About me
Amateur astrophotographer born in '76, always fascinated by the cosmos and its mysteries. In 2018, I set up my first astronomical gear, finally bringing my eyes to places where only my imagination had ventured before. Today, astrophotography has become a way of life, a gathering place, a hub of friends, and a way of being. Over the years, I have studied photographic techniques, processing, and post-production of digital astronomical images.Hard work has given me the chance to see my name reach places I never could have imagined. In 2021, one of my shoots was selected by NASA as the Astronomy Picture of the Day, bringing me a touch of recognition. This honor, along with all subsequent acknowledgments, has boosted my self-confidence and motivated me to keep improving.
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Tutorial
Polar alignment with Synscan Skywatcher
Thank you for exploring the cosmos through my eyes. Never stop looking beyond… the next dream is already among the stars.
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© Valerio Avitabile
Galaxy
Galaxies are enormous collections of stars, gas, dust, and dark matter, all held together by the force of gravity. Each galaxy can contain millions, billions, or even trillions of stars, along with planetary systems, nebulae, and black holes. Galaxies are the primary components of the observable universe and come in a variety of shapes, sizes, and compositions. Our Milky Way is a spiral galaxy, but more specifically, it is a barred spiral galaxy. This means that, in addition to the classic spiral arms, it features a central bar of stars extending through its core. This bar is a distinctive characteristic of barred spiral galaxies, setting them apart from "normal" spiral galaxies, where the center is primarily a compact nucleus without a bar structure.
The central bar of the Milky Way is composed of older stars and acts as a sort of "conduit," channeling gas and material toward the center of the galaxy. There, processes of star formation and activity involving the supermassive black hole take place.
M33 Galaxy
The Triangulum Galaxy, also known as Messier 33 or M33, is a spiral galaxy located in the constellation Triangulum.
At an approximate distance of 2.73 million light-years from Earth and with a diameter of 18.74 kiloparsecs (about 61,100 light-years), the Triangulum Galaxy is the third-largest member of the Local Group of galaxies, following the Andromeda Galaxy and the Milky Way. It is composed of countless clusters of young blue stars that illuminate its swirling arms and vast regions of ionized hydrogen and oxygen, which serve as stellar nurseries. Among these is the NGC 604 nebula, the largest and brightest star-forming region in the galaxy—an immense nursery where new young stars are born.
Under exceptionally good observation conditions, free from light pollution, the Triangulum Galaxy can be seen by some people with fully dark-adapted naked eyes. To such observers, it is the farthest permanent object visible without magnification, being about one and a half times farther away than Messier 31, the Andromeda Galaxy.
M31 Andromeda
The Andromeda Galaxy, located in the constellation of the same name, lies about 2.5 million light-years away from us. Under a perfectly clear and dark sky, it can be faintly visible to the naked eye. It is the largest member of the Local Group of galaxies, containing a trillion stars within a disk spanning 220,000 light-years, far surpassing the number of stars in our Milky Way. It is also the closest spiral galaxy to ours.
The Andromeda Galaxy is approaching the Milky Way at a speed of approximately 400,000 kilometers per hour. In about 5 billion years, the two galaxies will pass through each other, and these gravitational interactions will drastically alter the appearance of both.
Astronomer Edwin Hubble was the first to identify Cepheid variable stars in photographs of Andromeda, which allowed him to measure the galaxy's distance. His measurements proved that Andromeda was not a cluster of stars and gas within the Milky Way but a completely separate galaxy located at a significant distance from ours. For this reason, it was historically also referred to as the Great Nebula of Andromeda.
Leo Triplet
The Leo Triplet is a fascinating example of a group of galaxies interacting gravitationally. Here are some insights into each of the galaxies that make up this triplet:
NGC 3628 (Hamburger Galaxy)
NGC 3628 is an unbarred spiral galaxy located approximately 35 million light-years from Earth. It is known for its spectacular edge-on view, showcasing a thin disk of stars, gas, and interstellar dust. The galaxy's inclination relative to our line of sight emphasizes its “hamburger” shape. Recent studies have revealed a vast cloud of gas and dust surrounding the galaxy, indicating ongoing star formation activity and the presence of stellar nurseries within NGC 3628.
M66 (NGC 3627)
M66 is a barred spiral galaxy about 36 million light-years away. It is one of the brightest galaxies in the group, with a well-defined structure of spiral arms wrapping around a central bar of stars. M66 also hosts a significant number of star-forming regions, highlighted by the presence of young star clusters and bright nebulae in its spiral arms. The galaxy shows clear signs of distortion caused by gravitational interaction with the other galaxies in the triplet.
M65 (NGC 3623)
M65 is another spiral galaxy located roughly 35 million light-years from Earth. It has a structure similar to M66, with well-defined spiral arms surrounding a bright central nucleus. M65, like its counterparts, exhibits characteristics influenced by gravitational interactions within the Leo Triplet.
M51 Whirpool Galaxy
The Whirlpool Galaxy (M51) is a spiral galaxy located about 31 million light-years from Earth in the constellation Canes Venatici. It is famous for its well-defined spiral structure and its gravitational interaction with the smaller galaxy NGC 5195, which gives it a distinctive appearance.
M51's spiral arms host many star-forming regions, and it contains a supermassive black hole at its center. This galaxy is an excellent example of an interacting galaxy and is a key object of study for understanding galactic dynamics and star formation. It is easily observable with telescopes, making it a popular target for both amateur and professional astronomers.It is on average over 35 million light years from Earth.
Leo Triplet
The Draco Triplet is a group of three galaxies located in the constellation Draco. The triplet consists of NGC 5981, NGC 5982, and NGC 5985, all of which are interacting gravitationally.
NGC 5981 is an elliptical galaxy that is relatively bright and shows signs of past star formation.
NGC 5982 is a lenticular galaxy with a well-defined central bulge, often considered an intermediate type between elliptical and spiral galaxies.
NGC 5985 is a spiral galaxy, characterized by prominent arms, and is the most active of the three, showing strong star formation.
These galaxies are approximately 70 million light-years away from Earth and provide a unique example of galactic interactions and evolution within a small group.
NGC 4565 Needle Galaxy
52 million light years that's the distance the photons traveled before reaching the sensor of my astronomical camera. This is the most distant deep-space object I have ever photographed: NGC 4565, the Needle Galaxy, a stunning spiral galaxy observed in the direction of the constellation Coma Berenices.It's shape and structure are strikingly similar to the Milky Way, and its edge-on orientation allows us to marvel at the dark dust lane that defines its appearance.
M81 - M82 Bode & Cigar Galaxy
M81 and M82 respectively Bode and Cigar are 2 galaxies located in the Big Dipper distant on average from our solar system about 11.7 million light years, a measure that makes it one of the closest groups of galaxies to our Local Group. M81 and M82 are now separated by about 300,000 light years, but 250 million years ago there was a meeting between the two galaxies, and a large amount of gas poured into M82, particularly its central regions. This interaction resulted in a sharp increase in star formation in both galaxies. Still the tidal forces of M81 deform M82 and enormously increase the phenomena of star formation making it a "Starburst" galaxy causing the formation of super clusters. M81 is also known as the Bode Galaxy or NGC 3031, it is a rather bright spiral galaxy was first observed in 1774 by Johann Elert Bode, from which it takes its name, later in 1781 Charles Messier inserted it in his catalog, M82 also known as "Cigar Galaxy" or NGC 3034 is an active galaxy like its companion M81, this galaxy reveals a powerful magnetic field and is a source of intense radio waves. A huge explosion is taking place in its center which has now lasted for 1.5 million years, where fragments of incandescent matter move away from the galactic core at a thousand km / s, the mass involved in the explosion is equivalent to five million suns. It was also discovered by Bode in 1774.
M64 Black Eye Galaxy
Messier 64, Black Eye Galaxy (also known as Devil's Eye Galaxy), is a spiral, pinwheel-shaped galaxy visible in the constellation Berenice's Coma.
Opposite the bright galactic centre is a conspicuous dark band of light-absorbing dust, hence the nickname 'Black Eye'. It has a size of about 50000 light years and is about 17.3 million light years away from Earth. It is characterised by its bizarre internal movement. The gas in the outer regions of this extraordinary galaxy is rotating in the opposite direction to the gas and stars in its inner regions. This strange behaviour can be attributed to a merger between M64 and a satellite galaxy that occurred over a billion years ago.
NGC 2903
NGC 2903 is a barred spiral galaxy in the constellation of Leo about 20.5 million light years from the solar system discovered by William Herschel in 1784.This is a galaxy in many ways similar in shape to the Milky Way. Its size is only slightly smaller than ours, with an area of about 80,000 light years. But unlike ours, it is younger and has a cluster of bright massive stars in place of the globular.The central region of the galaxy has an exceptional rate in terms of star formation, concentrated in a ring around the nucleus, which has a diameter of just over 600 parsecs and includes not only a large number of bright young people, but also a notable presence of emission nebulosity and dark dust.
Wolf-Rayet
Wolf-Rayet stars (often abbreviated as WR stars) are massive and hot stars in the final stages of their evolution. They are named after French astronomers Charles Wolf and Georges Rayet, who first discovered them in 1867. Wolf-Rayet stars are characterized by intense radiation emissions, particularly in the ultraviolet range. WR stars are typically very massive, with masses ranging from 5 to 20 times that of our Sun, or even more. These stars have exhausted the hydrogen in their cores and have entered the phase of fusing heavier elements, such as helium, carbon, and oxygen. This fusion process generates a tremendous amount of energy, causing the star to become extremely hot.Wolf-Rayet stars are known for their intense mass loss. Due to the enormous amount of energy they emit, these stars eject material into the surrounding space through powerful stellar winds, with speeds on the order of thousands of kilometers per second. This mass ejection contributes to the formation of circumstellar nebulae made of gas and dust.
WR 134
Wolf-Rayet stars (WR) are stars that exhibit broad and prominent emission lines of ionized helium and highly ionized nitrogen or carbon. Their spectra indicate a significant surface enrichment of heavy elements, hydrogen depletion, and strong stellar winds. WR 134 is one of the first WR stars discovered by astronomers Charles Wolf and Georges Rayet in 1867.WR 134 has shed its outer atmosphere, which is now disturbed by the hot and fast winds from the WR star, forming a visible bubble. It is most easily observed in the light of ionized oxygen ([OIII]) and therefore appears turquoise in images of the WR bubble. WR 134 itself is visible as the brightest star near the apparent center of the bubble.
Dark Nebulae
A dark nebula or molecular cloud is a large cloud composed predominantly of gas (molecular hydrogen and helium) with a small fraction of dust responsible for the cloud's appearance. Dark nebulae are among the coldest known objects in the universe. Their appearance is primarily due to the presence of this small amount of dust, which absorbs light (especially in the blue part of the spectrum).Dark clouds can be most easily observed when they obscure part of an emission nebula or reflection nebula, or when they block the light from background stars. The largest dark nebulae, known as giant molecular clouds, have a mass of about one million times that of the Sun. They often have highly irregular shapes, with no well-defined outer boundaries and many filaments.The largest dark nebulae are visible to the naked eye and appear as dark patches against the brighter background of the Milky Way.
B 150 Seahorse Nebula
Barnard 150 (B150), also known as the Seahorse Nebula, is a dark nebula located in the constellation Cepheus. It is part of the catalog of dark nebulae compiled by Edward Emerson Barnard in the early 20th century. This nebula is notable for its distinctive shape, resembling a seahorse, visible against the bright starry background of the Milky Way.B150 is primarily composed of gas and dust, which block the light from background stars, making it appear as a dark silhouette. It is located about 1,200 light-years from Earth and is a region of star formation, containing young stars and protostars hidden within. The dust and gas within the nebula serve as the main ingredients for the birth of new stars.Its position in the constellation Cepheus makes it an interesting target for astrophotography and astronomical observation, especially in long-exposure images where the contrast between the dark nebula and the starry background is particularly striking.
LDN 1157
LDN 1157 (Lynds Dark Nebula 1157) is a dark nebula in the constellation Taurus, approximately 800 light-years from Earth. It is a dense region of gas and dust that blocks background starlight, appearing as a dark patch. LDN 1157 is an active site of star formation, hosting young stellar objects and protostars. It is known for molecular outflows, including carbon monoxide emissions, which provide insights into its structure and dynamics. The nebula is important for studying the early stages of star and planetary formation. Best observed with infrared or submillimeter telescopes, as visible light is obscured by dust.
NGC 7035 Iris Nebula
LDN 1157 (Lynds Dark Nebula 1157) is a dark nebula in the constellation Taurus, approximately 800 light-years from Earth. It is a dense region of gas and dust that blocks background starlight, appearing as a dark patch. LDN 1157 is an active site of star formation, hosting young stellar objects and protostars. It is known for molecular outflows, including carbon monoxide emissions, which provide insights into its structure and dynamics. The nebula is important for studying the early stages of star and planetary formation. Best observed with infrared or submillimeter telescopes, as visible light is obscured by dust.
LDN 772 The Lock Ness Nebula
Several dark dust structures named with the acronyms LDN and LBN (LBN 133 and 134, LDN 768, 769, 772, 773, 774, 775, 779) stand out on a carpet of stars assuming the shape of the "Monster" of Loch Ness." Furthermore, there are two beautiful reflection nebulae in the area. The gas and dust within these clouds can collapse under the influence of gravity, leading to the formation of new stars. Observations of these regions help astronomers better understand star formation processes and the evolution of molecular clouds.
Supernova Renmant
AA supernova remnant is the material ejected by a massive explosion. This occurs when a very massive star exhausts its nuclear fuel and collapses under its own gravitational force, or when a white dwarf accumulates enough material from a companion star to reach the critical mass, causing it to collapse. In both cases, the resulting explosion violently ejects most of the star's matter.
In the case of a massive star's explosion, the star's core can collapse so rapidly that it forms an extremely compact object, usually a neutron star or a black hole. In all such explosions, the outer layers of the star are expelled at speeds of thousands of kilometers per second, creating an expanding cloud of gas and dust.A supernova remnant can be diffuse, an ephemeral object that dissolves into the interstellar medium within a few thousand years, or compact, such as neutron stars or black holes, which are virtually immortal.Numerous supernova remnants are observable, as supernovae occur in our galaxy at a rate of about one every few decades.
M1 Crab Nebula
The Crab Nebula (M1 or NGC 1952) is a supernova remnant visible in the constellation Taurus. Discovered in 1731 by English astronomer John Bevis, the nebula became the first object in the catalog of astronomical objects published by Charles Messier in 1774, designed to help comet hunters avoid confusion with similar-looking objects. Spanning approximately six light-years, the nebula is composed of expanding gases ejected during the explosion of Supernova 1054. This supernova produced a glow so bright it was observed with the naked eye for the first time on July 4, 1054, and was recorded in detail by Chinese and Arab astronomers of the time.The Crab Nebula is located about 6,500 light-years from the solar system in the Perseus Arm of the Milky Way. At its center lies the Crab Pulsar (also known as PSR B0531+21), a neutron star with a diameter of about 28–30 kilometers. Discovered in 1968, the pulsar rotates at an astonishing rate of 30 times per second, emitting pulses of radiation across the electromagnetic spectrum, from radio waves to gamma rays. This makes the Crab Nebula a valuable object for studying both the aftermath of supernova explosions and the behavior of neutron stars.
Planetary Nebulae
Planetary nebulae are fascinating and complex structures representing a transitional phase in the life of medium- to low-mass stars (about 1–8 solar masses). They form when a star nearing the end of its life expels its outer layers into space, leaving behind a hot, dense core that will become a white dwarf. The central star emits intense ultraviolet radiation that ionizes the surrounding gas, causing it to glow in vibrant colors. These colors result from emissions of elements like hydrogen (red-pink), doubly-ionized oxygen (green-blue), and nitrogen (deep red). Planetary nebulae exhibit a variety of shapes, including spherical, elliptical, bipolar, and more complex forms, influenced by factors such as magnetic fields, stellar winds, or the presence of companion stars. Typically spanning a few light-years, they have a short lifespan on cosmic scales, about 10,000–20,000 years, before dispersing into the interstellar medium. Examples include the Ring Nebula (M57), the Helix Nebula (NGC 7293), and the Dumbbell Nebula (M27). Planetary nebulae play a crucial role in enriching the interstellar medium with heavier elements like carbon, nitrogen, and oxygen, contributing to the formation of new stars and planets. The term "planetary" originated in the 18th century when their round appearance through early telescopes resembled planets, though they have no relation to them. They offer a glimpse into the future of our Sun, which will form a planetary nebula in about 5 billion years.
M27 Dumbbell Nebula
M27, or the Dumbbell Nebula, is a bright planetary nebula located about 1,200 light-years away in the constellation Vulpecula. Discovered in 1764 by Charles Messier, it spans 2.5 light-years and has a characteristic dumbbell shape formed by gas ejected from a dying star. The nebula glows with red hydrogen and green-blue oxygen emissions, illuminated by its central white dwarf, which has a temperature of over 85,000 K. With a magnitude of +7.4, M27 is visible with binoculars or small telescopes, especially during summer in the Northern Hemisphere. It offers valuable insights into stellar evolution and the enrichment of the interstellar medium.
Hubble Palette
The Hubble Palette is a color mapping technique used in astrophotography to highlight the structure and composition of celestial objects. It assigns red to sulfur-II (SII) emissions, green to hydrogen-alpha (Hα), and blue to oxygen-III (OIII), based on narrowband filters. Popularized by the Hubble Space Telescope, this palette is not true to natural color but emphasizes the distribution of elements and processes in nebulae. Iconic images like the Pillars of Creation showcase its ability to reveal intricate details. Widely used by both professional and amateur astrophotographers, the Hubble Palette creates striking, high-contrast images that combine scientific insight with visual appeal.
Cygnus wall
The Cygnus Wall, viewed in the SHO (Hubble Palette), showcases the star-forming region within the North America Nebula (NGC 7000) with striking detail. In this palette, sulfur-II (SII) is mapped to red, hydrogen-alpha (Hα) to green, and oxygen-III (OIII) to blue, emphasizing the distribution of ionized gases. The Wall appears as a glowing ridge of gas and dust with intricate structures like pillars, filaments, and dark lanes, shaped by stellar winds and ultraviolet radiation from nearby massive stars. The SHO technique enhances contrasts between gases, revealing the nebula’s dynamic processes and composition while providing a vibrant and aesthetically captivating view of this stellar nursery.
IC443 Jellyfish Nebula
IC 443 is a diffuse nebula located in the constellation Gemini, the result of a supernova explosion about 30,000 years ago. It is located about 5,000 light years from Earth. The nebula formed as a result of a supernova explosion, releasing a large amount of gas and dust into space. IC 443 has a complex and interesting structure, with filaments of ionised gas and cosmic dust. Its shape is sometimes associated with that of a jellyfish, hence the alternative name Medusa Nebula. The region around IC 443 is still active in terms of stellar activity, all due to the continuous interactions between stellar winds and the enormous amounts of surrounding dust and gas. The image was created using the Hubble palette technique to perceive and distinguish individual hydrogen, sulphur and oxygen emissions.
NGC281 Pacman Nebula
The Pacman Nebula (NGC 281) is a large emission nebula appearing near the orange giant Schedar in the constellation Cassiopeia. The nebula lies approximately 9,200 light years away and occupies 35 arcminutes of the apparent sky. It is also catalogued as IC 11 and Sharpless 184 (Sh2-184). It was named the Pacman Nebula for its resemblance to Pac-Man, the character in the popular 1980s maze video game. In optical images, a dark dust lane forms the Pac-Man’s mouth. The Pacman Nebula stretches 48 light years across. It is a star-forming region that contains young stars, large dark dust lanes and Bok globules. Bok globules are small, dense dark nebulae packed with material from which new stars are formed. The dark dust lane spreads unevenly across glowing clouds of hydrogen and its appearance suggests that it being sculpted by a massive star in the background, concealed by the dark clouds.
Bright Nebulae
A nebula is an interstellar cluster of dust, hydrogen, and plasma. There are several types of nebulae: reflection nebulae, which shine thanks to the light emitted by a star passing through them; planetary nebulae or supernova remnants, formed from the explosions of massive stars; and emission nebulae, which are interstellar clouds of ionized gas that emit light in various colors depending on their chemical composition. Due to the abundance of hydrogen in interstellar gas and the relatively low energy required for its ionization, many emission nebulae appear red. Where higher energy is present, other elements such as oxygen, sulfur, and helium can become ionized, creating contrasting colors ranging from blue to green (which are invisible to the human eye). Nebulae are true star factories, as molecular clouds, dark nebulae, and HII regions (ionized hydrogen) within them interact with stellar winds and gravity, triggering star formation processes.
M8-M20 Lagoon & Trifid nebulae
The Lagoon and Trifida Nebulae are the brightest pair of nebulae in the constellation Sagittarius, queens of the summer sky. The Lagoon Nebula (M8) is an HII region or interstellar cloud that glows red due to ionised hydrogen as it is crossed by stellar winds. The distance of the nebula from Earth is estimated at 5000 light years, which would make its physical diameter about 100 light years. The Lagoon is an active stellar nursery and contains a number of dark globules, clouds of protostellar material from which new stars form and are born. From Earth, the apparent size of the Lagoon is 40 by 90 arcminutes and shines at apparent magnitude +6.0.The Trifid Nebula (M20) consists partly of an emission nebula and a considerable reflection zone. The emission nebula glows red in the characteristic colour of ionised hydrogen, while the reflection nebula is blue due to nearby hot, young stars. The Trifid Nebula takes its name from its three-lobed appearance. The distance to the nebula is estimated at 5000 light years but there are great uncertainties about this value. The apparent size of the Trifida is 28 arcminutes and its apparent magnitude is +6.3.
IC 1318 & Sadr region
Located in the heart of the constellation Cygnus, Gamma Cygni, more commonly known as Sadr, is one of the brightest stars in the summer sky. It is a yellow supergiant that lies at the center of the "Northern Cross," a star formation in the constellation Cygnus. With an apparent magnitude of around 2.2, it is easily visible to the naked eye. Surrounding it, and in perspective, there are extensive clusters of ionized hydrogen, particularly IC 1318, or the "Butterfly Nebula." This is an emission nebula that shines due to the radiation emitted by the young stars within it. The nebula is divided into several parts by dark nebulas, creating complex and fascinating patterns of light. Near Sadr, there is also NGC 6910, an open star cluster often called the "Rock Cluster" due to the particular arrangement of its stars. In this area, there is intense star formation activity, where young massive stars ionize the surrounding gas, causing the nebulas to shine and creating splendid celestial landscapes. It is easily identifiable in the Northern Hemisphere, especially during the summer, by looking straight up above us.
NGC2264 The Cone nebula
The Cone Nebula located in the winter constellation of the UNICORN, is made up of a large cloud of hydrogen ionized by the ultraviolet radiation emitted by the stars that make up the star cluster NGC2264, called the "Christmas Tree". vertex of the "Cone" nebula. This nebula is a part of a vast dark nebula, consisting of dust and molecular hydrogen, which stands out on the underlying emission nebula and recognizable by its typical reddish color. It was first observed by the English astronomer William Herschel on December 26, 1785 and is about 2700 light years from Earth.
NGC 6888 Crescent Nebula
The Crescent Nebula (NGC 6888) is an extraordinary cosmic bubble approximately 25 light-years across, sculpted by the winds of its brilliant, massive central star. This image was captured using narrowband filters that isolate the light emitted by hydrogen and oxygen. Ionized oxygen atoms produce the characteristic cyan-green outer shell that encases the intricate folds and wispy filaments.At the heart of the nebula is the central star, classified as a Wolf-Rayet star (WR 136). This blazing star sheds its outer layers through a powerful stellar wind, ejecting an amount of material equivalent to one solar mass every 10,000 years. The nebula's complex structures are likely the result of this intense wind interacting with material expelled during an earlier phase.As it exhausts its fuel and reaches the end of its life cycle, the star will collapse and explode, ejecting its glowing gases outward to create a supernova.
The Crescent Nebula is located in the rich constellation Cygnus, approximately 5,000 light-years away from Earth.
Star Clusters
Star clusters are groups of stars born from the same cloud of gas and dust, bound together by gravity, and are divided into open clusters and globular clusters. Open clusters, such as the Pleiades and Hyades, are young, contain a few hundred to a few thousand stars, and are located in the galaxy's disk, with an irregular and bright arrangement. Globular clusters, like Omega Centauri, are billions of years old, contain hundreds of thousands of stars densely packed in a spherical shape, and are found in the galactic halo, representing some of the oldest structures in the universe.
M45 The Plaiades
The Pleiades, also known as the Seven Sisters or M45 in the catalog of Charles Messier, is an open cluster located in the constellation Taurus. This cluster, approximately 440 light-years away, consists of several stars visible to the naked eye, with greater visibility in locations less affected by light pollution.The stars of the Pleiades are closely bound by gravity and share a common origin. Due to their relative proximity, they appear warmer than usual and exhibit predominant colors of blue or white giants. The cluster is young, with an estimated age of about 100 million years and a projected lifespan of another 250 million years.The historical significance of the Pleiades is evident in their mention by ancient authors such as Homer and Ptolemy. The stars are also featured in the Nebra Sky Disk, a bronze artifact dating back to 1600 B.C. found in Germany, representing one of the earliest known depictions of the cosmos.The cluster's position north of the celestial equator makes it visible from all populated areas on Earth, down to the Antarctic Circle. The Pleiades are easily identifiable even in urban environments affected by light pollution, appearing as a group of closely spaced blue stars with a distinctive shape.
M13 Hercules Cluster
The Hercules Globular Cluster (M13) is one of the brightest and most famous globular clusters in the northern sky. Located in the constellation Hercules, M13 is about 22,000 light-years away and contains several hundred thousand stars densely packed into a spherical shape. This ancient cluster, estimated to be around 11.65 billion years old, is a stunning example of the universe's history and evolution. With its densely concentrated core and numerous bright stars, M13 is a favorite target for both amateur and professional astronomers, offering a glimpse into the early stages of our galaxy's formation.
M44 Beehive Cluster
A mere 600 light-years away, M44 is one of the closest star clusters to our solar system. Also known as the Praesepe or the Beehive cluster its stars are young though, about 600 million years old compared to our Sun's 4.5 billion years. Based on similar ages and motion through space, M44 and the even closer Hyades star cluster in Taurus are thought to have been born together in the same large molecular cloud. An open cluster spanning some 15 light-years, M44 holds 1,000 stars or so and covers about 3 full moons (1.5 degrees) on the sky in the constellation Cancer. Visible to the unaided eye, M44 has been recognized since antiquity.
NGC 869 & NGC 884 Double Cluster
The Double Cluster is a breathtaking pair of open star clusters, NGC 869 and NGC 884, located in the constellation Perseus. Situated about 7,500 light-years away, these clusters are relatively young, with an estimated age of 12.8 million years, and are rich in bright, massive stars. The Double Cluster is a stunning sight in the night sky, offering a view of two closely positioned clusters shining with a mix of blue and orange stars. Its beauty and proximity make it a popular target for astrophotography and a favorite among stargazers exploring the wonders of our galaxy.
Polar alignment with Synscan Skywatcher
In this tutorial, I will explain how to perform a proper polar alignment using the “Polar Alignment” tool on the SynScan Hand Controller for SkyWatcher mounts.
When we do astrophotography, we need an equatorial mount to track the Earth's rotation. To achieve this, it is necessary to "align" our mount with the Celestial North Pole, using Polaris as a reference. This is done by adjusting the polar scope included with most equatorial mounts.However, during this process, some initial issues might arise: what if you don’t have a clear view of the north or can’t see Polaris? How would you align your mount? Well, don’t throw your equipment off the balcony! Follow this simple procedure to perform a polar alignment using the Polar Alignment tool on the SynScan Hand Controller for SkyWatcher mounts.Let’s Begin:There are several ways to work around this issue. One of the most well-known and effective is the Bigourdan method. This method uses drift analysis to achieve very precise alignment, but the downside is its convoluted, lengthy, and complicated process. Instead, we want to achieve quick results without overcomplicating things. Therefore, we’ll turn to technology and use a tool available on many equatorial mounts: the Polar Alignment tool.Specifically, I will demonstrate the Polar Alignment tool included in the SynScan Hand Controller for SkyWatcher mounts. Unfortunately, this tool is not available in all versions of the Hand Controller (if I’m not mistaken, it’s available from version 3.35 onward), so please check your version when turning on the controller before proceeding.
The Procedure for Polar Alignment with the SynScan Hand ControllerLet’s get straight to the steps:1. First, roughly position your mount facing north, perhaps using a compass for assistance.
2. Next, turn on the mount and enter all the required data (coordinates, date, time, altitude, etc.).
3. Start by performing a star alignment: remember that to use the Polar Alignment tool, you need to perform at least a 2- or 3-star alignment.
We will select the stars suggested by the Hand Controller based on our field of view. At this point, the camera you’ll use for photography (or the eyepiece if you’re a visual observer) and the associated software will come into play. In this example, I used a SkyWatcher EQ6-R mount, a ZWO ASI 294 MC Pro camera, and SharpCap software. If you’re using a DSLR, I recommend the Astro Photography Tool (APT) software, which is compatible with many Canon and Nikon DSLRs.In our case, since we have a very limited field of view (ranging between West and Northwest), we’ll opt for a 2-star alignment: Alpheratz and Deneb. Open SharpCap, select your camera from the “Cameras” menu, and adjust the gain and exposure time until the stars appear in your field of view.
Activate your reticle (the red crosshair next to the Zoom function), and now use the arrow keys on your controller to move the selected star until it is perfectly centered in the crosshair. Once aligned, press ENTER.
Repeat the same procedure with the second star.
Once this alignment is complete, the mount will provide, via the Hand Controller, some values indicating the polar error in degrees, minutes, and seconds. These values will show how far off the alignment is in AZ (Azimuth) and EL (Elevation).
Let's read the values: it tells us that we have an error of 2 minutes and 59 seconds in Elevation and 26 minutes and 34 seconds in Azimuth.
Reducing AZ EL Error
Here is the procedure to minimize this error. By scrolling through the menu using the down arrows on the Hand Controller, we will find the Polar Alignment tool.
Press ENTER, and it will prompt us to choose a star on which it will apply the corrections we provide by adjusting Azimuth and Elevation.
In our case, we will select Deneb again.
Using the arrows on the Hand Controller, we will bring it back to the center of the SharpCap crosshair.
Now, by pressing ENTER, the Polar Alignment tool will shift our star by an amount equal to the Elevation error calculated after the 2/3-star alignment—in our case, 2 minutes and 59 seconds.
On the SharpCap crosshair, we will see this situation (refer to the figure).
As you can see, the star has been shifted. Now, by adjusting ONLY the Elevation adjustment screws (refer to the figure), we will aim to bring the star back to the center of the SharpCap crosshair.
Don't worry if we can't bring it precisely to the center. Remember, we are correcting only one axis at a time, so the important thing is to get as close to the center as possible.
Once completed, the Hand Controller will register the adjustment and prompt us to make the correction in Azimuth as well.
The Polar Alignment tool will shift our star by an amount equal to the Azimuth error calculated after the 2/3-star alignment in our case, 26 minutes and 34 seconds.Tip: Since this is a very large shift, our reference star will likely have moved out of the camera's field of view. To assist with the adjustments, it is advisable to have a finder scope mounted on the main tube to help guide the movements and bring the star back to the center of the crosshair.Repositioning the Star
To reposition the star and allow the mount to register the correction, this time we need to adjust the Azimuth adjustment screws (refer to the figure).
Again, we aim to bring the star as close as possible to the center of the crosshair. Once Azimuth has been adjusted, we can press ENTER on the Hand Controller to complete the correction phase.Now, we need to verify whether the polar alignment error has reached an acceptable value. This is checked by performing a new 2/3-star alignment.Personal Tip: I prefer to return the mount to its starting position (with the tube pointing North) by powering it off and restarting the system.
From the Hand Controller, scroll through the menus and select Park Scope, which will park the mount while retaining all the previously entered data.
Turn off and restart the mount. The Hand Controller will ask if we want to restore the previous Park data. We will select Yes, recalling the configuration and simply confirming the date and time.
Once the data has been restored, use the selection arrows to scroll through the menu and choose "Setup". In the Setup menu, look for the option "Alignment".
Verification of Polar Alignment Error Correction
At this stage, repeat a 2 or 3-star alignment to verify that the polar alignment error has been minimized. Once again, we will first point to Alpheratz and then to Deneb, following the same steps as outlined earlier.At the end of the process, check the Hand Controller to see the updated error values it provides.
As you can see, we achieved an excellent result given the initial conditions, and we managed to do so in just one pass. That said, if the result is not satisfactory, the entire procedure can be repeated multiple times to achieve better accuracy.With values like these, I can take 600-second guided exposures with image deviation below 5%. Of course, mechanical errors or other variables may come into play, but overall, I’ve been using this system from my balcony with good results for about two and a half years.This tutorial comes from my personal experience as a beginner who needed to align to the polar axis without being able to see it and with limited guidance available online.
Nowadays, there are many programs available, both free and paid, for polar alignment. Therefore, I recommend my method especially to beginners who are entering the world of astrophotography for the first time.This approach may be simpler for those who want to start aligning to the pole in an assisted way without relying on software. It’s particularly useful for those photographing with a DSLR camera without using a PC or automated systems like ASIair, Stellarmate, and similar tools.Remember, if something goes wrong, don’t blame me! 😄
Clear skies! 🌌