Believed to be the cosmic fire of creation by the Maya of Mesoamerica, M42 blazes brightly in the constellation Orion. Popularly called the Orion Nebula, this stellar nursery has been known to many different cultures throughout human history. The nebula is only 1,500 light-years away, making it the closest large star-forming region to Earth and giving it a relatively bright apparent magnitude of 4. Because of its brightness and prominent location just below Orion’s belt, M42 can be spotted with the naked eye, while offering an excellent peek at stellar birth for those with telescopes. It is best observed during January.

Messier 4 or M4 (also known as NGC 6121 or the Spider Globular Cluster) is a globular cluster in the constellation of Scorpius.

M4 is a rather loosely concentrated cluster of class IX and measures 75 light-years across. It features a characteristic "bar" structure across its core, visible to moderate sized telescopes. The structure consists of 11th-magnitude stars and is approximately 2.5' long and was first noted by William Herschel in 1783. At least 43 variable stars have been observed within M4.[9]

M4 is approximately 6,000 light-years away,[10] making it the closest globular cluster to the Solar System. It has an estimated age of 12.2 billion years.[7]

The Lagoon Nebula (catalogued as Messier 8 or M8, NGC 6523, Sharpless 25, RCW 146, and Gum 72) is a giant interstellar cloud in the constellation Sagittarius. It is classified as an emission nebula and has an H II region. The Lagoon Nebula is estimated to be between 4,000–6,000 light-years away from the Earth. In the sky of Earth, it spans 90' by 40', which translates to an actual dimension of 110 by 50 light years. Like many nebulae, it appears pink in time-exposure color photos but is gray to the eye peering through binoculars or a telescope, human vision having poor color sensitivity at low light levels.

Messier 13 or M13 (also designated NGC 6205 and sometimes called the Great Globular Cluster in Hercules, the Hercules Globular Cluster, or the Great Hercules Cluster), is a globular cluster of several hundred thousand stars in the constellation of Hercules.

The Eagle Nebula  (Messier 16) is part of a diffuse emission nebula which is catalogued as IC 4703. This region of active current star formation is about 5700 light-years distant. A spire of gas that can be seen coming off the nebula in the northeastern part is approximately 9.5 light-years or about 90 trillion kilometers long.[6]

The cluster associated with the nebula has approximately 8100 stars, which are mostly concentrated in a gap in the molecular cloud to the north-west of the Pillars.[7] The brightest star (HD 168076) has an apparent magnitude of +8.24, easily visible with good binoculars. It is actually a binary starformed of an O3.5V star plus an O7.5V companion.[8] This star has a mass of roughly 80 solar masses, and a luminosity up to 1 million times that of the Sun. The cluster's age has been estimated to be 1–2 million years.[9]

M17, also known as the Omega Nebula or Swan Nebula, is one of the largest star-forming regions in the Milky Way galaxy.  The Omega Nebula was discovered in 1745 by the Swiss astronomer Jean-Philippe Loys de Chéseaux. It is located 5,500 light-years from Earth in the constellation Sagittarius. The nebula has an apparent magnitude of 6 and can be seen with a pair of binoculars. M17, which appears near M16 and M18 in the sky, is best viewed on clear nights in August.  M17 contains one of our galaxy’s youngest star clusters, at only 1 million years old. However, many of the young stars in this cluster are impossible to see because of the gas and dust that surrounds them. The powerful radiation from the young stars evaporates and erodes the dense clouds of cold gas in which new stars form. One such pocket of gas is seen at the center of the brightest region of the nebula and is about 10 times larger than our solar system. 

The Trifid Nebula (catalogued as Messier 20 or M20 and as NGC 6514) is an H II region in the north-west of Sagittarius in a star-forming region in the Milky Way'sScutum–Centaurus Arm.[3] It was discovered by Charles Messier on June 5, 1764.[4] Its name means 'three-lobe'. The object is an unusual combination of an open cluster of stars, an emission nebula (the relatively dense, reddish-pink portion), a reflection nebula(the mainly NNE blue portion), and a dark nebula (the apparent 'gaps' in the former that cause the trifurcated appearance, also designated Barnard 85). Viewed through a small telescope, the Trifid Nebula is a bright and peculiar object, and is thus a perennial favorite of amateur astronomers.[5]

Messier 29 (M29), also known as NGC 6913 or the Cooling Tower Cluster, is a quite small, bright open cluster of stars just south of the central bright star Gamma Cygni of a northerly zone of the sky, in the constellation Cygnus. M29 is well within the several degrees of the arms of the Milky Way. It is at least many hundreds of lighjt years short of the Yardstick distance to the Galactic Center, as is between 4,000 and 7,200 light years away.. Data from Gala EDR3 gives a parallactic distance4 of about 5,240 light yerars.[2]

The Andromeda Galaxy is a barred spiral galaxy and is the nearest major galaxy to the Milky Way. It was originally named the Andromeda Nebula and is cataloged as Messier 31, M31, and NGC 224. Andromeda has a D25 isophotal diameter of about 46.56 kiloparsecs (152,000 light-years)[8] and is approximately 765 kpc (2.5 million light-years) from Earth. The galaxy's name stems from the area of Earth's sky in which it appears, the constellation of Andromeda, which itself is named after the princess who was the wife of Perseus in Greek mythology.[8] 

The Pleiades also known as Seven Sisters and Messier 45 (M45), is an asterism of an open star cluster containing young B-type stars in the northwest of the constellation Taurus. At a distance of about 444 light-years, it is among the nearest star clusters to Earth and the nearest Messier object to Earth, being the most obvious star cluster to the naked eye in the night sky.  Around 2330 BC it marked the vernal point. 

The cluster is dominated by hot blue luminous stars that have formed within the last 100 million years. Reflection nebulae around the brightest stars were once thought to be leftover material from their formation, but are now considered likely to be an unrelated dust cloud in the interstellar medium through which the stars are currently passing. This dust cloud is estimated to be moving at a speed of approximately 18 km/s relative to the stars in the cluster. 

(Note: Used a wider field of view Seestar S30.)

M57, more commonly known as The Ring Nebula, is about 2,000 light-years away in the constellation Lyra. Discovered by the French astronomer Antoine Darquier de Pellepoix in 1779, the Ring Nebula has an apparent magnitude of 8.8. It is easy to find, as it lies about halfway between the two 3rd-magnitude stars “Sheliak” and “Sulafat” which form the bottom of Lyra’s lyre. It is best observed using a telescope with an aperture of at least 20 cm (8 in), but even a 7.5 cm (3 in) telescope will reveal its elliptical ring shape.[14] Using a UHC or OIII filter greatly enhances visual observation, particularly in light polluted areas.

https://youtu.be/6FSIfUYFeTM

The M66 Group (also known as The Leo Triplet ) is a small group of galaxies about 35 million light-years away[5] in the constellation Leo. This galaxy group consists of the spiral galaxies M65, M66, and NGC 3628.  NGC 3628 (The Hamburger Galaxy) is seen edge-on, with dark dust lanes that obscure the bright core of the galaxy. M65 and M66 are on angles that show off their beautiful spiral structure.

M76 aka Little Dumbbell Nebula, the Cork Nebula or the Barbell Nebula. M76 was also given two New General Catalog numbers, NGC 650 and NGC 651, because it was formerly suspected to be a double nebula with two components touching each other. The name 'Little Dumbbell' comes from its shape that is a two-lobed structure of colorful, mottled, glowing gases resembling a balloon that’s been pinched around a middle waist. 

M76 is a planetary nebula, which is an expanding shell of gas around an aging or dying star, and it is one of only four planetary nebulae in Charles Messier’s catalog. M76 is in the constellation Perseus and is approximately 3,400 light-years away from Earth.

Discovered in 1780 by Messier’s colleague Pierre Méchain, M76 has an apparent magnitude of 12 and is best viewed in December. The nebula’s small size and faintness make it one of the more difficult Messier objects to observe. Telescopes 8 inches or larger are needed to reveal the double-lobed structure of the nebula.

M78 or NGC 2068, also known as Casper the Ghost Nebula, is a reflection nebula in the constellation Orion.

M78 is the brightest diffuse reflection nebula of a group of nebulae that includes NGC 2064, NGC 2067 and NGC 2071. This group belongs to the Orion B molecular cloud complex and is about 1,350 light-years distant from Earth.[2] M78 is easily found in small telescopes as a hazy patch and involves two stars of 10th and 11th magnitude. These two B-type stars, HD 38563 A and HD 38563 B, are responsible for making the cloud of dust in M78 visible by reflecting their light.[5]

Messier 81 (also known as NGC 3031 or Bode's Galaxy) is a grand design spiral galaxy about 12 million light-years away in the constellation Ursa Major. It has a D25 isophotal diameter of 29.44 kiloparsecs (96,000 light-years).[2][5] Because of its relative proximity to the Milky Way galaxy, large size, and active galactic nucleus (which harbors a 70 million M☉[6] supermassive black hole), Messier 81 has been studied extensively by professional astronomers

NGC 891 (also known as Caldwell 23, the Silver Sliver Galaxy, and the Outer Limits Galaxy) is an edge-on unbarred spiral galaxy about 30 million light-years away in the constellation Andromeda. It was discovered by William Herschel on October 6, 1784.[3]The galaxy is a member of the NGC 1023 group of galaxies in the Local Supercluster. It has an H II nucleus.[4]

 The object is visible in small to moderate size telescopes as a faint elongated smear of light with a dust lane visible in larger apertures.

NGC 925 is a barred spiral galaxy located about 30[4] million light-yearsaway in the constellation Triangulum. German-British astronomer William Herschel discovered this galaxy on 13 September 1784.[6]

The morphological classification of this galaxy is SB(s)d,[3] indicating that it has a bar structure and loosely wound spiral arms with no ring.[7] The spiral arm to the south is stronger than the northern arm, with the latter appearing flocculent and less coherent. The bar is offset from the center of the galaxy and is the site of star formation all along its length. Both of these morphological traits—a dominant spiral arm and the offset bar—are typically characteristics of a Magellanic spiral galaxy.[8] The galaxy is inclined at an angle of 55° to the line of sight along a position angle of 102°.[3]

The NGC 925 is a member of the NGC 1023 Group, a nearby, gravitationally-bound group of galaxies associated with NGC 1023.[5]However, the nearest member lies at least 650,000 ly (200,000 pc) distant from NGC 925. There is a 10 million solar mass (M☉) cloud of neutral hydrogen attached to NGC 925 by a streamer. It is uncertain whether this is a satellite dwarf galaxy, the remnant of a past tidal interaction, or a cloud of primordial gas.[9]

Although no supernovae have been observed in NGC 925 yet, a luminous red nova, designated AT 2023nzt (type LRN, mag. 19), was discovered on 26 July 2023.[10]

NGC 1579 (also known as the Northern Trifid) is a diffuse nebula located in the constellation of Perseus. It is referred to as the Northern Trifid because of its similar appearance to the Trifid Nebula, which is located in the southern celestial hemisphere of the sky. It is a H II region, a region of star formation.[4]

The star cluster contains the emission-line star LkHα 101, which provides much of the ionizing radiation in the nebula.[5]

NGC 1579 lies within a giant molecular cloud known as the California Molecular Cloud.[6]

NGC 1975, also known as the Running Man Nebula, is an emission nebula situated in the constellation Orion. It forms part of the larger complex known as the Orion Nebula. With its distinctive shape resembling a running figure, it showcases vibrant hues of glowing gas and dust, captivating observers with its celestial elegance.

The Flame Nebula, designated as NGC 2024, is an emission nebula in the constellation Orion. It is about 1350 light-years away.[1] At that distance, the Flame Nebula lies within the Orion B cloud of the larger Orion Molecular Cloud Complex.  The Flame Nebula is an emission nebula, glowing red and orange due to ionized hydrogen.

The bright star Alnitak (ζ Ori), the easternmost star in the Belt of Orion, appears very close to the Flame Nebula in the sky. But the star and nebula are not physically associated with one another. The Flame Nebula contains a young cluster of stars which includes at least one hot, luminous O-type star labeled IRS 2b.[2] The dense gas and dust in the foreground of the nebula heavily obscures the star cluster inside the nebula, making studies at infrared wavelengths most useful.

The Rosette Nebula, catalogued NGC 2237 is a flowery emission nebula composed of hot hydrogen gas, giving it its reddish color. Inside the nebula lies an open cluster of bright young stars designated NGC 2244. These stars formed about four million years ago from the nebular material and their stellar winds are clearing a hole in the nebula's center and causing the hydrogen gas to glow. The Rosette Nebula spans about 130 light-years across, lies about 5200 light-years away, and can be seen with a small telescope towards the constellation Monoceros aka the Unicorn.  

(Note: Used a wider field of view Seestar S30.)

NGC 2903 is an isolated barred spiral galaxy in the equatorial constellation of Leo, positioned about 1.5° due south of Lambda Leonis.[10] It was discovered by German-born astronomer William Herschel, who cataloged it on November 16, 1784. He mistook it as a double nebula, as did subsequent observers, and it wasn't until the nineteenth century that the Third Earl of Rosse resolved into a spiral form.[5] J. L. E. Dreyer assigned it the identifiers 2903 and 2905 in his New General Catalogue; NGC 2905 now designates a luminous knot in the northeastern spiral arm.[11]

This field galaxy[12] is located about 30[3] million light-years away from the Milky Way, and is a member of the Virgo Supercluster.[4] The morphological classification of this galaxy is SBbc,[6] indicating a barred spiral (SB) with moderate to tightly-wound spiral arms (bc). De Vaucouleurs and associates assigned it the class SAB(rs)bc, suggesting a weaker bar structure (SAB) with a partial ring (rs). The bar structure appears stronger in the near infrared band. The galaxy as a whole is inclined by an angle of 60° to the line of sight from the Earth.[7]

NGC 5033 is an inclined spiral galaxy located in the constellation Canes Venatici. Distance estimates vary from between 38 and 60 million light years from the Milky Way. The galaxy has a very bright nucleus and a relatively faint disk. Significant warping is visible in the southern half of the disk. The galaxy's relatively large angular size and relatively high surface brightness make it an object that can be viewed and imaged by amateur astronomers. The galaxy's location relatively near Earth and its active galactic nucleus make it a commonly studied object for professional astronomers.  NGC 5033 contains a Seyfert nucleus, a type of active galactic nucleus.[6] Like many other active galactic nuclei, this galaxy's nucleus is thought to contain a supermassive black hole. The bright emission seen in visible light (as well as other wavebands) is partially produced by the hot gas in the environment around this black hole. 

NGC 5907 (also known as Knife Edge Galaxy or Splinter Galaxy) is a spiral galaxy located approximately 50 million light years from Earth. William Herschel discovered the galaxy in 1788. NGC 5907 has an anomalously low metallicity and few detectable giant stars, being apparently composed almost entirely of dwarf stars. It is a member of the NGC 5866 Group. NGC 5907 has long been considered a prototypical example of a warped spiral in relative isolation. In 2006, an international team of astronomers announced the presence of an extended tidal stream surrounding the galaxy that challenges this picture and suggests the gravitational perturbations induced by the stream progenitor may be the cause for the warp. The existence of part of these tidal streams has been recently challenged by some deeper surveys.

NGC 6882 is an open cluster in the northern constellation of Vulpecula,[9] captured here with the orange-hued star 19 Vulpeculae (middle) and the white star 18 Vulpeculae (upper right).

19 Vulpeculae is located approximately 1,690[1] light years from Earth. It is a probable member of the open cluster NGC 6882.[4] (Seen in the lower half of the frame) This object is visible to the naked eye with an apparent visual magnitude of 5.40.[2] It is moving closer to the Earth with a heliocentric radial velocity of −19 km/s.[4] This is an aging giant star with a stellar classification of K2 IIIa,[3] having already consumed the hydrogen at its core and evolved away from the main sequence. It has nearly five[6] times the mass of the Sun but has expanded to around 100[1] times the Sun's radius. The star is radiating 2,889[1] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,200 K.[7]

18 Vulpeculae is a binary star[5] system located about 489 light years away from the Sun.[2] It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.51.[3] The system is moving closer to the Earth with a heliocentric radial velocity of −11.7 km/s.[4]  This is a double-lined spectroscopic binary system with an orbital period of 9.3 days.  The combined stellar classification of this system remains unclear, with classes of A3 III, A1 IV, A3 V, and A2 IV being given. The ultraviolet spectrum matches an A3 dwarf star. 

The Crescent Nebula (also known as NGC 6888, Caldwell 27, Sharpless 105) is an emission nebula in the constellation Cygnus, about 5000 light-years away from Earth. It was discovered by William Herschel in 1792.[2] It is formed by the fast stellar wind from the Wolf-Rayet star WR 136 (HD 192163) colliding with and energizing the slower moving wind ejected by the star when it became a red giant around 250,000[3] to 400,000 years ago. The result of the collision is a shell and two shock waves, one moving outward and one moving inward. The inward moving shock wave heats the stellar wind to X-ray-emitting temperatures.

NGC 6992 (also known as the East Veil Nebula) is a cloud of heated and ionized gas and dust in the constellation Cygnus. The source supernova was a star 20 times more massive than the Sun which exploded between 10,000 and 20,000 years ago.[2] At the time of the explosion, the supernova would have appeared brighter than Venus in the sky, and visible in the daytime.[6] The remnants have since expanded to cover an area of the sky roughly 3 degrees in diameter (about 6 times the diameter, and 36 times the area, of the full Moon!)

The North America Nebula (NGC 7000 or Caldwell 20) is an emission nebula in the constellation Cygnus, close to Deneb (the tail of the swan and its brightest star) in the night sky. The North America Nebula covers a region more than ten times the area of the full moon, but its surface brightness is low, so normally it cannot be seen with the unaided eye. Binoculars and telescopes with large fields of view (approximately 3°) will show it as a foggy patch of light under sufficiently dark skies. However, using a UHC filter, which filters out some unwanted wavelengths of light, it can be seen without magnification under dark skies. The North America nebula stretches 90 light years north to south.[2]

NGC 7023 (also known as the Iris Nebula and Caldwell 4) is a bright reflection nebulain the constellation Cepheus. The designation NGC 7023 refers to the open clusterwithin the larger reflection nebula designated LBN 487.

The nebula, which shines at magnitude +6.8, is illuminated by a magnitude +7.4 star designated HD 200775.[1] It is located near the Mira-type variable star T Cephei, and near the bright magnitude +3.23 variable star Beta Cephei (Alfirk). It lies 1,300 light-years away and is six light-years across.[2] 

IC 405 (also known as the Flaming Star Nebula, SH 2-229, or Caldwell 31) is an emission and reflection nebula[1] in the constellation Auriga north of the celestial equator, surrounding the bluish, irregular variable star AE Aurigae. It shines at magnitude +6.0. Its celestial coordinates are RA 05h 16.2m dec +34° 28′.[2] It is located near the emission nebula IC 410, the open clusters M38 and M36, and the K-class star Iota Aurigae.

The nebula measures approximately 37.0' x 19.0', and lies about 1,500 light-years away from Earth.[2] It is believed that the proper motion of the central star can be traced back to the Orion's Belt area.[2] The nebula is about 5 light-years across.[1]

IC 410 (The Tadpoles Nebula) a dusty emission nebula located in the constellation of Auriga at about 12.000 light years from Earth. The gas structures in this picture are lit by the radiation from the open star cluster NGC 1893 that lies in the center of the nebula. This star cluster is about 4 million years old, but in astronomical terms it is still very young, with hot, massive stars.  At the top-left of the star cluster two more dense structures are faintly visible and these structures point away from the center of the nebula. This is because of the stellar winds and radiation pressure from the stars in NGC 1893. Due to these structure's shape, the nebula is also called the Tadpoles Nebula.