In the hearth of Corona Australis

Large clouds of cosmic dust spread over a rich starfield in this patch of sky near the northern border of Corona Australis, the southern crown. At the center is the beautiful group of reflection nebulae NGC 6726, 6727, 6729 and IC 4812. The characteristic blue color is produced when the light of hot stars is reflected by cosmic dust. Top right is the globular cluster NGC 6723, which is actually about 30,000 light years away, well beyond the Corona Australis dust clouds. Takahashi CCA250 (250/f5) - ZWO 6200MM - L (280m) R (90m) G (90m) B (70m) - AMT Observatory (A.Lau/M.Lorenzi/T.Tse), Río Hurtado, Chile. Image processing M.Lorenzi.

M42 Trapezium from white zone

The core of the Orion nebula M42 imaged from my badly light polluted terrace in Singapore (white zone). A quick experiment of deep sky "lucky imaging" technique, 60 x 10 sec subs, no flat, no dark, no bias (and no guiding ^_^). C14 + Starizona reducer 0.63x (F=2460 mm / f/6.9) - ZWO ASI533MC - ZWO Duo Band filter - iOptron CEM120 - Singapore

The Dark Tower in Scorpius

In silhouette against a crowded star field toward the constellation Scorpius, this dusty cosmic cloud evokes for some the image of an ominous dark tower. In fact, clumps of dust and molecular gas collapsing to form stars may well lurk within the dark nebula, a structure that spans almost 40 light-years across this gorgeous telescopic portrait. Known as a cometary globule, the swept-back cloud, extending from the lower right to the head (top of the tower) left and above center, is shaped by intense ultraviolet radiation from the OB association of very hot stars in NGC 6231, off the upper edge of the scene. That energetic ultraviolet light also powers the globule's bordering reddish glow of hydrogen gas. Hot stars embedded in the dust can be seen as bluish reflection nebulae. This dark tower, NGC 6231, and associated nebulae are about 5,000 light-years away (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha(330m) L (330m) R (130m) G (120m) B (180m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia. Spikes added with StarSpikes Pro 4.

Monoceros nebular complex

What do the following things have in common: a cone, the fur of a fox, and a Christmas tree? Answer: they all occur in the constellation of the unicorn (Monoceros). Just below the center of the left panel of this 4 degree wide mosaic is a star forming region cataloged as NGC 2264. The complex jumble of cosmic gas and dust is about 2,700 light-years distant and mixes reddish emission nebulae excited by energetic light from newborn stars with dark interstellar dust clouds. Where the otherwise obscuring dust clouds lie close to the hot, young stars they also reflect starlight, forming blue reflection nebulae. Outlined by the red glow of hydrogen gas, the cone points toward the left and bright, blue-white S Monocerotis. Itself a multiple system of massive, hot stars S Mon is adjacent to bluish reflection nebulae and the convoluted Fox Fur nebula. Given their distribution, the stars of NGC 2264 are also known as the Christmas Tree star cluster. The curious compact cometary shape at the bottom of the left panel is known as Hubble's Variable Nebula. Expansive dark markings on the sky are silhouetted by a larger region of fainter emission with yellowish open star cluster Trumpler 5 near the center of the frame. On the right panel lays several interesting objects as well, with the largest bluish reflection nebula at the utmost right being IC2169, known as Dreyer's Nebula. The color comes from scattered star light of the illuminating stars which are either in or behind it. The nebula is blue for the same reason our sky is blue. The tiny molecules of dust and gas scatter blue light better than the other colors due to its short wavelength. It matters little what color the illuminating stars are, as long as they emit some blue light the nebula was take on a blue color same as the somewhat yellow sun still results in our blue sky. IC2169 is thought to be part of the same huge cloud of dust and gas that includes the Cone Nebula as well as the Christmas Tree, laying at the same distance and considerably further away than the nearby Orion Nebula complex. The remaining bright reflection nebula are NGC 2245, NGC 2246 and IC446 which seems connected to the Dreyer's Nebula by a bridge of dust (text adapted from APOD). Two panel mosaic, Apo TEC140 (140/f7.2) - FLI Proline 16803 - total exposure Ha(480m) L(400m) R (270m) G (270m) B (270m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia. Spikes added with StarSpikes Pro 4.

The Rosette Nebula

Would the Rosette Nebula by any other name look as sweet? The bland New General Catalog designation of NGC 2237 doesn't appear to diminish the appearance of this flowery emission nebula. 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, insulated by a layer of dust and hot gas. Ultraviolet light from the hot cluster stars causes the surrounding nebula to glow. The Rosette Nebula spans about 100 light-years across, lies about 5000 light-years away, and can be seen with a small telescope towards the constellation of the Unicorn (Monoceros). (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha(360m) OIII(360m) L (300m) R (120m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia. Spikes added with StarSpikes Pro 4.

Snake in the Dark

Dark nebulae snake across a gorgeous expanse of stars in this telescopic view toward the pronounceable constellation Ophiuchus and the center of our Milky Way Galaxy. In fact, the twisting central shape seen here is well known as the Snake Nebula. It is also listed as Barnard 72 (B72), one of 182 dark markings of the sky cataloged in the early 20th century by astronomer E. E. Barnard. Unlike bright emission nebulae and star clusters, Barnard's nebulae are interstellar dark clouds of obscuring gas and dust. Their shapes are visible in cosmic silhouette because they lie in the foreground along the line of sight to rich star fields and glowing stellar nurseries near the plane of our Galaxy. Many of Barnard's dark nebulae are themselves likely sites of future star formation. Barnard 72 is about 650 light years away. With bluish star 44 Ophiuchi at bottom left, the intriguing star field spans nearly 2 degrees or almost 20 light-years at the estimated distance of the Snake Nebula (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - L (210m) R (120m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia. Spikes added with StarSpikes Pro 4.

Tarantula Nebula (NGC2070) in LMC

The 16th century Portuguese navigator Ferdinand Magellan and his crew had plenty of time to study the southern sky during the first circumnavigation of planet Earth. As a result, two fuzzy cloud-like objects easily visible to southern hemisphere skygazers are known as the Clouds of Magellan, now understood to be satellite galaxies of our much larger, spiral Milky Way galaxy. About 160,000 light-years distant in the constellation Dorado, the Large Magellanic Cloud (LMC) is seen here in a remarkably deep, colorful composite image, starlight from the central bluish bar contrasting with the telltale reddish glow of ionized atomic hydrogen gas. Spanning about 15,000 light-years or so, it is the most massive of the Milky Way's satellite galaxies and is the home of the closest supernova in modern times, SN 1987A. The prominent patch at top left is 30 Doradus, also known as the magnificent Tarantula Nebula. The giant star-forming region is about 1,000 light-years across and is the largest and most complex star forming region in the entire galactic neighborhood. Were it placed at the distance of Milky Way's Orion Nebula, only 1,500 light-years distant and the nearest stellar nursery to Earth, it would appear to cover about 30 degrees (60 full moons) on the sky. Intriguing details of the nebula are visible in the above image shown in composite narrowband and RGB "true colors". The spindly arms of the Tarantula nebula surround NGC 2070, a star cluster that contains some of the brightest, most massive stars known, visible in blue in the image center. Since massive stars live fast and die young, it is not so surprising that the cosmic Tarantula also lies near the site of a close recent supernova (text adapted from APOD). Officina Stellare Rifast 500 (500/f3.8) - FLI Proline 16803 - Ha (270m) OIII (270m) R (60m) G (60m) B (60m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Cometary Globule CG30/31/38 in Puppis

Cometary globules, first observed in 1976, are interstellar clouds with comet-like morphology, consisting of compact, dusty, and opaque heads and long, faintly luminous tails. Unlike most dark clouds, CG's are isolated neutral globules surrounded by a hot ionized medium. Most CG's known are located in the Gum nebula, a large HII region mostly stretching between the constellations of Vela and Puppis. CG30/31/38 is a cometary globule and dark clouds complex located in southern portion of the Gum Nebula. Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (300m) L (280m) R (120m) G (120m) B (150m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Cometary Globule CG13 in Puppis

Cometary globules, first observed in 1976, are interstellar clouds with comet-like morphology, consisting of compact, dusty, and opaque heads and long, faintly luminous tails. Unlike most dark clouds, CG's are isolated neutral globules surrounded by a hot ionized medium. Most CG's known are located in the Gum nebula, a large HII region mostly stretching between the constellations of Vela and Puppis. CG13 is a large diffuse globule, with an opaque core surrounded by extended bright rims, and a rather inconspicuous tail. It is associated with a nebulous star, Bernes 136, which is a F star merely passing through the globule. Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (180m) L (190m) R (120m) G (60m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Cometary Globule CG1 & BE135 in Puppis

Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (270m) L (300m) R (110m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Sh2-54 (RCW 167) & NGC 6604

Sh2-54 is an extended bright nebula in the constellation of Serpens that belongs to an extended nebulosity that includes also the Eagle Nebula and the Omega Nebula. The older star population in this region has an average age of 4-5 millions years, and its components are grouped in the open cluster NGC 6604. Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (720m) L (210m) R (150m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

The Great Orion Nebula (M42)

The Great Nebula in Orion, an immense, nearby starbirth region, is probably the most famous of all astronomical nebulas. Here, glowing gas surrounds hot young stars at the edge of an immense interstellar molecular cloud only 1500 light-years away. In the above deep image, faint wisps and sheets of dust and gas are particularly evident. The Great Nebula in Orion can be found with the unaided eye just below and to the left of the easily identifiable belt of three stars in the popular constellation Orion. In addition to housing a bright open cluster of stars known as the Trapezium, the Orion Nebula contains many stellar nurseries. These nurseries contain hydrogen gas, hot young stars, proplyds, and stellar jets spewing material at high speeds. Also known as M42, the Orion Nebula spans about 40 light years and is located in the same spiral arm of our Galaxy as the Sun. The blue nebula above M42 is NGC1977, also named the running man nebula (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (300m) OIII(120m) L (270m) R (190m) G (180m) B (230m) - M43 & M42's core data courtesy of Angus Lau, taken with a TEC180 (180mm f/7.1, R:G:B = 2m:2m:2m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

GUM14 / RCW27 Nebula

Gum 14 is a large emission nebula complex that also includes the bright and prominent reflection nebula NGC 2626, which is illuminated by a 10th magnitude star. Gum 14 is ionized by the supergiant star HD 73882 and was first catalogued in 1955 by the Australian astronomer Colin Gum. Subsequently, it was also included in the RCW catalogue in 1960 and is therefore also known as RCW 27. With a size of approximately 2 degrees, this giant nebula is the largest of a prominent grouping of emission nebulae to the north of the Vela Supernova remnant. Along with Gum 14, this group is comprised of the smaller Gum 15 (RCW 32) and the almost equally large Gum 17 (RCW 33). Gum 14 is a fairly active site of star formation and has an extensive series of dark clouds and bright rimmed globules. Detailed observations and studies by professional astronomers have also uncovered a small collection of Herbig Haro objects (not visible at a widefield scale) and cometary reflection nebulae associated with young stellar objects. Also visible near the top edge is the small planetary nebula Hen 2-11, one of hundreds discovered by the famous astronomer Karl Henize in the 1960's (text provided by Sakib Rasool) Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (300m) L (270m) R (120m) G (120m) B (130m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

NGC 4372 and the Dark Doodad

The delightful Dark Doodad Nebula drifts through southern skies, a tantalizing target for binoculars in the constellation Musca, The Fly. The dusty cosmic cloud is seen against rich starfields just south of the prominent Coalsack Nebula and the Southern Cross. Stretching for about 3 degrees across this scene the Dark Doodad seems punctuated at its southern tip (lower left) by globular star cluster NGC 4372. Of course NGC 4372 roams the halo of our Milky Way Galaxy, a background object some 20,000 light-years away and only by chance along our line-of-sight to the Dark Doodad. The Dark Doodad's well defined silhouette belongs to the Musca molecular cloud, but its better known alliterative moniker was first coined by astro-imager and writer Dennis di Cicco in 1986 while observing comet Halley from the Australian outback. The Dark Doodad is around 700 light-years distant and over 30 light-years long (text adapted from APOD). Full resolution image shown at about 75% of original resolution. Apo TEC140 (140/f7.2) - FLI Proline 16803 - 2 panels mosaic, total L (440m) R (300m) G (300m) B (300m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Vela Supernova Remnant

The plane of our Milky Way Galaxy runs through this complex and beautiful skyscape. At the northwestern edge of the constellation Vela (the Sails) the telescopic frame is about 4 degrees wide, centered on the brightest glowing filaments of the Vela Supernova Remnant, an expanding debris cloud from the death explosion of a massive star. Light from the supernova explosion that created the Vela remnant reached Earth about 11,000 years ago. In addition to the shocked filaments of glowing gas, the cosmic catastrophe also left behind an incredibly dense, rotating stellar core, the Vela Pulsar. Some 800 light-years distant, the Vela remnant is likely embedded in a larger and older supernova remnant, the Gum Nebula (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - 4 panels mosaic, total Ha (1440m) OIII (1200m) R (480m) G (480m) B (360m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Supernova Remnant Puppis A

Driven by the explosion of a massive star, supernova remnant Puppis A is blasting into the surrounding interstellar medium about 7,000 light-years away. The expanding shock waves from that explosion are heating up the dust and gas clouds surrounding the supernova, causing them to glow and creating the beautiful red cirrus we see scattered around the center of the image. Much of the material from that original star was violently thrown out into space. However, some of the material remained in an incredibly dense object called a neutron star. This particular neutron star (too faint to be seen in this image) is moving inexplicably fast: over 3 million miles per hour! Astronomers are perplexed over its absurd speed, and have nicknamed the object, the “Cosmic Cannonball." Some of the teal-colored gas and dust in the image is from yet another ancient supernova, the Vela supernova remnant. That explosion happened around 12,000 years ago and was four times closer to us than Puppis A. If you had X-ray vision like the comic book hero Superman, both of these remnants would be among the largest and brightest objects you would see in the sky. On the top of the image the little bluish glare is vdBH15. (Text adapted from APOD and "Star explosion leaves behind a rose" ScienceDaily, 12 Dec. 2011, NASA/Jet Propulsion Laboratory) Many thanks to Sakib Rasool for suggesting me this interesting target. Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (540m) OIII (540m) L (180m) R (70m) G (80m) B (60m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Alnilam and Mintaka

Alnilam and Mintaka are the two bright bluish stars from east to west (left to right) in this cosmic vista. Otherwise known as the Belt of Orion (together with Alnitak), these blue supergiant stars are hotter and much more massive than the Sun. They lie about 1,500 light-years away, born of Orion's well-studied interstellar clouds. In fact, clouds of gas and dust adrift in this region have intriguing and some surprisingly familiar shapes, including the dark Horsehead Nebula and Flame Nebula near Alnitak. The famous Orion Nebula itself lies off the bottom of this star field that covers about 2x2 degrees on the sky (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (360m) L (230m) R (150m) G (130m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Great Rift around Mu Serpentis

Mu Serpentis (μ Serpentis) is a blue giant star in the head of constellation Serpens (Serpens Caput). Located about 160 light years away, Mu Serpentis shines at an apparent visual magnitude of 3.54. This area is a dense part of the Great Rift, a series of overlapping, molecular dust clouds that are located between the Solar System and the Sagittarius Arm of the Milky Way Galaxy. Apo TEC140 (140/f7.2) - FLI Proline 16803 - L (290m) R (80m) G (150m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Bernes 149 in Scorpius

Bernes 149 is an obscure nebula complex consisting of the reflection nebula GN 16.05.2 at the centre of an elongated dusty dark nebula. Although mostly unknown to amateurs, it has been well studied by professionals and is also known as the Lupus 3 cloud. The name comes from its connection with many other dark clouds in the constellation of Lupus. Near the centre of the image are the blazing bright stars HR 5999 and HR 6000. They belong to a class of YSO known as Herbig Ae/Be stars, which are intermediate mass pre-main sequence precursors to supergiant stars. The central reflection nebula is illuminated by HR 5999, the southern of the pair. Out of all the Lupus clouds, Lupus 3 exhibits the highest rate of star formation. Searches for young stellar objects have yielded the detection of more than a hundred x-ray sources in a 30 arcminute radius around HR 5999 and HR 6000. The Lupus 3 cloud also contains protostars with detected jets and outflows and Herbig Haro objects have been found near the central region (not visible in image). Near the bottom right corner is the small reflection nebula GN 16.01.6. The Lupus clouds are approximately 450-650 light years away (text and target suggestion by Sakib Rasool). Apo TEC140 (140/f7.2) - FLI Proline 16803 - L (300m) R (170m) G (120m) B (100m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

The Seagull Nebula (IC 2177)

A broad expanse of glowing gas and dust presents a bird-like visage to astronomers from planet Earth, suggesting its popular moniker - The Seagull Nebula. This portrait of the cosmic bird covers a 2 degree wide swath across the plane of the Milky Way, near the direction of Sirius, alpha star of the constellation Canis Major. Of course, the region includes objects with other catalog designations: notably NGC 2327, a compact, dusty emission region with an embedded massive star that forms the bird's head (aka the Parrot Nebula, right center). IC 2177 forms the sweeping arc of the seagull's wings. Dominated by the reddish glow of atomic hydrogen, the complex of gas and dust clouds with bright young stars spans over 100 light-years at an estimated 3,800 light-year distance (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (330m) OIII (300m) L (250m) R (160m) G (120m) B (60m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Tarantula Nebula (NGC2070) with labels

Tarantula Nebula (NGC2070) with labels reporting the main objects visible in the area

Tarantula Nebula (NGC2070) in LMC

The 16th century Portuguese navigator Ferdinand Magellan and his crew had plenty of time to study the southern sky during the first circumnavigation of planet Earth. As a result, two fuzzy cloud-like objects easily visible to southern hemisphere skygazers are known as the Clouds of Magellan, now understood to be satellite galaxies of our much larger, spiral Milky Way galaxy. About 160,000 light-years distant in the constellation Dorado, the Large Magellanic Cloud (LMC) is seen here in a remarkably deep, colorful composite image, starlight from the central bluish bar contrasting with the telltale reddish glow of ionized atomic hydrogen gas. Spanning about 15,000 light-years or so, it is the most massive of the Milky Way's satellite galaxies and is the home of the closest supernova in modern times, SN 1987A. The prominent patch at top left is 30 Doradus, also known as the magnificent Tarantula Nebula. The giant star-forming region is about 1,000 light-years across and is the largest and most complex star forming region in the entire galactic neighborhood. Were it placed at the distance of Milky Way's Orion Nebula, only 1,500 light-years distant and the nearest stellar nursery to Earth, it would appear to cover about 30 degrees (60 full moons) on the sky. Intriguing details of the nebula are visible in the above image shown in composite narrowband and RGB "true colors". The spindly arms of the Tarantula nebula surround NGC 2070, a star cluster that contains some of the brightest, most massive stars known, visible in blue in the image center. Since massive stars live fast and die young, it is not so surprising that the cosmic Tarantula also lies near the site of a close recent supernova (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (300m) OIII (300m) L (180m) R (120m) G (120m) B (150m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Cometary Globule CG12 (NGC 5367)

Cometary Globule 12 is a high latitude low mass star forming region associated with the young cluster and reflection nebula NGC 5367. While the cluster and associated nebula were discovered by John Herschel in 1834, the cometary globule was discovered only in 1976 on an ESO/SRC Sky Survey plate taken with the UK Schmidt telescope. It is estimated to be about 600 pc away, toward the constellation of Centaurus. Cometary globules are known stellar bithplaces that show a head–tail morphology similar to comets. Their heads are dusty, compact and bright-rimmed. A faintly luminous tail extending from the head generally points away from a nearby bright early-type star. CG12 is not only unusual because its isolated location far from the galactic plane, but Chandra also discovered more than 50 new young stars in CG12 with their age and stellar distributions inconsistent with the simple radiation driven implosion model that is believed to be a major triggering process of star formation in many cometary clouds. Apo TEC140 (140/f7.2) - FLI Proline 16803 - L (300m) R (130m) G (130m) B (130m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

LDN 1622: "The Boogie Man" Dark Nebula in Orion

The silhouette of an intriguing dark nebula inhabits this cosmic scene. Lynds' Dark Nebula (LDN) 1622 appears against a faint background of glowing hydrogen gas only easily seen in long telescopic exposures of the region. LDN 1622 lies near the plane of our Milky Way Galaxy, close on the sky to Barnard's Loop - a large cloud surrounding the rich complex of emission nebulae found in the Belt and Sword of Orion. But the obscuring dust of LDN 1622 is thought to be much closer than Orion's more famous nebulae, perhaps only 500 light-years away. At that distance, this 2 degrees wide field of view would span less than 20 light-years. (Text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (330m) L (240m) R (120m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

The Horsehead and Alnitak region

The Horsehead Nebula is one of the most famous nebulae on the sky. It is visible as the dark indentation to the red emission nebula seen above and to the right of center in the above photograph. The Horsehead is some 1,500 light-years distant, embedded in the vast Orion cloud complex. About five light-years "tall", the dark cloud is cataloged as Barnard 33 and is visible only because its obscuring dust is silhouetted against the glowing red emission nebula IC 434. Contrasting blue reflection nebula NGC 2023 is visible on the lower left. In this color image, both Horsehead and NGC 2023 seem to be caught in beams of light shining from above -- but the beams are actually just internal reflections from bright star Sigma Orionis, just off the upper edge of the view. The bright star on the left is located in the belt of the familiar constellation of Orion. The horse-head feature is dark because it is really an opaque dust cloud which lies in front of the bright red emission nebula. Like clouds in Earth's atmosphere, this cosmic cloud has assumed a recognizable shape by chance. After many thousands of years, the internal motions of the cloud will alter its appearance. The emission nebula's red color is caused by electrons recombining with protons to form hydrogen atoms. Also visible in the picture are blue reflection nebulae, which preferentially reflect the blue light from nearby stars. (Text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (270m) L (200m) R (120m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

The Helix Nebula (NGC 7293)

A mere seven hundred light years from Earth, in the constellation Aquarius, a sun-like star is dying. Its last few thousand years have produced the Helix Nebula (NGC 7293), a well studied and nearby example of a Planetary Nebula, typical of this final phase of stellar evolution. A total of 16.5 hours of exposure time have gone in to creating this deep view of the nebula. It shows details of the Helix's brighter inner region, about 3 light-years across, but also follows fainter outer halo features that give the nebula a span of well over six light-years. The white dot at the Helix's center is this Planetary Nebula's hot, central star. A simple looking nebula at first glance, the Helix is now understood to have a surprisingly complex geometry (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (630m) OIII (600m 5nm + 240m 3nm) L (270m) R (80m) G (190m) B (170m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

M78 and Reflecting Dust Clouds in Orion

Interstellar dust clouds and bright nebulae abound in the fertile constellation of Orion. One of the brightest, M78, is just left of center in this colorful telescopic view, covering an area north of Orion's belt. At a distance of about 1,500 light-years, the bluish nebula itself is about 5 light-years across. Its blue tint is due to dust preferentially reflecting the blue light of hot, young stars in the region. Dark dust lanes and other nebulae can easily be traced through this gorgeous skyscape. The scene also includes the remarkable McNeil's Nebula -- a newly recognized nebula associated with the formation of a sun-like star, and the telltale reddish glow of many Herbig- Haro objects, energetic jets from stars in the process of formation (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (420m) L (220m) R (220m) G (150m) B (280m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

At the feet of Orion (NGC1999) Full Frame

South of the large star-forming region known as the Orion Nebula, lies bright blue reflection nebula NGC 1999. The nebula is marked with a dark inverted T-shape at the lower left in a broad cosmic vista that spans over 10 light-years. The dark shape is a dense gas and dust cloud, or Bok globule, seen in silhouette against the bright nebula, and likely a site of future star formation. At the edge of the Orion molecular cloud complex some 1,500 light-years distant, NGC 1999's illumination is provided by the embedded variable star V380 Orionis. The region abounds with energetic young stars producing jets and outflows that create luminous shock waves, including HH (Herbig-Haro) 1 and 2 just below and left of NGC 1999, and the apparent cascade of reddish arcs and bow shocks beginning at the upper right. The stellar jets and outflows push through the surrounding material at speeds of hundreds of kilometers per second (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (330m) L (360m) R (120m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Ring of Ice and Fire in SMC

At the "feet" of the SMC, east of the nebular group know as the "magnificent seven" is this amazing area rich of HII and O3 emissions. NGC456, NGC460 and NGC465 is the array of bright emission nebulae at right in the image above. The assortment of irregular shapes appear to be cut through with dark lanes, while the individual nebulae have a large brightness range amongst them. On the middle-left of the image is visible the blue spot of (Henize) N-89, than at its left lays NGC 602 (a young, bright open cluster) and the very faint but large ring of N-90. Radiation and shock waves from the stars have pushed away much of the lighter surrounding gas and dust that compose N90, and this in turn has triggered new star formation in the ridges (or "elephant trunks") of the nebula. Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (360m) OIII(450m) L (180m) R (120m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Gas and stars of a nearby galaxy

NGC 292, or the Small Magellanic Cloud (SMC) is the smaller of the two ‘Nubeculas’ first sighted by Ferdinand Magellan during his circumnavigation around the globe at the beginning of the sixteenth century. At a distance of "merely" 210,000 light-years away in the constellation Tucana, the SMC is tidally distorted by both the LMC and our own Milky Way. It actually spans 15,000 light-years or so and contains several hundred million stars. Despite being often overlooked due to the smaller size and brightness compared to the Large Magellanic cloud, the SMC is very rich of objects to see. The large blue patch in the top right of the image is clusters and nebulae NGC 346, a a star forming region about 200 light-years across, as big as the Eta Carinae Nebula. Exploring NGC 346, astronomers have identified a population of embryonic stars strung along the dark, intersecting dust lanes visible here on the right. Still collapsing within their natal clouds, the stellar infants' light is reddened by the intervening dust. Under this giant nebula, close the center of the image lay Henize N36 and N37, a pair of emission nebulae fairly bright. Al bottom left in the picture above there is a group of objects known as "the Magnificent Seven", in fact NGC 249–261–267, Dem 132 and N 25–28–30. Apo TEC140 (140/f7.2) - FLI Proline 16803 - - Mosaic of two panels - Ha (750m) OIII(840m) L (410m) R (240m) G (270m) B (280m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Ancient Supernova SN185 (RCW86)

In 185 AD, Chinese astronomers recorded the appearance of a new star in the Nanmen asterism - a part of the sky identified with Alpha and Beta Centauri on modern star charts. The new star was visible for months and is thought to be the earliest recorded supernova. The gaseous shell RCW 86 is probably the supernova remnant of this event and has a relatively large angular size of roughly 45 arc minutes (larger than the apparent size of the full moon). The distance to RCW 86 is estimated to be 9,100 light-years. Recent X-ray studies show a good match for the expected age. New infrared observations from NASA's Spitzer Space Telescope and Wide-field Infrared Survey Explorer (WISE) reveal how the supernova occurred and how its shattered remains ultimately spread out to great distances. The findings show that the stellar explosion took place in a hollowed-out cavity, allowing material expelled by the star to travel much faster and farther than it would have otherwise (text adapted from Wikipedia). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (1020m) OIII (490m) R (90m) G (90m) B (90m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Inside the Small Magellanic Cloud

NGC 292, or the Small Magellanic Cloud (SMC) is the smaller of the two ‘Nubeculas’ first sighted by Ferdinand Magellan during his circumnavigation around the globe at the beginning of the sixteenth century. At a distance of "merely" 210,000 light-years away in the constellation Tucana, the SMC is tidally distorted by both the LMC and our own Milky Way. It actually spans 15,000 light-years or so and contains several hundred million stars. Despite being often overlooked due to the smaller size and brightness compared to the Large Magellanic cloud, the SMC is very rich of objects to see. The large blue patch in the top centre of the image is clusters and nebulae NGC 346, a a star forming region about 200 light-years across, as big as the Eta Carinae Nebula. Exploring NGC 346, astronomers have identified a population of embryonic stars strung along the dark, intersecting dust lanes visible here on the right. Still collapsing within their natal clouds, the stellar infants' light is reddened by the intervening dust. Under this giant nebula, close the center of the image lay Henize N36 and N37, a pair of emission nebulae fairly bright. Lower right in the picture above there is a group of objects known as "the Magnificent Seven", in fact NGC 249–261–267, Dem 132 and N 25–28–30. Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (390m) OIII(390m) L (230m) R (120m) G (150m) B (160m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Octans dust and molecular cloud

Octans is an inconspicuous constellation introduced by Nicolas Louis de Lacaille. Its name is Latin for the eighth part of a circle, but it is named after the octant, a navigational instrument. Octans is notable as the location of the south celestial pole but, unlike the north pole, it has no bright pole star. This constellation is circumpolar to the south celestial pole, so it can be seen in Southern Hemisphere skies during the evening in any month of the year. Octans does not contain many deep sky objects but contain a vast complex of dust and molecular clouds, of which a small part is imaged here. The blue reflection nebula close to the center of the image is cataloged as GN 19.41.5 and is merely 4' across. Apo TEC140 (140/f7.2) - FLI Proline 16803 - L (270m) R (120m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

The huge halo of NGC3242

NGC 3242, commonly known as the Ghost of Jupiter, is a planetary nebula located in the constellation Hydra. William Herschel discovered the nebula that later was catalogued by Dreyer as NGC 3242. After a star like our Sun completes fusion in its core, it throws off its outer layers it a striking display called a planetary nebula. NGC 3242 is such a planetary nebula, with the stellar remnant white dwarf star visible at the center. While the planetary nebula's core measure only about 16" x 26" in diameter, NGC 3242 is surrounded by a first fainter shell and by another very faint giant halo measuring almost half degree in diameter, same as the full Moon, with a prominent arc containing both strong emissions of Ha and OIII. This huge halo was first discovered on the Palomar DSS plates and later confirmed to be related to the planetary nebula itself. Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (510m) OIII (540m) R (90m) G (90m) B (110m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

IC4633 and APUS IFN

Apus, the Bird of Paradise, is a very small southern constellation with no spectacular deep sky objects. The most significat patch of sky here is this one around IC4633, a faint galaxy surrounded by a very faint Integrated Flux Nebula. IFN is a gauze of gas and dust that glows by reflecting all the collective light of the Milky Way. Its material is so thin that light from external galaxies shine through it. IC 4633 (at centre top) is conspicuous on the edge of the emission glow while just below lies the bright sliver of a distant edge-on spiral or lenticular system, IC4635. Apo TEC140 (140/f7.2) - FLI Proline 16803 - L (300m) R (90m) G (90m) B (90m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

The Lupus I molecular cloud

The Lupus clouds compose one of the main low-mass star forming complexes within 200 pc of the Sun. They contain four main star forming sites, including B228 in Barnard’s catalogue pictured above, more frequently referred to as Lupus 1 in modern literature. It is likely that the Sun formed in a similar star formation region more than four billion years ago. B228 is sometime named the Dark Wolf nebula. Apo TEC140 (140/f7.2) - FLI Proline 16803 - L (340m) R (120m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

A wispy wave in Vela SNR

The Vela Supernova Remnant is one of the best examples of the aftermath of a supernova explosion: the violent death of a star many times more massive than the sun which took place over 10,000 years ago. Pictured above a delicate wisp in the suthern part of the remnant. Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (180m) OIII (270m) R (90m) G (90m) B (90m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Sharpless SH2-308

Blown by fast winds from a hot, massive star, this cosmic bubble is huge. Cataloged as Sharpless 308 it lies some 5,200 light-years away in the constellation Canis Major and covers over 2/3 degree on the sky (compared with 1/2 degree for the Full Moon). That corresponds to a diameter of 60 light-years at its estimated distance. The massive star itself, a Wolf-Rayet star, is the bright blue one near the center of the nebula. Wolf-Rayet stars have over 20 times the mass of the Sun and are thought to be in a brief, pre-supernova phase of massive star evolution. Fast winds from this Wolf-Rayet star create the bubble-shaped nebula as they sweep up slower moving material from an earlier phase of evolution. The windblown nebula has an age of about 70,000 years. Relatively faint emission captured in the expansive image is dominated by the glow of ionized oxygen atoms mapped to bluish hues (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (210m) OIII (450m) R (130m) G (90m) B (130m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Sharpless 63

This is the high latitude molecular cloud MBM 159, which is located at a distance of about 220 pc and may form part of the Aquila rift. Apo TEC140 (140/f7.2) - FLI Proline 16803 - L (450m) R (90m) G (90m) B (150m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

M16 and the Eagle Nebula

Young star cluster M16 is surrounded by natal clouds of cosmic dust and glowing gas also known as The Eagle Nebula. This image of the region includes fantastic shapes made famous in well-known Hubble Space Telescope close-ups of the starforming complex. Described as elephant trunks or Pillars of Creation, dense, dusty columns rising near the center are light-years in length but are gravitationally contracting to form stars. Energetic radiation from the cluster stars erodes material near the tips, eventually exposing the embedded new stars. Extending from the upper left edge of the nebula is another dusty starforming column known as the Fairy of Eagle Nebula. M16 and the Eagle Nebula lie about 7,000 light-years away, an easy target for binoculars or small telescopes in a nebula rich part of the sky toward the split constellation Serpens Cauda (the tail of the snake) (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (310m) OIII (590m) R (300m) G (240m) B (310m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

IC 4628: The Prawn Nebula

South of Antares, in the tail of the nebula-rich constellation Scorpius, lies emission nebula IC 4628. Nearby hot, massive stars, millions of years young, radiate the nebula with invisible ultraviolet light, stripping electrons from atoms. The electrons eventually recombine with the atoms to produce the visible nebular glow. At an estimated distance of 6,000 light-years, the region shown is about 250 light-years across. The nebula is also cataloged as Gum 56 for Australian astronomer Colin Stanley Gum, but seafood-loving astronomers might know this cosmic cloud as The Prawn Nebula (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (315m) R (210m) G (160m) B (170m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Lobster Nebula NGC 6357

For reasons unknown, NGC 6357 is forming some of the most massive stars ever discovered. Near the more obvious Cat's Paw nebula, NGC 6357 houses the open star cluster Pismis 24, home to these tremendously bright and blue stars. The overall red glow near the inner star forming region results from the emission of ionized hydrogen gas. The surrounding nebula, shown above, holds a complex tapestry of gas, dark dust, stars still forming, and newly born stars. The intricate patterns are caused by complex interactions between interstellar winds, radiation pressures, magnetic fields, and gravity. NGC 6357 spans about 400 light years and lies about 8,000 light years away toward the constellation of the Scorpion (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (410m) OIII (415m) R (120m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Stars and Dust Across Corona Australis

Cosmic dust clouds sprawl across a rich field of stars in this sweeping telescopic vista near the northern boundary of Corona Australis, the Southern Crown. Probably less than 500 light-years away and effectively blocking light from more distant, background stars in the Milky Way, the densest part of the dust cloud is about 8 light-years long. At its tip (upper right) is a group of lovely reflection nebulae cataloged as NGC 6726, 6727, 6729, and IC 4812. A characteristic blue color is produced as light from hot stars is reflected by the cosmic dust. The smaller yellowish nebula (NGC 6729) surrounds young variable star R Coronae Australis. Magnificent globular star cluster NGC 6723 is toward the upper right corner of the view. While NGC 6723 appears to be part of the group, it actually lies nearly 30,000 light-years away, far beyond the Corona Australis dust clouds (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - L (530m) R (150m) G (150m) B (150m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

The Cat's Paw Nebula NGC 6334

Nebulae are perhaps as famous for being identified with familiar shapes as cats are for getting into trouble. Still, no known cat could have created the vast Cat's Paw Nebula visible in Scorpius. At 5,500 light years distant, Cat's Paw is an emission nebula with a red color that originates from an abundance of ionized hydrogen atoms. Alternatively known as the Bear Claw Nebula or NGC 6334, stars nearly ten times the mass of our Sun have been born there in only the past few million years (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (310m) OIII (300m) R (180m) G (180m) B (180m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Circinus Star Forming Complex

Like black ink spilt on a galactic beach, the twisting filamentary tendrils of the dark nebula Sandqvist 169 snake across a glittering field of bright Milky Way stars in the constellation of Circinus. It forms the western part of the giant Circinus Cloud complex, which measures a whopping 2x5 degrees in total! The series of filaments that seemingly emanate outwards from the dense central part of Sandqvist 169 (also known as Circinus-W) are indicative of past violent activity. The filamentary appearance of the cloud is likely to be the result of multiple outflows from young stars, whose formation might have been triggered by a supernova that exploded in close proximity to the cloud. If star formation has ensued for a few hundred thousand years, then the cloud has produced many dozens of young stars, whose outflows have torn the cloud apart. The filaments and cavities provide a fossil record of past star formation as they trace the boundaries of the outflows. Optically visible signs of star formation in Sandqvist 169 include the tiny cometary reflection nebulae vdBH65a and vdBH65b. vdBH65a is a small nebulous patch that is near a bright yellow star that is situated towards the north of the central portion of the cloud. Its illuminating star drives a bipolar molecular outflow that includes the optical bowshock HH 139 (which cannot be seen at a widefield scale). vdBH65b is a small fan shaped cometary reflection nebula that can be seen embedded in the filaments to the right of the cloud core (which are catalogued as Sandqvist 171). It is also the source of numerous Herbig Haro outflows and objects, which are not visible at this scale. Despite its size and apparent interesting past history, the Circinus Cloud has been the subject of very few detailed studies but future investigation and observations will help unravel more of its mysteries. Since it has only received one major study since its discovery, its distance is extremely uncertain and is estimated to be 2275 light years. However, a study in 2011 with observations from the Widefield Infrared Survey Explorer (WISE) telescope uncovered an embedded infrared cluster of YSO's. The Sandqvist catalogue is a collection of 95 southern dark clouds that was published in 1977 by the Swedish astronomer Aage Sandqvist. Confusingly the numbering of the catalogue starts from the number 101 to avoid mix-up with the SL catalogue, which was published by Aage Sandqvist and K.P. Lindroos in the previous year (description provided by Sakib Rasool) Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (690m) L (520m) R (120m) G (120m) B (120m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

The Chamaeleon I Cloud

Home to some of the nearest molecular clouds, the constellation of Chamaeleon is filled with many dark nebula complexes. The Chamaeleon I complex is one of three large clouds found in this southern constellation and has an age of 2 million years. The distances of the three main clouds range from 520-580 light years and are also isolated from other major star forming complexes. The Chamaeleon I complex is a site of low mass star formation, which is characterised visually by various reflection nebulae including IC 2631 to the north and the blue nebula Ced 111 and the white reflection nebula Ced 110 to the south. The great obscuring mass of thick brown dust in the region absorbs the blue light of distant stars making them appear much redder than they actually are. This process of interstellar reddening also affects the light of distant galaxies in the line of sight, making them look less blue. Despite the copious amounts of dust, the Chamaeleon I complex is regarded by astronomers to impose only a moderate level of extinction on the background starfield in comparison with other dark nebulae. The Chamaeleon I complex is near the south celestial pole and is situated at the edge of the Scorpius-Centaurus OB association. The cloud is illuminated by massive stars that belong to a subgroup of this OB association. Due to its proximity, the Chamaeleon I complex has been subjected to many searches for young stellar objects by many astronomers including Karl Henize in 1963. Recent surveys in the past two decades have also yielded a large sample of YSO's, including the first X-ray emitting brown dwarf, which was discovered in 1998. Young stellar objects have also been discovered in various infrared surveys of the clouds. The cluster of sources associated with the complex is split into two northern and southern subclusters and the cloud contains 200 known low mass YSO's. Analysis of data predicts that star formation began 3-4 million years ago in the northern half of the cloud and 5-6 million years ago in the southern half. Star formation in the cloud is still ensuing at a declining rate until eventually it will completely cease. Other optically visible signs of star formation in the cloud are represented by small Herbig Haro objects and outflows. The first Herbig Haro objects to be discovered in this complex were found in a survey for Herbig Haro objects in dark clouds by Richard Schwartz in 1977. They include HH 48-9 and HH 50. Due to its tiny size, HH 48 isn't visible in this widefield image but the bright Herbig Haro objects HH 49 and HH 50 are prominently visible in the region between Ced 110 and Ced 111. HH 49/50 are associated with the largest outflow in this complex, a giant outflow with a length of 27 arcminutes (or 6.5 light years) and its source is the protostar Cha-MMS1. Spitzer infrared images of HH 49/50 reveal infrared emission associated with them. This infrared nebula has an incredible shape of a "tornado" formed by a pair of twisting helical filaments. Deep imaging surveys in the past decade have found a total of 30 Herbig Haro objects associated with 20 separate outflows. Also visible in the image is a unique curiosity, a colourful orange nebula below the reflection nebula Ced 111. This is the Chamaeleon Infrared Nebula, a bipolar infrared reflection nebula that also happens to be visible optically. Its bipolar nature is only visible in infrared images as well as its illuminating source. Studies of the nebula have shown it to exhibit a complex geometry consisting of a disk surrounding the central source as well as bipolar lobes tracing two cavities cleared out by ouflow activity. Infrared images reveal the two bipolar lobes to be separated by a dark structure, which is a circumstellar disk around the central source (description provided by Sakib Rasool) Apo TEC140 (140/f7.2) - FLI Proline 16803 - L (580m) R (90m) G (90m) B (90m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

The Eta Carinae Nebula (NGC 3372)

A jewel of the southern sky, the Great Carina Nebula, also known as NGC 3372, spans over 300 light-years, one of our galaxy's largest star forming regions. Like the smaller, more northerly Great Orion Nebula, the Carina Nebula is easily visible to the unaided eye, though at a distance of 7,500 light-years it is some 5 times farther away. This gorgeous telescopic portrait reveals remarkable details of the region's glowing filaments of interstellar gas and obscuring cosmic dust clouds. Wider than the Full Moon in angular size, the field of view stretches nearly 100 light-years across the nebula. The Carina Nebula is home to young, extremely massive stars, including the still enigmatic variable Eta Carinae, a star with well over 100 times the mass of the Sun. Eta Carinae is the brightest star at the left, near the dusty Keyhole Nebula. While Eta Carinae itself maybe on the verge of a supernova explosion, X-ray images indicate that the Great Carina Nebula has been a veritable supernova factory (text adapted from APOD). Apo TEC140 (140/f7.2) - FLI Proline 16803 (4 panels mosaic) - Ha (850m) OIII (1110m) R (290m) G (290m) B (350m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia

Henize2-111 and Alpha Centauri

Blazing brightly in the southern sky, the supergiant binary Alpha Centauri is the host of an expansive starscape sprinkled with numerous deep sky objects in this telescopic view. The most visually striking of its retinue of glittering jewels is the exotic and unique planetary nebula Hen 2-111, which is one of 468 planetary nebulae that were catalogued by Karl Henize in 1967. The main central part of Hen 2-111 is a bright peanut shaped core that measures only 29 x 15 arcseconds. However, its most visually striking aspect is a faint giant ionized halo that spans 10 x 5 arcminutes! This extreme structure was discovered by B. Louise Webster in 1978 in deep photographic plates taken with the (at the time) Anglo-Australian Observatory. At an estimated distance of 7800 light years, the entire nebula spans approximately 23 light years! The halo is actually a rare bipolar outflow and the other notable planetary nebula known to exhibit this unique feature is the northern hemisphere nebula KjPn 8 in Cassiopeia. Hen 2-111 exhibits some of the highest radial velocities detected in a planetary nebula to date! The radial velocities of the outer lobes are 370 kms, which is indicative of the high speed of the material ejected. Bipolar outflows with even greater velocities have been observed in a few other planetary nebulae. Almost perfectly symmetrical, the geometric regularity of the outflow is due to the ionized gas flowing outwards along the walls of two bi-conical structures. The twisted appearance is caused by the axis of the structures being viewed at an angle of 45 degrees from our line of sight. The most likely explanation for the origin of the outer lobes is an eruptive event of the central star within a circumstellar disk. To the right of Hen 2-111 is the attractive pairing of the open clusters NGC 5617 and Pismis 19. NGC 5617 is the larger and younger of the two and despite its apparent youthful appearance, it is actually an intermediate age cluster with an estimated age of 80 million years. Contrastingly, the smaller rich condensed cluster Pismis 19 appears much older than NGC 5617 and indeed its golden ancient light betrays its great age of 800 million years! It is at a similar distance to Hen 2-111 of about 7800 light years whereas NGC 5617 is much nearer at 5000 light years. However, it is subject to severe reddening due to interstellar dust between us and the cluster and would shine more brightly if this dust was less prevalent. Pismis 19 is one of 24 open clusters that were discovered by Paris Pismis in 1959 by analysing photographic plates taken at the Tonantzintla Observatory. Also barely visible in the glare of Alpha Centauri is a round broken roughly circular shell, which can be seen to the north of the halfway point between Alpha Centauri and Hen 2-111. This is the supernova remnant G315.4-0.3, which was discovered by Anne Green in 1974 and identified as a supernova remnant in 1975. However, its extremely dim optical shell was discovered recently in 2011 in a search for new supernova remnants in SuperCOSMOS Ha Survey (SHS) images by Milorad Stupar and Quentin Parker. Thanks to Sakib Rasool for suggesting me this little known object and for preparing the above object description. Apo TEC140 (140/f7.2) - FLI Proline 16803 - Ha (720m) OIII (660m) R (160m) G (120m) B (180m) - Warrumbungle Observatory, Coonabarabran, NSW, Australia