 5,149 km diameter, is the second largest moon in the Solar System and Saturn's largest.^[71][47] Out of all the large moons, Titan is the only one with a dense (surface pressure of 1.5 atm), cold atmosphere, primarily made of nitrogen with a small fraction of methane.^[72] The dense atmosphere frequently produces bright white convective clouds, especially over the south pole region.^[72] On 6 June 2013, scientists at the IAA-CSIC reported the detection of polycyclic aromatic hydrocarbons in the upper atmosphere of Titan.^[73] On 23 June 2014, NASA claimed to have strong evidence that nitrogen in the atmosphere of Titan came from materials in the Oort cloud, associated with comets, and not from the materials that formed Saturn in earlier times.^[74]

The surface of Titan, which is difficult to observe due to persistent atmospheric haze, shows only a few impact craters and is probably very young.^[72] It contains a pattern of light and dark regions, flow channels and possibly cryovolcanos.^[72][75] Some dark regions are covered by longitudinal dune fields shaped by tidal winds, where sand is made of frozen water or hydrocarbons.^[76] Titan is the only body in the Solar System beside Earth with bodies of liquid on its surface, in the form of methane–ethane lakes in Titan's north and south polar regions.^[77] The largest lake, Kraken Mare, is larger than the Caspian Sea.^[78] Like Europa and Ganymede, it is believed that Titan has a subsurface ocean made of water mixed with ammonia, which can erupt to the surface of the moon and lead to cryovolcanism.^[75] On 2 July 2014, NASA reported the ocean inside Titan may be "as salty as the Earth's Dead Sea".^[79][80]

• Hyperion is Titan's nearest neighbor in the Saturn system. The two moons are locked in a 4:3 mean-motion resonance with each other, meaning that while Titan makes four revolutions around Saturn, Hyperion makes exactly three.^[47] With an average diameter of about 270 km, Hyperion is smaller and lighter than Mimas.^[81] It has an extremely irregular shape, and a very odd, tan-colored icy surface resembling a sponge, though its interior may be partially porous as well.^[81] The average density of about 0.55 g/cm^3[81] indicates that the porosity exceeds 40% even assuming it has a purely icy composition. The surface of Hyperion is covered with numerous impact craters—those with diameters 2–10 km are especially abundant.^[81] It is the only moon besides the small moons of Pluto known to have a chaotic rotation, which means Hyperion has no well-defined poles or equator. While on short timescales the satellite approximately rotates around its long axis at a rate of 72–75° per day, on longer timescales its axis of rotation (spin vector) wanders chaotically across the sky.^[81] This makes the rotational behavior of Hyperion essentially unpredictable.^[82]
• Iapetus is the third-largest of Saturn's moons.^[56] Orbiting the planet at 3.5 million km, it is by far the most distant of Saturn's large moons, and also has the largest orbital inclination, at 15.47°.^[48] Iapetus has long been known for its unusual two-toned surface; its leading hemisphere is pitch-black and its trailing hemisphere is almost as bright as fresh snow.^[83] Cassini images showed that the dark material is confined to a large near-equatorial area on the leading hemisphere called Cassini Regio, which extends approximately from 40°N to 40°S.^[83] The pole regions of Iapetus are as bright as its trailing hemisphere. Cassini also discovered a 20 km tall equatorial ridge, which spans nearly the moon's entire equator.^[83] Otherwise both dark and bright surfaces of Iapetus are old and heavily cratered. The images revealed at least four large impact basins with diameters from 380 to 550 km and numerous smaller impact craters.^[83] No evidence of any endogenic activity has been discovered.^[83]

A clue to the origin of the dark material covering part of Iapetus's starkly dichromatic surface may have been found in 2009, when NASA's Spitzer Space Telescope discovered a vast, nearly invisible disk around Saturn, just inside the orbit of the moon Phoebe – the Phoebe ring.^[84] Scientists believe that the disk originates from dust and ice particles kicked up by impacts on Phoebe. Because the disk particles, like Phoebe itself, orbit in the opposite direction to Iapetus, Iapetus collides with them as they drift in the direction of Saturn, darkening its leading hemisphere slightly.^[84] Once a difference in albedo, and hence in average temperature, was established between different regions of Iapetus, a thermal runaway process of water ice sublimation from warmer regions and deposition of water vapor onto colder regions ensued. Iapetus's present two-toned appearance results from the contrast between the bright, primarily ice-coated areas and regions of dark lag, the residue left behind after the loss of surface ice.^[85][86]

Irregular moons are small satellites with distant, inclined, and frequently retrograde orbits, believed to have been acquired by the parent planet through a capture process. They often occur as collisional families or groups.^[30] The precise size and albedo of many of the irregular moons are not known because they are too small to be resolved by telescopes on Earth and in space, so their sizes are estimated from their brightness by assuming a dark surface or low albedo of around 6% (albedo of Phoebe) or less.^[29] The irregular moons generally have featureless visible and near infrared spectra dominated by water absorption bands.^[30] They are typically gray (spectrally neutral) or moderately red in color—similar to C-type, P-type, or D-type asteroids,^[44] though they are much less red than Kuiper belt objects.^[30][c]

The Inuit group includes 36 prograde outer moons that are similar enough in their distances from the planet (190–300 radii of Saturn), their orbital inclinations (45–50°) and their colors that they can be considered a group.^[29][44] The Inuit group is further split into three distinct subgroups at different semi-major axes, and are named after their respective largest members. Ordered by increasing semi-major axis, these subgroups are the Kiviuq subgroup (188 Saturn radii), Paaliaq (249 Saturn radii), and the Siarnaq subgroup (297 Saturn radii).^[87][88][89] It is unknown whether all of these subgroups of the Inuit group share a common origin.^[88]

The Kiviuq group includes 20 members, with the only named members being Ijiraq and the group's largest member and namesake Kiviuq. Kiviuq has a diameter of about 17 km and has a highly elongated shape, which may indicate it is a contact binary.^[90] The Siarnaq group includes 15 members, with the only named members being Tarqeq and the group's namesake Siarnaq.^[89] Siarnaq is the largest member of its subgroup and the entire Inuit group, with an estimated diameter of about 39 km.^[91] The moons of the Kiviuq and Siarnaq subgroups are tightly clustered in semi-major axis and inclination with respect to their namesake moon, which makes them distinct collisional families.^[88][39] In contrast to Kiviuq and Siarnaq, Paaliaq (diameter ~25 km) does not have an associated subgroup.^[88][87]

The Gallic group includes 17 prograde outer moons that are similar in their orbital inclination (35–40°), their orbital eccentricity, and their color that they can be considered a group.^[29][44] The named members of the Gallic group are Albiorix, Bebhionn, Erriapus, and Tarvos.^[89] The largest of these moons is Albiorix with an estimated diameter of about 29 km.^[91] The Gallic group may be divided into the Albiorix subgroup, which consists of 16 moons with semi-major axes between 200–330 radii of Saturn, and the outlier moon S/2004 S 24 which has a lower eccentricity and a much more distant semi-major axis of ~400 Saturn radii.^[89][88] S/2004 S 24 may not be directly related to the Gallic group, although it is possible that it could have formed as a fragment of an Albiorix subgroup member that was collisionally disrupted when it was at its farthest distance from Saturn in its elliptical orbit.^[88]

All 197 retrograde outer moons of Saturn are broadly classified into the Norse group.^[29][44] Only 31 moons of the Norse group have been named: Aegir, Angrboda, Alvaldi, Beli, Bergelmir, Bestla, Eggther, Farbauti, Fenrir, Fornjot, Geirrod, Gerd, Greip, Gridr, Gunnlod, Hati, Hyrrokkin, Jarnsaxa, Kari, Loge, Mundilfari, Narvi, Phoebe, Skathi, Skoll, Skrymir, Surtur, Suttungr, Thiazzi, Thrymr, and Ymir.^[89]

Although the Norse group does not show obvious clustering in orbital elements, researchers led by Edward Ashton have proposed splitting the Norse group into four different subgroups by inclination.^[88] These subgroups still have a broad range of orbital semi-major axes, inclinations, and eccentricities, and may not necessarily have an impact origin.^[88]

• The Phoebe subgroup consists of moons between inclinations 172.5° and 180° and is named after Phoebe,^[88] by far the largest irregular moon of Saturn with a diameter of 213±1.4 km.^[30] It has a retrograde orbit and rotates on its axis every 9.3 hours.^[92] Phoebe was the first moon of Saturn to be studied in detail by Cassini, in June 2004; during this encounter Cassini was able to map nearly 90% of the moon's surface. Phoebe has a nearly spherical shape and a relatively high density of about 1.6 g/cm³.^[30] Cassini images revealed a dark surface scarred by numerous impacts—there are about 130 craters with diameters exceeding 10 km. Such impacts may have ejected fragments of Phoebe into orbit around Saturn—two of these may be S/2006 S 20 and S/2006 S 9, whose orbits are similar to Phoebe.^[87][93][94] Spectroscopic measurement showed that the surface is made of water ice, carbon dioxide, phyllosilicates, organics and possibly iron-bearing minerals.^[30] Phoebe is believed to be a captured centaur that originated in the Kuiper belt.^[30] It also serves as a source of material for the largest known ring of Saturn, which darkens the leading hemisphere of Iapetus (see above).^[84]

• The Mundilfari subgroup consists of moons between inclinations 157° and 172.5° and is the most populated of the four Norse subgroups proposed by Ashton and collaborators.^[88] Named after its largest member Mundilfari (diameter ~7 km), this subgroup is dominated by tiny moons smaller than 4 km in diameter, which suggests they were formed by a relatively recent collisional event that destroyed a progenitor moon at least 100 million years ago.^[88][39] Ashton and collaborators proposed that this progenitor moon of the Mundifari subgroup would have orbited Saturn at a semi-major axis of ~19.5 million km (~320 Saturn radii), inclination ~165°, and eccentricity ~0.28.^[88] The collision that destroyed this progenitor moon would have to eject its fragments at a speed of at least 200 m/s, and subsequent collisions of its fragments may further disperse their orbits to produce the broad orbital distribution of the Mundilfari group observed today.^[88]

• The Kari subgroup consists of moons between inclinations 151° and 157° and appears mostly concentrated around the orbit of its namesake and largest member Kari (diameter ~6 km) with a semi-major axis range between 0.14–0.16 au (21–24 million km) from Saturn.^[88] This tight clustering may be a collisional family.^[88] There are several other moons in the Kari subgroup's inclination range that have semi-major axes less than the aforementioned range, and thus may not be related to the proposed collisional family.^[88][39]

• The remaining Norse group moons with inclinations below 151° are sparse in number and are assigned to the low-inclination subgroup by Ashton and collaborators.^[88] Of the moons of the low-inclination subgroup, Narvi and S/2019 S 11 have the most similar orbits to each other, which suggests these two moons share an origin.^[88]

The Saturnian moons are listed here by orbital period (or semi-major axis), from shortest to longest. Moons massive enough for their surfaces to have collapsed into a spheroid are highlighted in bold and marked with a blue background, while the irregular moons are listed in red, orange, green, and gray background. The orbits and mean distances of the irregular moons are strongly variable over short timescales due to frequent planetary and solar perturbations, so the orbital elements of irregular moons listed here are averaged over a 5,000-year numerical integration by the Jet Propulsion Laboratory. These may sometimes strongly differ from the osculating orbital elements provided by other sources.^[89][95] Otherwise, recently-discovered irregular moons without published proper elements are temporarily listed here with inaccurate osculating orbital elements that are italicized to distinguish them from other irregular moons with proper orbital elements. The mean orbital elements are based on a reference epoch of 1 January 2000,^[89] whereas the osculating orbital elements of the 128 newly-discovered moons are based on a reference epoch of 5 May 2025.^[1]