Comet 220P/McNaught is a periodic, Jupiter-family comet that completes an orbit around the Sun every 5.5 years. Discovered on May 20, 2004, by astronomer Robert H. McNaught, the comet follows an elliptical path ranging from a closest approach (perihelion) of 1.55 AU—just outside Mars's orbit—to a maximum distance (aphelion) of 4.68 AU. It possesses a small nucleus with an estimated radius under 1.3 km.
The Messier 76 (M76) nebula—commonly known as the Little Dumbbell Nebula—is a bipolar planetary nebula located roughly 2,500 to 3,500 light-years away in the constellation Perseus. Its complex 3D architecture is shaped by gas ejected from a dying star as it sheds its outer layers.
Located in the constellation of Cassiopeia, SNR G107.5-5.2 is a gigantic and extremely delicate supernova remnant, spanning approximately 3 degrees across the sky.
Discovered in 2023 by Bray Falls, Marcel Drechsler and their team, this structure is distinguished by its remarkably delicate ionized oxygen emission lines (OIII 500.7 nm). Its shock waves, forming what appear to be vast gaseous “draperies”, have earned the object the nickname The Nereides, in tribute to the sea nymphs of Greek mythology.
The Iris Nebula (NGC 7023) formed through a combination of star formation, light scattering, and stellar interaction with surrounding interstellar dust. Located approximately 1,300 light-years away in the constellation Cepheus, it spans about six light-years across.
Deep in the constellation Cassiopeia lies LDN 1355, the "Helping Hand" nebula. Located approximately 1,400 light-years away, this dark nebula features vast clouds of cosmic dust silhouetted against a brilliant backdrop of stars, glowing alongside the reflection nebula vdB 9 and variable star SU Cassiopeiae.
Sharpless 114 (Sh2-114, LBN 347), commonly referred to as the Flying Dragon Nebula, is a faint emission nebula located approximately 3,000 light-years away in the constellation Cygnus. Exhibiting a complex morphology with long, thread-like filaments of ionized gas, its spectral signature is dominated by deep red Hydrogen-Alpha emission alongside subtle doubly ionized oxygen cyan regions. While cataloged primarily as an ha region, its delicate arc structures and the absence of a clear central ionizing star lead astronomers to debate whether it is driven by ionizing stellar radiation, an ancient supernova remnant, or an energetic stellar wind-blown bubble interacting with the interstellar medium.
The Vulcan Nebula (cataloged as WPS 46) is a faint deep-sky emission and reflection nebula situated roughly two degrees west of the famous spiral galaxies Messier 81 and Messier 82 in the constellation Ursa Major. Discovered and brought to prominence by amateur astrophotographers capturing ultra-deep exposure widefield integration data, the object is embedded within extensive integrated flux nebula (IFN) clouds, dust and ionized gas floating above the plane of the Milky Way that are lit up by ambient starlight and ionized by surrounding stars like TYC 4376-968-1. Because of its extremely low surface brightness, bringing out its faint blue-green oxygen structures and hydrogen-alpha filaments requires hundreds of hours of total integration time across multiple optical systems and dark-sky sites.
Lunar regolith is a layer of fine dust, fragmented rock, glass spheres, and mineral grains covering the Moon's bedrock, formed by billions of years of meteoroid impacts, solar wind, and radiation exposure without atmospheric weathering or organic matter. Over 98% of its mass is composed of oxygen, silicon, iron, aluminum, calcium, magnesium, and titanium, primarily structured in minerals like plagioclase feldspar, pyroxenes, olivine, and ilmenite. Its composition varies significantly by region: the light-colored Lunar Highlands are rich in aluminum-heavy anorthosite, whereas the dark Lunar Maria feature basaltic flows higher in iron and titanium. Due to constant space weathering, regolith also unique features agglutinates (grains welded together by impact-melted glass), nanophase metallic iron, and embedded solar-wind volatiles like helium-3 and hydrogen.
NGC 6726/6727 is a prominent pair of reflection nebulae located within the southern constellation Corona Australis, situated approximately 420 to 500 light-years from Earth. As reflection nebulae, they do not produce their own visible light through gas ionization; instead, fine interstellar dust particles efficiently scatter shorter wavelengths of starlight, creating a characteristic vibrant blue glow (Rayleigh scattering). This ethereal light is primarily energized and reflected by nearby hot, young stars embedded in the cloud, including the variable star TY Crs, as well as HD 176386 and HD 176269.
LBN 331 (also known as the "Cygnus Waves") is a faint, sweeping emission nebula situated in the Cygnus constellation near Omicron² Cygni (o2 Cyg) and 31/32 Cygni. Composed predominantly of delicate, filamentary tendrils of ionized hydrogen (Hα) and oxygen (O III), this low-surface-brightness deep-sky object is excited by radiation from neighboring massive stars and requires long-exposure astrophotography with narrowband filtering to properly capture against the dense background of the Milky Way plane.
Sh2-99 (Sharpless 99) and Sh2-100 (Sharpless 100) are two H II emission nebulae and active star-forming regions located in the plane of the Milky Way within the constellation Cygnus.
Both regions are embedded in the larger W58 complex, a massive molecular cloud complex and powerful radio source situated thousands of light-years away along the Perseus Arm of the Milky Way.
What makes NGC 6819 particularly remarkable to astronomers is its age and stellar population. Estimated to be between 2.3 and 2.5 billion years old, it is considerably older than typical open star clusters, which usually disperse after just a few hundred million years. Containing roughly 150 member stars, with its brightest individuals shining between 10th and 12th magnitude—its high star density and intermediate age made it a primary target for NASA's Kepler space telescope to study asteroseismology, starspots, and the long-term evolution of stars.
Silent and ancient, a cosmic serpent glides through the northern sky. Caught in the delicate interplay between dust and starlight, the reflection nebula vdB 152 glows like a celestial torch at the tip of a towering, opaque dust lane known as LDN 1221. Here in the Cepheus Flare, cosmic dust grains scatter the soft light of the embedded star BVD 111, painting the dark canvas of space with vivid shades of blue. Surrounding this stellar sanctuary, dense interstellar dust clouds cloak the background stars, weaving intricate dark lanes that reveal the quiet, ongoing birth of stars within our Milky Way.
The Minkowski 2-51 Planetary Nebula (also designated as M 2-51 or PN G103.2+00.6) is a faint planetary nebula located roughly 6,300 light-years away in the constellation Cepheus. Discovered in 1947 by the German-American astronomer Rudolph Minkowski using objective-prism survey plates at Mount Wilson, the nebula represents the expanding, glowing shell of ionized gas expelled by an aging, low- to intermediate-mass star entering its final evolutionary stages. Sometimes informally nicknamed the "Little Ring Nebula," it measures under 1 arcminute in angular size (around 39 to 56 arcseconds) and shines dimly at an optical magnitude of approximately 13.5.
The Pelican Nebula (cataloged as IC 5070 and IC 5067) is a large emission nebula situated approximately 1,800 to 2,000 light-years away in the constellation Cygnus. Spanning roughly 30 light-years across, it is a dynamic star-forming region whose glowing, ionized gas clouds trace an outline resembling a pelican's head and bill. This visible glow is caused by strong ultraviolet radiation from nearby massive stars—most notably Deneb and the energetic stars in the neighboring North America Nebula (NGC 7000), from which the Pelican is separated by a dark, dense lane of interstellar dust known as LDN 935.
The Seahorse Nebula (cataloged as LDN 1082 or Barnard 150) is a prominent dark absorption nebula situated approximately 1,200 light-years away from Earth in the northern constellation Cepheus. Unlike glowing emission or reflection nebulae, this object is composed of dense, cold cosmic dust and interstellar gas that emits no visible light of its own. Instead, it acts as an opaque silhouette, obscuring the rich, bright star fields of the Milky Way lying directly behind it.
On the night between September 11 and 12, together with my dear friend Filippo, companion of countless astrophotography adventures, we planned a night photography session to bid farewell to the summer Milky Way. The noticeably cooler conditions compared with the previous months, together with the Galactic Center setting during the early hours of the evening, encouraged us to choose a nearby coastal location for our images.
Finally, with a sky free from the excessive humidity of summer, we had the chance to carry out more meaningful tests with our UV/IR-cut modified cameras and explore the wonders of the cosmos with greater accuracy and detail. The unique scenery offered by our coastline would also help enhance a spectacle that was already magnificent on its own.
With the best intentions, we spent hours taking exposures, trying to collect as much light as possible from stars and nebulae far away in both space and time.
Apart from the Gecko Nebula itself and the dominating bright red hydrogen clouds the numerous „small“ background galaxies make this image special.
I collected the data for this image of the Gecko Nebula (LBN 437) in constellation Lacerta during 7 nights in August/September 2026 with a small refractor and an OSC camera from my balcony in Eltville, Germany - Bortle class 5.
The image represents 30.4 hours of total exposure time (15.9h without filter and 14.5h dual narrowband) - taken with following equipment:
telescope: Askar SQA85
camera: ZWO ASI2600MC Air
mount: ZWO AM5N
filter: Optolong L-eXtreme (Ha/OIII)
This wide-field view captures the famous Horsehead Nebula (Barnard 33), a dark cloud of dense interstellar dust silhouetted against the glowing red emission nebula IC 434 in the constellation Orion. Located roughly 1,300 to 1,500 light-years away near the star Alnitak, the region is sculpted by intense radiation and stellar winds from nearby massive stars, which ionize the surrounding hydrogen gas and light up neighboring reflection nebulae like NGC 2023.
In Thiago Prado's featured submission, the target for this technique is IC 2944, also known as the Running Chicken Nebula.
Located in the southern constellation Centaurus, IC 2944 is an open cluster with an associated emission nebula characterized by intricate ionization fronts, dense dark globule structures (Bok globules), and subtle transitions between Sulfur-II and Hydrogen-alpha emissions.
The (SH)(SH)OO palette technique is a custom false-color composition method used in narrowband astrophotography to combine data captured through standard Sulfur-II, Hydrogen-alpha , and Oxygen-III filters.
It modifies the traditional SHO (Hubble Palette) and HOO color-mapping schemes to achieve better contrast, dynamic range, and highlight retention for intricate nebula structures.
The Montes Apenninus (Lunar Apennines) is a rugged, prominent mountain range located on the northern near side of the Moon, forming the dramatic southeastern boundary of the vast Mare Imbrium (Sea of Rains) impact basin. Created roughly 3.9 billion years ago during the cataclysmic impact event that excavated the Imbrium basin, the range stretches for nearly 600 kilometers (370 miles) and features towering peaks such as Mons Huygens, which rises about 5.5 kilometers high. Unlike Earth's tectonic mountain chains, these mountains represent the uplifted outer rim of a giant impact crater, characterized by steep, jagged scarps facing the smooth lava plains of Mare Imbrium and gentler, sloping topography descending into the lunar highlands.
Geologically, the range encompasses several notable features, including Hadley Rille (Rima Hadley)—a deep, sinuous lava channel winding along its northern base near Mons Hadley and Mons Hadley Delta. This region achieved historical fame as the landing site for the Apollo 15 mission in 1971, where astronauts David Scott and James Irwin explored the mountainous terrain and retrieved ancient deep-crustal lunar rock samples like the famous Genesis Rock. Flanked by prominent impact structures like the 58-kilometer-wide Eratosthenes Crater at its southwestern tip and the nested Conon Crater, the Apennine range remains a prime geological showcase and a favorite target for amateur lunar observations.
This high-resolution capture highlights the rugged terrain of the lunar southern highlands, featuring the prominent impact crater Werner alongside neighboring Aliacensis. Werner, measuring roughly 70 kilometers in diameter, displays striking structural details including crisp, terraced inner walls, a well-defined rim, and a sharp central peak complex rising from its floor. Surrounding the pair is a heavily pockmarked, ancient lunar landscape sculpted by billions of years of cosmic impacts.
Captured during the August 12, 2026 total solar eclipse over León, Spain, this composite image by Engelbert Vollmer showcases the ethereal solar corona flanked by the rapid transition phases of totality. To bring out the intricate details of the Sun's outer atmosphere—a superheated plasma stretching millions of kilometers along magnetic field lines—the photograph was crafted using an HDR (High Dynamic Range) sequence. By bracket-exposing shots in 1 EV increments from 1/1000 second to 1/2 second, the camera captured both the dazzling highlights of the solar photosphere and the delicate, faint streamers of the outer corona, which were then digitally blended together.
Flanking the central eclipse image are brief, fleeting phenomena that lasted only seconds before and after totality. These edge sequences capture Baily's beads—tiny, brilliant points of light created when the final rays of sunlight stream through the rugged peaks, craters, and valleys along the Moon's silhouetted rim. Interspersed alongside bright pink solar prominences, these glowing beads merge into the diamond ring effect just as the Sun slips completely behind the Moon, offering a spectacular visual summary of the eclipse's most dynamic moments.
The Iris Nebula (NGC 7023 or Caldwell 4) is a striking reflection nebula located roughly 1,300 to 1,400 light-years from Earth in the northern constellation Cepheus. Unlike emission nebulae that glow from ionized gas, the Iris Nebula shines by scattering starlight off vast clouds of interstellar dust. At its core lies HD 200775, a massive, hot, young star about ten times the mass of the Sun that provides the main illumination for the surrounding material. This glowing dust and gas spans approximately six light-years across, forming petal-like structures that give the nebula its distinctive flower-like appearance in deep-space imagery.
In the heart of the constellation Cassiopeia, approximately 7,900 light-years from Earth, lies NGC 457, one of the most striking open clusters in the autumn sky. Known by the nicknames "Owl Cluster" or "ET Cluster," this group of stars immediately catches the eye due to the peculiar arrangement of its stars, which appear to outline the silhouette of a creature with large, bright eyes.
488 Sagittae (Nova Sagittae 2026) is a classical nova discovered on August 25, 2026, in the constellation Sagitta. Before the eruption, the system was around magnitude 20, but brightened to approximately magnitude 7 – an increase of more than 13 magnitudes, corresponding to over 200,000 times more optical flux.
This composite image captures the partial lunar eclipse over Capo Sant'Elia in Cagliari, Sardinia, creating a striking interplay between celestial mechanics and historical architecture. In the foreground, the illuminated 17th-century Torre di Calamosca stands prominently atop the rugged, dark terrain. Above, the composite exposure traces the eclipse's progression: near the center, a brilliant full moon casts a warm ambient glow, while higher up, a second lunar disk sits deeply shadowed in Earth's umbra. This characteristic coppery red hue occurs due to Rayleigh scattering, as Earth's atmosphere filters out shorter blue wavelengths of light and bends the longer red wavelengths into the umbilical shadow, illuminating the moon alongside a bright sliver of direct, reflected sunlight.
Gliding through the dark cosmic ocean of Cepheus, the vast red glow of the Flying Bat Nebula (Sh2-129) frames the ethereal, cyan body of the Giant Squid Nebula (Ou4). Powered by the ultraviolet radiation of massive surrounding stars ionizing hydrogen gas, Sh2-129 hosts the delicate doubly ionized oxygen (OIII) structure of Ou4 nestled within its wings. Discovered in 2011 by Nicolas Outters, this rare bipolar outflow spans roughly 50 light-years and is driven by the central triple-star system HR 8119—requiring dozens of hours of targeted narrowband integration to reveal its faint, captivating beauty.
Located approximately 6,000 light-years away in the constellation Cygnus, WR 134 is an extremely massive and luminous Wolf-Rayet star embedded inside a delicate, glowing bubble of blown-off gas.
Wolf-Rayet stars represent a brief, violent evolutionary phase in the lives of the universe's most massive stars (typically starting at over 20 times the mass of our Sun). WR 134 has shed its outer hydrogen atmosphere through incredibly intense stellar winds traveling at millions of miles per hour. These powerful winds collide with the surrounding interstellar medium, sweeping up surrounding gas and carving out the stunning, crescent-like ionized bubble highlighted in glowing oxygen (OIII) and hydrogen (Hα) emission lines.
Located roughly 6,500 to 7,000 light-years from Earth within the Eagle Nebula (M16), the Pillars of Creation are towering columns of cold molecular hydrogen gas and cosmic dust—spanning up to 4 light-years in length—that serve as an active stellar nursery where gravitational collapse births new stars. The intense ultraviolet light and radiation from nearby hot young stars continuously erode these structures through a process called photoevaporation, exposing dense pockets of gas called Evaporating Gaseous Globules (EGGs) containing protostars while guaranteeing the pillars will completely dissolve over the next few million years.