The table matches Messier numbers with NGC. For example it shows that M1 (Crab Nebula) is also called NGC 1952. A Few Cool Features: The table is searchable, sortable, and horizontally scrollable for mobile. The “Description” column is also vertically scrollable. Mobile: Double tap the description contents. The field will scroll to show the whole description. Large Screens: Place cursor in the field and you’ll get a scroll bar.
| Messier | Name | NGC/IC | Type | Constellation | Description |
|---|---|---|---|---|---|
| M1 | Crab Nebula | NGC 1952 | Supernova Remnant | Taurus | The Crab Nebula is the expanding debris of a massive star that exploded as a supernova recorded by observers in 1054 CE. At its center lies a rapidly spinning neutron star, or pulsar, whose intense radiation powers the nebula’s glow. Space-based observatories have revealed a complex network of filaments rich in energized gas and magnetic fields. It is one of the most studied supernova remnants in the sky. |
| M2 | – | NGC 7089 | Globular Cluster | Aquarius | Messier 2 is a large, ancient globular cluster containing hundreds of thousands of stars bound tightly by gravity. Its stars formed early in the Milky Way’s history, more than 10 billion years ago. High-resolution observations show a dense central core surrounded by an extended halo. The cluster’s isolation above the Galactic plane hints at the early structure of our galaxy. |
| M3 | – | NGC 5272 | Globular Cluster | Canes Venatici | Messier 3 is one of the richest globular clusters known, hosting an unusually large population of variable stars. These stars are critical tools for measuring cosmic distances and stellar evolution. The cluster contains several hundred thousand stars packed into a compact sphere. Its brightness and structure have made it a benchmark object for globular cluster studies. |
| M4 | – | NGC 6121 | Globular Cluster | Scorpius | Messier 4 is one of the closest globular clusters to Earth, allowing individual stars to be resolved with great clarity. Observations have identified white dwarf stars that help constrain the age of the Milky Way. Compared to many globular clusters, it has a relatively loose and irregular structure. Its proximity makes it a prime target for detailed stellar studies. |
| M5 | – | NGC 5904 | Globular Cluster | Serpens | Messier 5 is a massive globular cluster containing some of the oldest known stars in the galaxy. It has a dense, luminous core and a wide halo extending far into space. Numerous variable stars within the cluster provide insight into stellar aging and dynamics. M5 likely formed during the earliest stages of the Milky Way’s assembly. |
| M6 | Butterfly Cluster | NGC 6405 | Open Cluster | Scorpius | The Butterfly Cluster is a bright open cluster composed of young, hot stars arranged in a loose, wing-like pattern. Its stars formed from the same molecular cloud and are only tens of millions of years old. The cluster lies against a rich background of Milky Way stars, enhancing its visual appeal. It is an excellent example of early stellar evolution in open clusters. |
| M7 | Ptolemy Cluster | NGC 6475 | Open Cluster | Scorpius | Messier 7 is one of the largest and brightest open clusters visible from Earth. It contains dozens of young stars spread across a wide region of sky. The cluster was known to ancient astronomers and recorded by Ptolemy in the 2nd century. Its proximity makes it easily resolved even with small telescopes. |
| M8 | Lagoon Nebula | NGC 6523 | Emission Nebula | Sagittarius | The Lagoon Nebula is a vast cloud of gas and dust where new stars are actively forming. Embedded young stars illuminate the surrounding nebula, carving dark lanes and glowing cavities. Observations from space reveal intense ultraviolet radiation shaping its structure. It is one of the most prominent star-forming regions in the Milky Way. |
| M9 | – | NGC 6333 | Globular Cluster | Ophiuchus | Messier 9 is a compact globular cluster located near the center of the Milky Way. Its stars are tightly packed, forming a dense spherical system. Heavy foreground dust dims the cluster, making it challenging to observe from Earth. Despite this, it provides valuable insight into the inner regions of the galaxy. |
| M10 | – | NGC 6254 | Globular Cluster | Ophiuchus | Messier 10 is a bright globular cluster with a strongly concentrated core. It contains hundreds of thousands of ancient stars gravitationally bound together. The cluster shows signs of dynamical evolution, with heavier stars migrating toward its center. M10 is an important target for studying stellar interactions in dense environments. |
| M11 | Wild Duck Cluster | NGC 6705 | Open Cluster | Scutum | The Wild Duck Cluster is one of the richest and most compact open clusters known. It contains thousands of stars packed into a relatively small region of space. Its high stellar density gives it an appearance more typical of globular clusters. M11 offers clues about the transition between open and globular cluster properties. |
| M12 | – | NGC 6218 | Globular Cluster | Ophiuchus | Messier 12 is a loosely concentrated globular cluster compared to others of its kind. Its stars are more widely dispersed, suggesting past gravitational interactions with the Milky Way. The cluster contains an ancient population of low-mass stars. Its structure provides insight into how tidal forces affect globular clusters over time. |
| M13 | Hercules Cluster | NGC 6205 | Globular Cluster | Hercules | Messier 13 is the brightest and most famous globular cluster in the northern sky. It contains several hundred thousand stars tightly bound by gravity. Observations have revealed a dense core and long stellar streams extending outward. M13 has long served as a showcase object for studies of stellar evolution. |
| M14 | – | NGC 6402 | Globular Cluster | Ophiuchus | Messier 14 is a distant globular cluster with a dense and compact structure. It contains an ancient stellar population formed early in the Milky Way’s history. Evidence suggests it may have experienced a past nova event. The cluster’s characteristics hint at possible origins outside the Milky Way. |
| M15 | – | NGC 7078 | Globular Cluster | Pegasus | Messier 15 is one of the most densely packed globular clusters known. Its core hosts a concentration of stars that may include a central black hole. The cluster contains numerous variable stars and exotic stellar systems. It is a key object for studying extreme gravitational environments. |
| M16 | Eagle Nebula | NGC 6611 | Open Cluster / Emission Nebula | Serpens | The Eagle Nebula is a star-forming region famous for towering columns of gas and dust sculpted by radiation from young stars. These structures are sites where new stars are actively forming. Observations have shown how intense stellar winds erode the surrounding material. M16 provides a dramatic view of stellar birth and destruction. |
| M17 | Omega / Swan Nebula | NGC 6618 | Emission Nebula | Sagittarius | Messier 17 is a massive star-forming nebula glowing from intense ultraviolet radiation emitted by young, hot stars. Its curved shape has earned it several popular names. Dense clouds within the nebula continue to collapse and form new stars. It is one of the brightest emission nebulae in the Milky Way. |
| M18 | – | NGC 6613 | Open Cluster | Sagittarius | Messier 18 is a small open cluster composed of relatively young stars. It lies near several prominent nebulae, suggesting a shared star-forming environment. The cluster’s stars are loosely bound and will gradually disperse over time. It provides insight into the early evolution of stellar groups. |
| M19 | – | NGC 6273 | Globular Cluster | Ophiuchus | Messier 19 is a globular cluster with a noticeably elongated shape. This distortion is likely caused by gravitational interactions with the Milky Way’s core. Its stars are ancient and densely packed near the center. The cluster’s unusual form makes it a valuable object for dynamical studies. |
| M20 | Trifid Nebula | NGC 6514 | Emission Nebula / Open Cluster | Sagittarius | The Trifid Nebula is a complex region combining emission, reflection, and dark nebulae. Its distinctive dark lanes divide the glowing gas into three prominent lobes. Young stars within the nebula illuminate and shape the surrounding material. M20 showcases multiple stages of star formation in one object. |
| M21 | – | NGC 6531 | Open Cluster | Sagittarius | Messier 21 is a young open cluster closely associated with nearby star-forming regions. Its hot, blue stars formed relatively recently from a shared molecular cloud. The cluster is still embedded in remnants of its natal material. It offers a snapshot of early stellar development. |
| M22 | – | NGC 6656 | Globular Cluster | Sagittarius | Messier 22 is one of the brightest globular clusters visible from Earth. It contains hundreds of thousands of ancient stars and a relatively large core. Observations have revealed multiple stellar populations within the cluster. This complexity provides clues about its formation history. |
| M23 | – | NGC 6494 | Open Cluster | Sagittarius | Messier 23 is a large open cluster containing many young, luminous stars. Its members are loosely bound and spread across a wide area of sky. The cluster formed from the same molecular cloud but will gradually disperse. It illustrates the transient nature of open clusters. |
| M24 | Sagittarius Star Cloud | – | Star Cloud | Sagittarius | Messier 24 is not a true cluster but a dense window into the Milky Way’s spiral arm. It allows a relatively unobscured view through interstellar dust. Thousands of stars at varying distances are visible along this line of sight. The object highlights the structure of our galaxy. |
| M25 | – | IC 4725 | Open Cluster | Sagittarius | Messier 25 is a loose grouping of young stars formed from a common origin. It contains several bright, evolved stars among its population. The cluster is moderately old for an open cluster and beginning to disperse. Its stars trace the life cycle of stellar associations. |
| M26 | – | NGC 6694 | Open Cluster | Scutum | Messier 26 is a small and relatively faint open cluster. Its stars are loosely arranged and partially obscured by interstellar dust. The cluster is several hundred million years old. It provides insight into how open clusters fade over time. |
| M27 | Dumbbell Nebula | NGC 6853 | Planetary Nebula | Vulpecula | The Dumbbell Nebula is a planetary nebula formed when a Sun-like star shed its outer layers. The exposed core now illuminates expanding shells of glowing gas. Observations show complex structures shaped by stellar winds and radiation. It represents the future fate of stars similar to our Sun. |
| M28 | – | NGC 6626 | Globular Cluster | Sagittarius | Messier 28 is a dense globular cluster located near the Galactic center. It contains numerous exotic objects, including millisecond pulsars. These systems offer insight into stellar evolution under extreme conditions. The cluster’s environment makes it a rich laboratory for high-energy astrophysics. |
| M29 | – | NGC 6913 | Open Cluster | Cygnus | Messier 29 is a small open cluster composed of young, massive stars. It lies within a complex region of interstellar dust that obscures many of its members. The cluster is part of a larger star-forming region in Cygnus. Its stars are short-lived and will evolve rapidly. |
| M30 | – | NGC 7099 | Globular Cluster | Capricornus | Messier 30 is a compact globular cluster with a highly concentrated core. It is undergoing core collapse, where stars crowd tightly at the center. The cluster contains an ancient stellar population. Its structure provides insight into long-term gravitational evolution. |
| M31 | Andromeda Galaxy | NGC 224 | Spiral Galaxy | Andromeda | The Andromeda Galaxy is the nearest large spiral galaxy to the Milky Way. It contains hundreds of billions of stars and numerous satellite galaxies. Observations show active star formation and a massive central bulge. Andromeda and the Milky Way are expected to merge in several billion years. |
| M32 | – | NGC 221 | Dwarf Elliptical Galaxy | Andromeda | Messier 32 is a compact dwarf elliptical galaxy orbiting Andromeda. Its stars are densely packed, giving it a smooth appearance. The galaxy may have been stripped of outer material by interactions with M31. It provides insight into galaxy evolution through tidal interactions. |
| M33 | Triangulum Galaxy | NGC 598 | Spiral Galaxy | Triangulum | The Triangulum Galaxy is a nearby spiral galaxy rich in gas and star-forming regions. It lacks a prominent central bulge compared to larger spirals. Observations reveal numerous stellar nurseries and supernova remnants. M33 helps astronomers study star formation in disk galaxies. |
| M34 | – | NGC 1039 | Open Cluster | Perseus | Messier 34 is a young open cluster with several hundred stars. Its members formed together but are gradually drifting apart. The cluster contains stars at various stages of early evolution. It serves as a useful reference for studying stellar aging. |
| M35 | – | NGC 2168 | Open Cluster | Gemini | Messier 35 is a large and rich open cluster easily resolved into individual stars. It lies near a distant background cluster, providing a striking contrast. Its stars are relatively young and loosely bound. M35 illustrates the early structure of stellar groups. |
| M36 | – | NGC 1960 | Open Cluster | Auriga | Messier 36 is a compact open cluster composed of young, hot stars. Its members formed from the same molecular cloud roughly 25 million years ago. The cluster is relatively small but well defined against the background of the Milky Way. It provides a clear example of early stellar evolution in open clusters. |
| M37 | – | NGC 2099 | Open Cluster | Auriga | Messier 37 is the richest and most densely populated of the Auriga open clusters. It contains hundreds of stars, including numerous red giants. The cluster is older than many open clusters, with an age of several hundred million years. Its diverse stellar population makes it valuable for evolutionary studies. |
| M38 | – | NGC 1912 | Open Cluster | Auriga | Messier 38 is an irregularly shaped open cluster with stars arranged in loose chains. It is moderately old for an open cluster, showing signs of gradual dispersal. The cluster’s stars vary in brightness and color. Its structure reflects the dynamic nature of stellar groupings. |
| M39 | – | NGC 7092 | Open Cluster | Cygnus | Messier 39 is a nearby open cluster composed of bright, widely spaced stars. Its loose arrangement indicates a relatively young age and weak gravitational binding. The cluster is easily resolved with small instruments. It offers insight into the early stages of cluster dissolution. |
| M40 | Winnecke 4 | – | Double Star | Ursa Major | Messier 40 consists of a pair of unrelated stars that appear close together from Earth. It is not a true binary system but an optical alignment. This object highlights the limitations of early observational techniques. M40 remains unique within the Messier catalog. |
| M41 | – | NGC 2287 | Open Cluster | Canis Major | Messier 41 is a bright open cluster containing several dozen stars. It includes a number of evolved red giant stars among younger members. The cluster is relatively nearby and easy to resolve. Its mixed population provides clues to stellar aging. |
| M42 | Orion Nebula | NGC 1976 | Emission Nebula | Orion | The Orion Nebula is the nearest massive star-forming region to Earth. It contains dense clouds of gas and dust illuminated by newly formed, hot stars. Observations reveal protoplanetary disks and active stellar nurseries. M42 offers an unparalleled view of star formation processes. |
| M43 | – | NGC 1982 | Emission Nebula | Orion | Messier 43 is a smaller emission nebula adjacent to the Orion Nebula. It is separated by a prominent lane of dust and illuminated by a single massive star. The nebula showcases how stellar radiation shapes surrounding gas. It is an integral part of the Orion star-forming complex. |
| M44 | Beehive Cluster / Praesepe | NGC 2632 | Open Cluster | Cancer | The Beehive Cluster is a large, nearby open cluster containing hundreds of stars. Its members share a common origin and motion through space. The cluster is several hundred million years old. It has been observed since antiquity and remains a benchmark for stellar studies. |
| M45 | Pleiades | NGC 1432 | Open Cluster | Taurus | The Pleiades is a young open cluster dominated by bright blue stars. Wisps of reflection nebulosity surround its members, illuminated by starlight. The cluster is only about 100 million years old. It is one of the most recognizable star groups in the sky. |
| M46 | – | NGC 2437 | Open Cluster | Puppis | Messier 46 is a rich open cluster containing several hundred stars. It lies along the plane of the Milky Way, creating a dense stellar background. A planetary nebula appears superimposed near its center but is not physically associated. The cluster illustrates the complexity of line-of-sight observations. |
| M47 | – | NGC 2422 | Open Cluster | Puppis | Messier 47 is a bright open cluster with relatively few but luminous stars. Its members are young and loosely bound. The cluster stands out clearly against the surrounding sky. It provides a contrast to richer but fainter open clusters nearby. |
| M48 | – | NGC 2548 | Open Cluster | Hydra | Messier 48 is a moderately old open cluster whose stars are beginning to drift apart. Its members span a range of brightness and evolutionary stages. The cluster is sparsely populated compared to younger clusters. It demonstrates the gradual dispersal of stellar groups. |
| M49 | – | NGC 4472 | Elliptical Galaxy | Virgo | Messier 49 is a giant elliptical galaxy and one of the brightest members of the Virgo Cluster. It contains an enormous population of old stars. Observations reveal a vast system of globular clusters surrounding it. M49 plays a key role in understanding galaxy clusters. |
| M50 | – | NGC 2323 | Open Cluster | Monoceros | Messier 50 is a compact open cluster with a roughly heart-shaped appearance. Its stars are relatively young and formed from the same cloud. The cluster stands out well against the Milky Way background. It offers insight into early cluster morphology. |
| M51 | Whirlpool Galaxy | NGC 5194 | Spiral Galaxy | Canes Venatici | The Whirlpool Galaxy is a classic grand-design spiral galaxy interacting with a smaller companion. Tidal forces have enhanced its prominent spiral arms. Observations reveal intense star formation along these arms. M51 is a key example of galaxy interaction. |
| M52 | – | NGC 7654 | Open Cluster | Cassiopeia | Messier 52 is a rich open cluster embedded in a dense region of the Milky Way. It contains young, luminous stars still associated with interstellar material. The cluster’s stars are loosely bound. It illustrates active star formation in spiral arms. |
| M53 | – | NGC 5024 | Globular Cluster | Coma Berenices | Messier 53 is a distant globular cluster with a compact structure. Its stars are ancient and tightly bound by gravity. The cluster lies far from the Galactic center. It provides insight into the outer halo of the Milky Way. |
| M54 | – | NGC 6715 | Globular Cluster | Sagittarius | Messier 54 is a massive globular cluster located at the core of the Sagittarius Dwarf Galaxy. It may represent the nucleus of that galaxy. The cluster contains multiple stellar populations. Its unique position links globular clusters and galaxy formation. |
| M55 | – | NGC 6809 | Globular Cluster | Sagittarius | Messier 55 is a large but loosely concentrated globular cluster. Its stars are ancient and widely distributed. The cluster shows relatively low central density. It provides a contrast to more compact globular clusters. |
| M56 | – | NGC 6779 | Globular Cluster | Lyra | Messier 56 is a moderately concentrated globular cluster. It contains an old population of low-metallicity stars. The cluster is located well above the Galactic plane. Its properties reflect early star formation conditions. |
| M57 | Ring Nebula | NGC 6720 | Planetary Nebula | Lyra | The Ring Nebula is a planetary nebula formed by a dying Sun-like star. Its glowing ring is produced by expanding shells of ionized gas. Observations reveal complex internal structures and faint outer halos. It represents a late stage of stellar evolution. |
| M58 | – | NGC 4579 | Spiral Galaxy | Virgo | Messier 58 is a barred spiral galaxy within the Virgo Cluster. It shows reduced star formation compared to isolated spirals. The galaxy’s structure is influenced by its dense environment. M58 helps illustrate environmental effects on galaxies. |
| M59 | – | NGC 4621 | Elliptical Galaxy | Virgo | Messier 59 is a smooth, elliptical galaxy dominated by older stars. It contains little gas or dust. The galaxy is part of the Virgo Cluster core. Its properties are typical of massive ellipticals. |
| M60 | – | NGC 4649 | Elliptical Galaxy | Virgo | Messier 60 is a giant elliptical galaxy rich in globular clusters. It hosts a supermassive black hole at its center. The galaxy is interacting gravitationally with nearby companions. M60 is central to studies of galaxy dynamics. |
| M61 | – | NGC 4303 | Spiral Galaxy | Virgo | Messier 61 is a spiral galaxy with active star formation. Its arms contain numerous star-forming regions and supernova remnants. The galaxy shows signs of past interactions. It is among the most active spirals in the Virgo Cluster. |
| M62 | – | NGC 6266 | Globular Cluster | Ophiuchus | Messier 62 is a dense globular cluster near the Galactic center. It has an unusually high number of variable stars. The cluster’s structure is distorted by tidal forces. It provides insight into extreme gravitational environments. |
| M63 | Sunflower Galaxy | NGC 5055 | Spiral Galaxy | Canes Venatici | The Sunflower Galaxy is a spiral galaxy with a bright central region and flocculent arms. Star formation occurs in patchy segments throughout its disk. The galaxy contains a massive dark matter halo. It is an important object for studying spiral structure. |
| M64 | Black Eye Galaxy | NGC 4826 | Spiral Galaxy | Coma Berenices | The Black Eye Galaxy is known for a prominent dark dust lane across its bright nucleus. It contains gas rotating in opposite directions within its disk. This unusual motion suggests a past merger or accretion event. M64 provides insight into galactic dynamics. |
| M65 | – | NGC 3623 | Spiral Galaxy | Leo | Messier 65 is a spiral galaxy that is part of the Leo Triplet. It shows moderate star formation and a well-defined disk. Gravitational interactions influence its structure. The galaxy offers clues to group dynamics. |
| M66 | – | NGC 3627 | Spiral Galaxy | Leo | Messier 66 is a disturbed spiral galaxy within the Leo Triplet. Its arms are asymmetrical due to gravitational interactions. The galaxy contains active star-forming regions. It illustrates the effects of close galactic encounters. |
| M67 | – | NGC 2682 | Open Cluster | Cancer | Messier 67 is one of the oldest known open clusters. Its stars are similar in age and composition to the Sun. The cluster provides a valuable benchmark for stellar evolution models. It represents a rare long-lived open cluster. |
| M68 | – | NGC 4590 | Globular Cluster | Hydra | Messier 68 is a metal-poor globular cluster with an extended shape. It contains ancient stars formed early in the galaxy’s history. The cluster lies in the outer halo of the Milky Way. Its properties reflect early chemical conditions. |
| M69 | – | NGC 6637 | Globular Cluster | Sagittarius | Messier 69 is a compact globular cluster near the Galactic center. Its stars are old and tightly bound. The cluster’s motion suggests a possible extragalactic origin. It contributes to understanding halo assembly. |
| M70 | – | NGC 6681 | Globular Cluster | Sagittarius | Messier 70 is a dense globular cluster with a strongly concentrated core. It contains an ancient population of stars. The cluster lies close to the center of the Milky Way. Its structure reflects long-term gravitational evolution. |
| M71 | – | NGC 6838 | Globular Cluster | Sagitta | Messier 71 is a loosely concentrated globular cluster with properties intermediate between open and globular clusters. Its stars are old but relatively metal-rich. The cluster’s structure suggests it has experienced significant tidal stripping. M71 helps bridge the gap between cluster classifications. |
| M72 | – | NGC 6981 | Globular Cluster | Aquarius | Messier 72 is a small and distant globular cluster located in the outer halo of the Milky Way. Its stars are ancient and tightly bound. The cluster has a compact core and low overall brightness. It provides insight into the galaxy’s most remote stellar populations. |
| M73 | – | NGC 6994 | Asterism | Aquarius | Messier 73 is a small grouping of stars that appear clustered from Earth but are not physically related. It is classified as an asterism rather than a true cluster. The stars lie at different distances and move independently. M73 highlights the importance of precise stellar measurements. |
| M74 | – | NGC 628 | Spiral Galaxy | Pisces | Messier 74 is a nearly face-on spiral galaxy with well-defined arms. It exhibits active star formation throughout its disk. The galaxy’s symmetry makes it a textbook example of spiral structure. M74 is frequently used to study star formation in spiral galaxies. |
| M75 | – | NGC 6864 | Globular Cluster | Sagittarius | Messier 75 is a compact globular cluster with a dense core. Its stars are ancient and metal-poor. The cluster contains multiple stellar populations. It offers clues to early globular cluster formation. |
| M76 | Little Dumbbell Nebula | NGC 650/651 | Planetary Nebula | Perseus | The Little Dumbbell Nebula is a planetary nebula formed by the expulsion of material from a dying star. Its bipolar structure is shaped by stellar winds and radiation. Observations reveal faint outer lobes extending beyond the main nebula. It represents a transitional phase in stellar evolution. |
| M77 | – | NGC 1068 | Spiral Galaxy | Cetus | Messier 77 is a bright spiral galaxy hosting an active galactic nucleus. Its core emits intense radiation powered by a supermassive black hole. Surrounding dust and gas obscure parts of the nucleus. M77 is a key object for studying active galaxies. |
| M78 | – | NGC 2068 | Reflection Nebula | Orion | Messier 78 is a reflection nebula illuminated by nearby young stars. Dust grains scatter blue light, giving the nebula its distinctive glow. The region contains forming stars embedded within molecular clouds. M78 provides insight into early stages of star formation. |
| M79 | – | NGC 1904 | Globular Cluster | Lepus | Messier 79 is a dense globular cluster located below the Galactic plane. Its stars are ancient and metal-poor. The cluster may have originated outside the Milky Way. It contributes to understanding galactic accretion. |
| M80 | – | NGC 6093 | Globular Cluster | Scorpius | Messier 80 is one of the densest globular clusters known. Its core hosts a high concentration of stars and stellar remnants. A historic nova was observed within the cluster. M80 offers a laboratory for studying stellar collisions. |
| M81 | Bode’s Galaxy | NGC 3031 | Spiral Galaxy | Ursa Major | Messier 81 is a grand-design spiral galaxy similar in structure to the Milky Way. It contains well-defined spiral arms and a bright central bulge. The galaxy interacts gravitationally with nearby companions. M81 is a cornerstone of nearby galaxy studies. |
| M82 | Cigar Galaxy | NGC 3034 | Starburst Galaxy | Ursa Major | Messier 82 is a starburst galaxy undergoing intense episodes of star formation. Powerful winds driven by stellar activity expel gas into intergalactic space. The galaxy’s distorted shape reflects past interactions. M82 illustrates extreme star formation processes. |
| M83 | Southern Pinwheel | NGC 5236 | Spiral Galaxy | Hydra | Messier 83 is a bright spiral galaxy with prominent arms and active star formation. It contains a high number of supernova remnants. The galaxy’s structure is influenced by a central bar. M83 is a key target for studying stellar life cycles. |
| M84 | – | NGC 4374 | Elliptical Galaxy | Virgo | Messier 84 is a giant elliptical galaxy at the heart of the Virgo Cluster. It hosts a supermassive black hole producing radio jets. The galaxy is dominated by old stars. M84 helps trace the cluster’s core dynamics. |
| M85 | – | NGC 4382 | Lenticular Galaxy | Coma Berenices | Messier 85 is a lenticular galaxy with features of both spirals and ellipticals. It shows evidence of past mergers. The galaxy contains little active star formation. It represents a transitional galaxy type. |
| M86 | – | NGC 4406 | Elliptical Galaxy | Virgo | Messier 86 is a massive elliptical galaxy moving rapidly through the Virgo Cluster. Its motion strips gas from the galaxy through ram pressure. The galaxy contains mostly old stars. It provides insight into cluster environmental effects. |
| M87 | Virgo A | NGC 4486 | Elliptical Galaxy | Virgo | Messier 87 is a giant elliptical galaxy with a powerful jet emitted from its central supermassive black hole. It contains one of the largest known systems of globular clusters. The galaxy dominates the Virgo Cluster. M87 is fundamental to black hole and galaxy studies. |
| M88 | – | NGC 4501 | Spiral Galaxy | Coma Berenices | Messier 88 is a spiral galaxy experiencing interaction with the Virgo Cluster environment. Its gas disk shows signs of stripping. Star formation continues in its spiral arms. M88 illustrates environmental influence on spirals. |
| M89 | – | NGC 4552 | Elliptical Galaxy | Virgo | Messier 89 is an elliptical galaxy with a smooth, symmetric appearance. It contains mostly old stars and little gas. The galaxy may have undergone past interactions. It is part of the Virgo Cluster core. |
| M90 | – | NGC 4569 | Spiral Galaxy | Virgo | Messier 90 is a spiral galaxy moving rapidly through the Virgo Cluster. Gas stripping has reduced its star formation activity. Its outer disk appears truncated. M90 demonstrates how clusters affect galaxy evolution. |
| M91 | – | NGC 4548 | Barred Spiral Galaxy | Coma Berenices | Messier 91 is a barred spiral galaxy with a prominent central bar. Its gas distribution has been influenced by its cluster environment. Star formation is modest. The galaxy illustrates bar-driven dynamics. |
| M92 | – | NGC 6341 | Globular Cluster | Hercules | Messier 92 is a bright and compact globular cluster containing extremely old stars. It is among the oldest objects in the Milky Way. The cluster has a dense core and extended halo. M92 provides insight into early galactic history. |
| M93 | – | NGC 2447 | Open Cluster | Puppis | Messier 93 is a rich open cluster with many bright, young stars. Its members formed together and are still loosely bound. The cluster has a pleasing, well-defined appearance. It exemplifies youthful stellar groupings. |
| M94 | – | NGC 4736 | Spiral Galaxy | Canes Venatici | Messier 94 is a spiral galaxy with a bright inner ring of star formation. Its outer disk is faint and extended. The galaxy’s structure suggests complex internal dynamics. M94 is useful for studying ringed galaxies. |
| M95 | – | NGC 3351 | Barred Spiral Galaxy | Leo | Messier 95 is a barred spiral galaxy with active star formation near its center. The bar channels gas inward, fueling new stars. The galaxy is part of the Leo I Group. It demonstrates bar-driven evolution. |
| M96 | – | NGC 3368 | Spiral Galaxy | Leo | Messier 96 is a spiral galaxy with asymmetrical arms. Its structure has been influenced by gravitational interactions. Star formation continues across its disk. The galaxy is a prominent member of the Leo I Group. |
| M97 | Owl Nebula | NGC 3587 | Planetary Nebula | Ursa Major | The Owl Nebula is a planetary nebula formed from a dying Sun-like star. Its appearance is shaped by expanding shells of gas. Dark regions within the nebula create its distinctive face-like features. It represents a late stage of stellar evolution. |
| M98 | – | NGC 4192 | Spiral Galaxy | Coma Berenices | Messier 98 is a spiral galaxy seen nearly edge-on. It shows signs of gas depletion due to cluster interactions. Star formation is uneven across its disk. M98 highlights environmental effects on galaxies. |
| M99 | – | NGC 4254 | Spiral Galaxy | Coma Berenices | Messier 99 is a spiral galaxy with a prominent, one-sided arm. This asymmetry is likely caused by gravitational interactions. The galaxy hosts active star formation. M99 is an example of disturbed spiral structure. |
| M100 | – | NGC 4321 | Spiral Galaxy | Coma Berenices | Messier 100 is a grand-design spiral galaxy in the Virgo Cluster. Its well-defined arms contain numerous star-forming regions. The galaxy has hosted multiple supernovae. M100 is a cornerstone for extragalactic distance studies. |
| M101 | Pinwheel Galaxy | NGC 5457 | Spiral Galaxy | Ursa Major | The Pinwheel Galaxy is a large, face-on spiral galaxy with extensive star-forming regions. Its arms are rich in gas and young stars. The galaxy’s disk extends far beyond its bright core. M101 is ideal for studying spiral structure. |
| M102 | – | NGC 5866 | Lenticular Galaxy | Draco | Messier 102 is a lenticular galaxy viewed nearly edge-on. It contains a prominent dust lane unusual for its type. The galaxy shows little active star formation. Its identity has been debated historically. |
| M103 | – | NGC 581 | Open Cluster | Cassiopeia | Messier 103 is a compact open cluster containing young stars. It lies within a rich Milky Way field. The cluster is relatively small but distinct. It represents early cluster development. |
| M104 | Sombrero Galaxy | NGC 4594 | Spiral Galaxy | Virgo | The Sombrero Galaxy is notable for its bright nucleus and dark dust lane. It contains a massive central black hole. The galaxy bridges characteristics of spiral and elliptical systems. M104 is one of the most striking galaxies known. |
| M105 | – | NGC 3379 | Elliptical Galaxy | Leo | Messier 105 is an elliptical galaxy dominated by old stars. It contains little gas or dust. The galaxy is a central member of the Leo I Group. It provides insight into elliptical galaxy structure. |
| M106 | – | NGC 4258 | Spiral Galaxy | Canes Venatici | Messier 106 is a spiral galaxy with an active nucleus powered by a supermassive black hole. Water masers in its disk allow extremely precise distance measurements. The galaxy exhibits anomalous spiral arms. M106 is crucial for cosmic distance calibration. |
| M107 | – | NGC 6171 | Globular Cluster | Ophiuchus | Messier 107 is a globular cluster with a loose and irregular structure. It lies close to the Galactic plane. The cluster’s stars are ancient. Its shape reflects tidal interactions. |
| M108 | – | NGC 3556 | Spiral Galaxy | Ursa Major | Messier 108 is an edge-on spiral galaxy with a mottled appearance. It shows active star formation and dust lanes. The galaxy’s structure is irregular. M108 offers insight into disk galaxy evolution. |
| M109 | – | NGC 3992 | Barred Spiral Galaxy | Ursa Major | Messier 109 is a barred spiral galaxy with well-defined arms. The bar influences gas flow toward the center. Star formation occurs throughout the disk. The galaxy is part of the Ursa Major Group. |
| M110 | – | NGC 205 | Dwarf Elliptical Galaxy | Andromeda | Messier 110 is a dwarf elliptical galaxy orbiting Andromeda. It contains both old stars and signs of recent star formation. Dust and gas are present despite its classification. M110 provides insight into satellite galaxy evolution. |
Credits: All content has been painstakingly reviewed on multiple authoritative sites such as ESA/Hubble, and major observatories. Descriptions are a brief composite of the key aspects of each object from those sites.