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NGC 6302 is a bipolar planetary nebula in the constellation Scorpius. It is also known the Bug Nebula, Butterfly Nebula, or Caldwell 69.
NGC 6302 resembles a butterfly with its wings outstretched. It is perhaps one of the most complex ever observed planetary nebulae. It has many dramatic areas, some containing roiling cauldrons of superheated gas along the areas resembling wings too thick dust concealing its heart. Superheated gas is moving through space at more than 950 000 kilometres per hour. At that speed, you could travel from the Earth to the Moon in around 24 minutes! Incredible.
The central star is one of the hottest stars known, with a surface temperature in excess of 250,000 degrees Celsius. This suggests that the star must have been enormous.
These cosmic trainwrecks always seem to leave the most beautiful structures in their wake. I created this image using cooled CCD monochromatic astronomical cameras with seven filters. A luminance filter captured most of the detail, followed by red, green, and blue filters to fill cre ate a traditional colour image. I then used SII, Ha, and OIII narrowband for a bit of extra structure and additional hues to balance the shot while trying to retain a traditional RGB colour image.
Instruments:
Telescope: 10" Ritchey-Chrétien RCOS
Camera: SBIG STL-11000 Mono
Mount: Astro-Physics AP-900
Focal Length: 2310.00 mm
Pixel size: 9.00 um
Resolution: 0.82 arcsec/pix
Exposure Details:
Red 18X600
Green 12X600
Blue 19X600
Lum 59X600
Ha 29X1200
SII 15X1200
OIII 28X1200
Total Exposure: 42 Hours
Thanks for looking
NGC6302, know as the Bug Nebula or the Butterfly Nebula is a bipolar planetary nebula in the constellation of Scorpius. The structure in the nebula is among the most complex ever observed in planetary nebulae and its central star is also one of the hottest stars known (Surface temperature is in excess of 250,000 degrees Celsius). It is approximately 3392 light years from earth.
This was a very quick imaging session before the clouds rolled in, and so is only 2 hours of narrowband subs. 1 hour of Hydrogen A (Ha) and 1 hour of Oxygen 3(Oiii), but processed using the H-O-O palette giving 3 hours..As this object is very small in our 6 inch RC telescope it is difficult to extract a lot of detail, but I am very happy how it turned out, and the ASIair made the whole process of setup and capturing very quick and easy.
Equipment Details:
•6 Inch GSO Ritchey-Chretien (RC) F9 1370mm Focal length
•Skywatcher NEQ6 Mount
•ZWO ASI1600mm Cmos Camera cooled to -10'c
•ZWO EFW7 Filter Wheel
•Baader 36mm unmounted Ha, Oiii
•Orion ST80 80mm Guide Scope
•ZWO ASI120mm mini Guide Camera
•ZWO ASIAIR Pro for full automation
Exposure Details:
•Ha 20X180 seconds - Bin 1x1 (Red)
•Oiii 20X180 seconds - Bin 1x1 (Green)
•Oiii 20X180 seconds - Bin 1x1 (Blue)
Total Integration Time: 2 hours
Planetary Nebula
NGC 6302, Caldwell 69
-------------------------------
Exposure: 45 minutes
Field of View:17.5 x 11.6 arcmin
Image date: 2021-06-17
-------------------------------
Magnitude: +9.7
Distance: 4,000 light years
Apparent size: 1.4 arc min
-------------------------------
Telescope: SkyWatcher Esprit 120
Camera: ZWO ASI 290
This rich and dense smattering of stars is a massive globular cluster, a gravitationally-bound collection of stars that orbits the Milky Way. Globular clusters are denser and more spherical than open star clusters like the famous Pleiades. They typically contain hundreds of thousands of stars that are thought to have formed at roughly the same time.
Studies have shown that this globular cluster, named NGC 6139, is home to an aging population of stars. Most globular clusters orbiting the Milky Way are estimated to be over 10 billion years old; as a result they contain some of the oldest stars in our galaxy, formed very early in the galaxy’s history. However, their role in galactic evolution is still a matter of study.
This cluster is seen roughly in the direction of the centre of the Milky Way, in the constellation of Scorpius (The Scorpion). This constellation is a goldmine of fascinating astronomical objects. Hubble has set its sights on Scorpius many times to observe objects such as the butterfly-like Bug Nebula, surprising binary star systems, and other dazzling globular clusters.
Credits: ESA/Hubble & NASA, CC BY 4.0
The Bug Nebula (NGC 6302), in the constellation Scorpius, is a bipolar planetary nebula. It has been discovered in 1888. The earliest-known study of this nebula is by Edward Emerson Barnard who drew and described it in 1907.
NGC 6302 lies about 3,400 light-years away. Its spectrum shows that its central star is exceptionally hot (one of the hottest known stars in our galaxy), with an estimated surface temperature of almost 250,000 °C. This star that was once roughly five times the mass of the Sun, shines brightly in ultraviolet light but it is hidden from direct view by dense equatorial torus of dust.
NGC 6302 has a complex structure and contains a prominent northwest lobe which extends up to 3.0′ away from the central star. This lobe is estimated to have formed from an eruptive event 1,900 years ago.
The dark line that runs through the center of the nebula has been shown to have an unusual composition, showing evidence for crystalline silicates, crystalline water ice and quartz.
Narrowband (HOO) version: H-Alpha mapped to red, OIII mapped to blue and OIII+Ha mapped to the green channel. While the colors in this image are not the true colors, the narrowband filters were used to create the nebula color. Then I added the natural star colors using RGB filters and Starnet process.
RA 17h 13m 44.1s
DEC -37° 06' 17.9"
ORIENTATION Up is 148 degrees E of N
CONSTELLATION Scorpius
DISTANCE 3,400 ly
MAGNITUDE 10.1
Captured September 2021
Fiel Of view: 9 x 8.17 arcmin
Total integration time of 16.5 hours.
Technical Details
Data acquisition: Martin PUGH
Processing: Nicolas ROLLAND
El Sauce Observatory, Rio Hurtado, Chile
R 3 x 600 sec
G 3 x 600 sec
B 4 x 600 sec
Ha 14 x 1800 sec
OIII 15 x 1800 sec
Optics: Planewave 17“ CDK @ F6.8
Mount: Paramount ME
CCD: SBIG STXL-11002 (AOX)
NGC 6302 - the Bug Nebula or Butterfly Nebula, is a bipolar planetary nebula in the constellation Scorpius. The structure in the nebula is among the most complex ever observed in planetary nebulae and its central star is one of the hottest in the galaxy, with a surface temperature > 200,000 K, implying that the star from which it formed must have been very large. Its small angular size (about 80 x 45 arc secs) is evidenced by the fact that this image was taken with a Planewave 20" (0.51m) CDK Astrograph, fl 2280mm (0.66 Focal Reducer Fitted) f/4.5
FLI-PL6303E CCD camera
8x 3mins Luminance
RGB each 2 minutes
This is the rich region in the Milky Way in the tail of Scorpius. It is replete with many nebulas, both bright emission and dark dust clouds.
At lower right is the False Comet area, as it looks comet-like to the naked eye. It is made of the small bright star cluster NGC 6231, along with the larger cluster Collinder 316, and the magenta emission nebula IC 4628. At top is the nebula NGC 6357 and below it NGC 6334, aka the Cat's Paw Nebula. The very tiny (on this scale) red Bug Nebula, NGC 6302, is at centre.
The pair of stars at left are Shaula and Lesath which make up the "Stingers" of the Scorpion tail. The tight double at right is made of Mu1 and Mu2 Scorpii.
This is a stack of 10 x 2 minute exposures with the Canon RF135mm lens at f/2 on the Canon Ra at ISO 800. It was on the Astro-Physics AP400 mount. The lens had an 82mm URTH Night broadband filter on it. Taken on the morning of March 14, 2024 from the Warrumbungles Mountain Motel near Coonabarabran, NSW, Australia during the OzSky star party.
Release Date: May 3, 2004
A Dying Star Shrouded by a Blanket of Hailstones Forms the Bug Nebula (NGC 6302)
The Bug Nebula, NGC 6302, is one of the brightest and most extreme planetary nebulae known. The fiery, dying star at its center is shrouded by a blanket of icy hailstones. This NASA Hubble Wide Field Plantery Camera 2 image shows impressive walls of compressed gas, laced with trailing strands and bubbling outflows.
Object Names: NGC 6302, Bug Nebula
Image Type: Astronomical
Credit: NASA, ESA and A.Zijlstra (UMIST, Manchester, UK)
To learn more about this image go to:
hubblesite.org/gallery/album/nebula/pr2004046a/
NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission.
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This structure may look like a cosmic butterfly unfurling its celestial wings, but there’s nothing gentle or delicate about this massive blowout. In Caldwell 69, also cataloged as NGC 6302 and commonly known as the Butterfly or Bug Nebula, layers of gas are being ejected from a Sun-like star that has exhausted its nuclear fuel. Medium-mass stars grow unstable as they run out of fuel, which leads to the dramatic expulsion of material into space at speeds of over a million miles per hour. Streams of energetic ultraviolet radiation cause the cast-off material to glow, but eventually the nebula will fade and leave behind only a small stellar corpse called a white dwarf. Our middle-aged Sun can expect a similar fate once it runs out of fuel in about 5 billion years.
Nebulae like Caldwell 69 are known as planetary nebulae but are not related to planets. The term was coined by astronomer William Herschel, who discovered the Butterfly Nebula in 1826. Through his small telescope, planetary nebulae had the appearance of glowing, planet-like orbs. While stars that generate planetary nebulae may have once had planets in orbit about them, scientists expect that the fiery death throes these stars undergo will ultimately destroy or leave any attending planets completely uninhabitable.
The Butterfly Nebula is located about 4,000 light-years away in the constellation Scorpius. Hubble obtained this close-up view in 2009 using its Wide Field Camera 3, installed by astronauts during the final shuttle servicing mission. These observations detected the nebula’s central star for the first time. Astronomers also compared the 2009 observations to those taken by Hubble’s Wide Field and Planetary Camera 2 in 2000 to determine the motions of the two lobes of ejected material, which appear to have been created rapidly in an event 2,250 years ago. Other parts of the nebula, specifically a dense, massive torus of material around the central star, were produced more slowly, starting about 5,000 years ago and then terminating about 2,900 years ago, preceding the lobe ejection. The delay between these events offers clues to how the stellar environment was modified as the central star evolved.
The Butterfly Nebula is highest and best viewed in the Southern Hemisphere during winter. From the Northern Hemisphere, its best season is the summer, but for most observers it will appear quite low above the southern horizon. With a magnitude of 9.5, the nebula is just visible with binoculars in dark skies, but a telescope will provide better views. In Hubble’s image above, filters that isolate emission from oxygen, helium, hydrogen, nitrogen and sulfur from the planetary nebula were used to create a composite color image. Through your telescope, you can expect to see something more reminiscent of a small, smoky eraser smudge. Use a medium to large telescope under dark skies to make out the nebula’s butterfly shape.
For more information about Hubble’s observations of Caldwell 69, see:
hubblesite.org/contents/media/images/2009/25/2616-Image.html
hubblesite.org/contents/news-releases/2004/news-2004-46.html
Credit: NASA, ESA, and the Hubble SM4 ERO Team
For Hubble's Caldwell catalog website and information on how to find these objects in the night sky, visit:
equipment: Leica Apo-Elmarit-R 180mmF2.8 and Canon EOS 5Dmk2-sp2, modified by Seo san on Takahashi EM-200 Temma 2 Jr, autoguided with hiro-design off-axis guider, SX Lodestar Autoguider, and PHD Guiding
exposure: 2 times x 30 minutes, 8 x 15 min, 4 x 4 min, and 2 x 1 minute at ISO 1,600 and f/4.0
site: 11,000 feet above sea level near Mauna Loa Observatory in Hawaii
This celestial object looks like a delicate butterfly. But it is far from serene.
What resemble dainty butterfly wings are actually roiling cauldrons of gas heated to more than 36,000 degrees Fahrenheit. The gas is tearing across space at more than 600,000 miles an hour — fast enough to travel from Earth to the Moon in 24 minutes!
A dying star that was once about five times the mass of the Sun is at the center of this fury. It has ejected its envelope of gases and is now unleashing a stream of ultraviolet radiation that is making the cast-off material glow. This object is an example of a planetary nebula, so-named because many of them have a round appearance resembling that of a planet when viewed through a small telescope.
The Wide Field Camera 3 (WFC3), the newest camera aboard NASA's Hubble Space Telescope, snapped this image of the planetary nebula, cataloged as NGC 6302, but more popularly called the Bug Nebula or the Butterfly Nebula. WFC3 was installed by NASA astronauts in May 2009, during the last servicing mission to upgrade and repair Hubble.
NGC 6302 lies within our Milky Way Galaxy, roughly 3,800 light-years away in the constellation Scorpius. The glowing gas is the star's outer layers, expelled over about 2,200 years. The "butterfly" stretches for more than two light-years, which is about half the distance from the Sun to the nearest star, Alpha Centauri.
The central star itself cannot be seen, because it is hidden within a doughnut-shaped ring of dust, which appears as a dark band pinching the nebula in the center. The thick dust belt constricts the star's outflow, creating the classic "bipolar" or hourglass shape displayed by some planetary nebulae.
The star's surface temperature is estimated to be about 400,000 degrees Fahrenheit, making it one of the hottest known stars in our galaxy. Spectroscopic observations made with ground-based telescopes show that the gas is roughly 36,000 degrees Fahrenheit, which is unusually hot compared to a typical planetary nebula.
The WFC3 image reveals a complex history of ejections from the star. The star first evolved into a huge red-giant star, with a diameter of about 1,000 times that of our Sun. It then lost its extended outer layers. Some of this gas was cast off from its equator at a relatively slow speed, perhaps as low as 20,000 miles an hour, creating the doughnut-shaped ring. Other gas was ejected perpendicular to the ring at higher speeds, producing the elongated "wings" of the butterfly-shaped structure. Later, as the central star heated up, a much faster stellar wind, a stream of charged particles traveling at more than 2 million miles an hour, plowed through the existing wing-shaped structure, further modifying its shape.
The image also shows numerous finger-like projections pointing back to the star, which may mark denser blobs in the outflow that have resisted the pressure from the stellar wind.
The nebula's reddish outer edges are largely due to light emitted by nitrogen, which marks the coolest gas visible in the picture. WFC3 is equipped with a wide variety of filters that isolate light emitted by various chemical elements, allowing astronomers to infer properties of the nebular gas, such as its temperature, density, and composition.
The white-colored regions are areas where light is emitted by sulfur. These are regions where fast-moving gas overtakes and collides with slow-moving gas that left the star at an earlier time, producing shock waves in the gas (the bright white edges on the sides facing the central star). The white blob with the crisp edge at upper right is an example of one of those shock waves.
NGC 6302 was imaged on July 27, 2009, with Hubble's Wide Field Camera 3 in ultraviolet and visible light. Filters that isolate emissions from oxygen, helium, hydrogen, nitrogen, and sulfur from the planetary nebula were used to create this composite image.
These Hubble observations of the planetary nebula NGC 6302 were part of the Hubble Servicing Mission 4 Early Release Observations.
For more information please visit:
hubblesite.org/image/2616/news_release/2009-25
See this link for an alternate near-ultraviolet to near-infrared view of the Butterfly Nebula, released in 2020: hubblesite.org/contents/news-releases/2020/news-2020-31?Y...
Credit: NASA, ESA, and the Hubble SM4 ERO Team
equipment: Leica Apo-Elmarit-R 180mmF2.8 and Canon EOS 5Dmk2-sp2, modified by Seo san on Takahashi EM-200 Temma 2 Jr, autoguided with hiro-design off-axis guider, SX Lodestar Autoguider, and PHD Guiding
exposure: 2 times x 30 minutes, 8 x 15 min, 4 x 4 min, and 2 x 1 minute at ISO 1,600 and f/4.0
site: 11,000 feet above sea level near Mauna Loa Observatory in Hawaii
The Bug Nebula, NGC 6302, is one of the brightest and most extreme planetary nebulae known. The fiery, dying star at its center is shrouded by a blanket of icy hailstones. This NASA Hubble Wide Field and Planetary Camera 2 image shows impressive walls of compressed gas, laced with trailing strands and bubbling outflows. A dark, dusty torus surrounds the inner nebula (seen at the upper right).
At the heart of the turmoil is one of the hottest stars known. Despite a sizzling temperature of at least 450,000 degrees Fahrenheit, the star itself has never been seen, as it is hidden by the blanket of dust and shines most brightly in the ultraviolet, making it hard to observe. The Bug Nebula lies about 4,000 light-years away in the southern constellation Scorpius.
For more information please visit:
hubblesite.org/image/1628/news_release/2004-46
Credit: NASA, ESA, and A.Zijlstra (UMIST, Manchester, UK)
This celestial object looks like a delicate butterfly. But it is far from serene. What resemble dainty butterfly wings are actually roiling cauldrons of gas heated to nearly 20 000 degrees Celsius. The gas is tearing across space at more than 950 000 kilometres per hour — fast enough to travel from Earth to the Moon in 24 minutes! A dying star that was once about five times the mass of the Sun is at the centre of this fury. It has ejected its envelope of gases and is now unleashing a stream of ultraviolet radiation that is making the cast-off material glow. This object is an example of a planetary nebula, so-named because many of them have a round appearance resembling that of a planet when viewed through a small telescope. The Wide Field Camera 3 (WFC3), a new camera aboard the NASA/ESA Hubble Space Telescope, snapped this image of the planetary nebula, catalogued as NGC 6302, but more popularly called the Bug Nebula or the Butterfly Nebula. WFC3 was installed by NASA astronauts in May 2009, during the Servicing Mission to upgrade and repair the 19-year-old Hubble. NGC 6302 lies within our Milky Way galaxy, roughly 3800 light-years away in the constellation of Scorpius. The glowing gas is the star's outer layers, expelled over about 2200 years. The "butterfly" stretches for more than two light-years, which is about half the distance from the Sun to the nearest star, Proxima Centauri. The central star itself cannot be seen, because it is hidden within a doughnut-shaped ring of dust, which appears as a dark band pinching the nebula in the centre. The thick dust belt constricts the star's outflow, creating the classic "bipolar" or hourglass shape displayed by some planetary nebulae. The star's surface temperature is estimated to be over 220 000 degrees Celsius, making it one of the hottest known stars in our galaxy. Spectroscopic observations made with ground-based telescopes show that the gas is roughly 20 000 degrees Celsius, which is unusually hot compared to a typical planetary nebula. The WFC3 image reveals a complex history of ejections from the star. The star first evolved into a huge red giant, with a diameter of about 1000 times that of our Sun. It then lost its extended outer layers. Some of this gas was cast off from its equator at a relatively slow speed, perhaps as low as 32 000 kilometres per hour, creating the doughnut-shaped ring. Other gas was ejected perpendicular to the ring at higher speeds, producing the elongated "wings" of the butterfly-shaped structure. Later, as the central star heated up, a much faster stellar wind, a stream of charged particles travelling at more than 3.2 million kilometres per hour, ploughed through the existing wing-shaped structure, further modifying its shape. The image also shows numerous finger-like projections pointing back to the star, which may mark denser blobs in the outflow that have resisted the pressure from the stellar wind. The nebula's reddish outer edges are largely due to light emitted by nitrogen, which marks the coolest gas visible in the picture. WFC3 is equipped with a wide variety of filters that isolate light emitted by various chemical elements, allowing astronomers to infer properties of the nebular gas, such as its temperature, density and composition. The white-coloured regions are areas where light is emitted by sulphur. These are regions where fast-moving gas overtakes and collides with slow-moving gas that left the star at an earlier time, producing shock waves in the gas (the bright white edges on the sides facing the central star). The white blob with the crisp edge at upper right is an example of one of those shock waves. NGC 6302 was imaged on 27 July 2009 with Hubble's Wide Field Camera 3 in ultraviolet and visible light. Filters that isolate emissions from oxygen, helium, hydrogen, nitrogen and sulphur from the planetary nebula were used to create this composite image. These Hubble observations of the planetary nebula NGC 6302 are part of the Hubble Servicing Mission 4 Early Release Observations.
The region in the tail of Scorpius around the Cat’s Paw Nebula, NGC 6334, centred, with NGC 6357 above at the top and the tiny planetary, the Bug Nebula, NGC 6302, at bottom right. Shaula or Lambda Scorpii, is the brightest star at lower left, along with Lesath, the stars marking the stinger in the tail of Scorpius.
This is a stack of 5 x 6-minute exposures with the Borg 77mm f/4 astrograph and filter-modified Canon 5D MkII taken from the Tibuc Cottage, Coonabarabran, NSW, Australia.
This celestial object looks like a delicate butterfly. But it is far from serene. What resemble dainty butterfly wings are actually roiling cauldrons of gas heated to nearly 20 000 degrees Celsius. The gas is tearing across space at more than 950 000 kilometres per hour — fast enough to travel from Earth to the Moon in 24 minutes! A dying star that was once about five times the mass of the Sun is at the centre of this fury. It has ejected its envelope of gases and is now unleashing a stream of ultraviolet radiation that is making the cast-off material glow. This object is an example of a planetary nebula, so-named because many of them have a round appearance resembling that of a planet when viewed through a small telescope. The Wide Field Camera 3 (WFC3), a new camera aboard the NASA/ESA Hubble Space Telescope, snapped this image of the planetary nebula, catalogued as NGC 6302, but more popularly called the Bug Nebula or the Butterfly Nebula. WFC3 was installed by NASA astronauts in May 2009, during the Servicing Mission to upgrade and repair the 19-year-old Hubble. NGC 6302 lies within our Milky Way galaxy, roughly 3800 light-years away in the constellation of Scorpius. The glowing gas is the star's outer layers, expelled over about 2200 years. The "butterfly" stretches for more than two light-years, which is about half the distance from the Sun to the nearest star, Proxima Centauri. The central star itself cannot be seen, because it is hidden within a doughnut-shaped ring of dust, which appears as a dark band pinching the nebula in the centre. The thick dust belt constricts the star's outflow, creating the classic "bipolar" or hourglass shape displayed by some planetary nebulae. The star's surface temperature is estimated to be over 220 000 degrees Celsius, making it one of the hottest known stars in our galaxy. Spectroscopic observations made with ground-based telescopes show that the gas is roughly 20 000 degrees Celsius, which is unusually hot compared to a typical planetary nebula. The WFC3 image reveals a complex history of ejections from the star. The star first evolved into a huge red giant, with a diameter of about 1000 times that of our Sun. It then lost its extended outer layers. Some of this gas was cast off from its equator at a relatively slow speed, perhaps as low as 32 000 kilometres per hour, creating the doughnut-shaped ring. Other gas was ejected perpendicular to the ring at higher speeds, producing the elongated "wings" of the butterfly-shaped structure. Later, as the central star heated up, a much faster stellar wind, a stream of charged particles travelling at more than 3.2 million kilometres per hour, ploughed through the existing wing-shaped structure, further modifying its shape. The image also shows numerous finger-like projections pointing back to the star, which may mark denser blobs in the outflow that have resisted the pressure from the stellar wind. The nebula's reddish outer edges are largely due to light emitted by nitrogen, which marks the coolest gas visible in the picture. WFC3 is equipped with a wide variety of filters that isolate light emitted by various chemical elements, allowing astronomers to infer properties of the nebular gas, such as its temperature, density and composition. The white-coloured regions are areas where light is emitted by sulphur. These are regions where fast-moving gas overtakes and collides with slow-moving gas that left the star at an earlier time, producing shock waves in the gas (the bright white edges on the sides facing the central star). The white blob with the crisp edge at upper right is an example of one of those shock waves. NGC 6302 was imaged on 27 July 2009 with Hubble's Wide Field Camera 3 in ultraviolet and visible light. Filters that isolate emissions from oxygen, helium, hydrogen, nitrogen and sulphur from the planetary nebula were used to create this composite image. These Hubble observations of the planetary nebula NGC 6302 are part of the Hubble Servicing Mission 4 Early Release Observations.
Technical information:
astroanarchy.blogspot.com/2010/07/ngc-6302-bug-nebula.html
An animated 3D:
astroanarchy.blogspot.com/2010/07/ngc-6302-bug-nebula-as-...
3D-studies in different formats:
NGC6302 "Nebulosa de la mariposa"
16/5/09
Hokenn 114/900
Webcam Phillips SPC900NC modificada a foco primario f/8
Montura EQ2
DSS + PS CS4
This celestial object looks like a delicate butterfly. But it is far from serene. What resemble dainty butterfly wings are actually roiling cauldrons of gas heated to nearly 20 000 degrees Celsius. The gas is tearing across space at more than 950 000 kilometres per hour — fast enough to travel from Earth to the Moon in 24 minutes! A dying star that was once about five times the mass of the Sun is at the centre of this fury. It has ejected its envelope of gases and is now unleashing a stream of ultraviolet radiation that is making the cast-off material glow. This object is an example of a planetary nebula, so-named because many of them have a round appearance resembling that of a planet when viewed through a small telescope. The Wide Field Camera 3 (WFC3), a new camera aboard the NASA/ESA Hubble Space Telescope, snapped this image of the planetary nebula, catalogued as NGC 6302, but more popularly called the Bug Nebula or the Butterfly Nebula. WFC3 was installed by NASA astronauts in May 2009, during the Servicing Mission to upgrade and repair the 19-year-old Hubble. NGC 6302 lies within our Milky Way galaxy, roughly 3800 light-years away in the constellation of Scorpius. The glowing gas is the star's outer layers, expelled over about 2200 years. The "butterfly" stretches for more than two light-years, which is about half the distance from the Sun to the nearest star, Proxima Centauri. The central star itself cannot be seen, because it is hidden within a doughnut-shaped ring of dust, which appears as a dark band pinching the nebula in the centre. The thick dust belt constricts the star's outflow, creating the classic "bipolar" or hourglass shape displayed by some planetary nebulae. The star's surface temperature is estimated to be over 220 000 degrees Celsius, making it one of the hottest known stars in our galaxy. Spectroscopic observations made with ground-based telescopes show that the gas is roughly 20 000 degrees Celsius, which is unusually hot compared to a typical planetary nebula. The WFC3 image reveals a complex history of ejections from the star. The star first evolved into a huge red giant, with a diameter of about 1000 times that of our Sun. It then lost its extended outer layers. Some of this gas was cast off from its equator at a relatively slow speed, perhaps as low as 32 000 kilometres per hour, creating the doughnut-shaped ring. Other gas was ejected perpendicular to the ring at higher speeds, producing the elongated "wings" of the butterfly-shaped structure. Later, as the central star heated up, a much faster stellar wind, a stream of charged particles travelling at more than 3.2 million kilometres per hour, ploughed through the existing wing-shaped structure, further modifying its shape. The image also shows numerous finger-like projections pointing back to the star, which may mark denser blobs in the outflow that have resisted the pressure from the stellar wind. The nebula's reddish outer edges are largely due to light emitted by nitrogen, which marks the coolest gas visible in the picture. WFC3 is equipped with a wide variety of filters that isolate light emitted by various chemical elements, allowing astronomers to infer properties of the nebular gas, such as its temperature, density and composition. The white-coloured regions are areas where light is emitted by sulphur. These are regions where fast-moving gas overtakes and collides with slow-moving gas that left the star at an earlier time, producing shock waves in the gas (the bright white edges on the sides facing the central star). The white blob with the crisp edge at upper right is an example of one of those shock waves. NGC 6302 was imaged on 27 July 2009 with Hubble's Wide Field Camera 3 in ultraviolet and visible light. Filters that isolate emissions from oxygen, helium, hydrogen, nitrogen and sulphur from the planetary nebula were used to create this composite image. These Hubble observations of the planetary nebula NGC 6302 are part of the Hubble Servicing Mission 4 Early Release Observations.
This celestial object looks like a delicate butterfly. But it is far from serene. What resemble dainty butterfly wings are actually roiling cauldrons of gas heated to nearly 20 000 degrees Celsius. The gas is tearing across space at more than 950 000 kilometres per hour — fast enough to travel from Earth to the Moon in 24 minutes! A dying star that was once about five times the mass of the Sun is at the centre of this fury. It has ejected its envelope of gases and is now unleashing a stream of ultraviolet radiation that is making the cast-off material glow. This object is an example of a planetary nebula, so-named because many of them have a round appearance resembling that of a planet when viewed through a small telescope. The Wide Field Camera 3 (WFC3), a new camera aboard the NASA/ESA Hubble Space Telescope, snapped this image of the planetary nebula, catalogued as NGC 6302, but more popularly called the Bug Nebula or the Butterfly Nebula. WFC3 was installed by NASA astronauts in May 2009, during the Servicing Mission to upgrade and repair the 19-year-old Hubble. NGC 6302 lies within our Milky Way galaxy, roughly 3800 light-years away in the constellation of Scorpius. The glowing gas is the star's outer layers, expelled over about 2200 years. The "butterfly" stretches for more than two light-years, which is about half the distance from the Sun to the nearest star, Proxima Centauri. The central star itself cannot be seen, because it is hidden within a doughnut-shaped ring of dust, which appears as a dark band pinching the nebula in the centre. The thick dust belt constricts the star's outflow, creating the classic "bipolar" or hourglass shape displayed by some planetary nebulae. The star's surface temperature is estimated to be over 220 000 degrees Celsius, making it one of the hottest known stars in our galaxy. Spectroscopic observations made with ground-based telescopes show that the gas is roughly 20 000 degrees Celsius, which is unusually hot compared to a typical planetary nebula. The WFC3 image reveals a complex history of ejections from the star. The star first evolved into a huge red giant, with a diameter of about 1000 times that of our Sun. It then lost its extended outer layers. Some of this gas was cast off from its equator at a relatively slow speed, perhaps as low as 32 000 kilometres per hour, creating the doughnut-shaped ring. Other gas was ejected perpendicular to the ring at higher speeds, producing the elongated "wings" of the butterfly-shaped structure. Later, as the central star heated up, a much faster stellar wind, a stream of charged particles travelling at more than 3.2 million kilometres per hour, ploughed through the existing wing-shaped structure, further modifying its shape. The image also shows numerous finger-like projections pointing back to the star, which may mark denser blobs in the outflow that have resisted the pressure from the stellar wind. The nebula's reddish outer edges are largely due to light emitted by nitrogen, which marks the coolest gas visible in the picture. WFC3 is equipped with a wide variety of filters that isolate light emitted by various chemical elements, allowing astronomers to infer properties of the nebular gas, such as its temperature, density and composition. The white-coloured regions are areas where light is emitted by sulphur. These are regions where fast-moving gas overtakes and collides with slow-moving gas that left the star at an earlier time, producing shock waves in the gas (the bright white edges on the sides facing the central star). The white blob with the crisp edge at upper right is an example of one of those shock waves. NGC 6302 was imaged on 27 July 2009 with Hubble's Wide Field Camera 3 in ultraviolet and visible light. Filters that isolate emissions from oxygen, helium, hydrogen, nitrogen and sulphur from the planetary nebula were used to create this composite image. These Hubble observations of the planetary nebula NGC 6302 are part of the Hubble Servicing Mission 4 Early Release Observations.
This celestial object looks like a delicate butterfly. But it is far from serene. What resemble dainty butterfly wings are actually roiling cauldrons of gas heated to nearly 20 000 degrees Celsius. The gas is tearing across space at more than 950 000 kilometres per hour — fast enough to travel from Earth to the Moon in 24 minutes! A dying star that was once about five times the mass of the Sun is at the centre of this fury. It has ejected its envelope of gases and is now unleashing a stream of ultraviolet radiation that is making the cast-off material glow. This object is an example of a planetary nebula, so-named because many of them have a round appearance resembling that of a planet when viewed through a small telescope. The Wide Field Camera 3 (WFC3), a new camera aboard the NASA/ESA Hubble Space Telescope, snapped this image of the planetary nebula, catalogued as NGC 6302, but more popularly called the Bug Nebula or the Butterfly Nebula. WFC3 was installed by NASA astronauts in May 2009, during the Servicing Mission to upgrade and repair the 19-year-old Hubble. NGC 6302 lies within our Milky Way galaxy, roughly 3800 light-years away in the constellation of Scorpius. The glowing gas is the star's outer layers, expelled over about 2200 years. The "butterfly" stretches for more than two light-years, which is about half the distance from the Sun to the nearest star, Proxima Centauri. The central star itself cannot be seen, because it is hidden within a doughnut-shaped ring of dust, which appears as a dark band pinching the nebula in the centre. The thick dust belt constricts the star's outflow, creating the classic "bipolar" or hourglass shape displayed by some planetary nebulae. The star's surface temperature is estimated to be over 220 000 degrees Celsius, making it one of the hottest known stars in our galaxy. Spectroscopic observations made with ground-based telescopes show that the gas is roughly 20 000 degrees Celsius, which is unusually hot compared to a typical planetary nebula. The WFC3 image reveals a complex history of ejections from the star. The star first evolved into a huge red giant, with a diameter of about 1000 times that of our Sun. It then lost its extended outer layers. Some of this gas was cast off from its equator at a relatively slow speed, perhaps as low as 32 000 kilometres per hour, creating the doughnut-shaped ring. Other gas was ejected perpendicular to the ring at higher speeds, producing the elongated "wings" of the butterfly-shaped structure. Later, as the central star heated up, a much faster stellar wind, a stream of charged particles travelling at more than 3.2 million kilometres per hour, ploughed through the existing wing-shaped structure, further modifying its shape. The image also shows numerous finger-like projections pointing back to the star, which may mark denser blobs in the outflow that have resisted the pressure from the stellar wind. The nebula's reddish outer edges are largely due to light emitted by nitrogen, which marks the coolest gas visible in the picture. WFC3 is equipped with a wide variety of filters that isolate light emitted by various chemical elements, allowing astronomers to infer properties of the nebular gas, such as its temperature, density and composition. The white-coloured regions are areas where light is emitted by sulphur. These are regions where fast-moving gas overtakes and collides with slow-moving gas that left the star at an earlier time, producing shock waves in the gas (the bright white edges on the sides facing the central star). The white blob with the crisp edge at upper right is an example of one of those shock waves. NGC 6302 was imaged on 27 July 2009 with Hubble's Wide Field Camera 3 in ultraviolet and visible light. Filters that isolate emissions from oxygen, helium, hydrogen, nitrogen and sulphur from the planetary nebula were used to create this composite image. These Hubble observations of the planetary nebula NGC 6302 are part of the Hubble Servicing Mission 4 Early Release Observations.
This celestial object looks like a delicate butterfly. But it is far from serene. What resemble dainty butterfly wings are actually roiling cauldrons of gas heated to nearly 20 000 degrees Celsius. The gas is tearing across space at more than 950 000 kilometres per hour — fast enough to travel from Earth to the Moon in 24 minutes! A dying star that was once about five times the mass of the Sun is at the centre of this fury. It has ejected its envelope of gases and is now unleashing a stream of ultraviolet radiation that is making the cast-off material glow. This object is an example of a planetary nebula, so-named because many of them have a round appearance resembling that of a planet when viewed through a small telescope. The Wide Field Camera 3 (WFC3), a new camera aboard the NASA/ESA Hubble Space Telescope, snapped this image of the planetary nebula, catalogued as NGC 6302, but more popularly called the Bug Nebula or the Butterfly Nebula. WFC3 was installed by NASA astronauts in May 2009, during the Servicing Mission to upgrade and repair the 19-year-old Hubble. NGC 6302 lies within our Milky Way galaxy, roughly 3800 light-years away in the constellation of Scorpius. The glowing gas is the star's outer layers, expelled over about 2200 years. The "butterfly" stretches for more than two light-years, which is about half the distance from the Sun to the nearest star, Proxima Centauri. The central star itself cannot be seen, because it is hidden within a doughnut-shaped ring of dust, which appears as a dark band pinching the nebula in the centre. The thick dust belt constricts the star's outflow, creating the classic "bipolar" or hourglass shape displayed by some planetary nebulae. The star's surface temperature is estimated to be over 220 000 degrees Celsius, making it one of the hottest known stars in our galaxy. Spectroscopic observations made with ground-based telescopes show that the gas is roughly 20 000 degrees Celsius, which is unusually hot compared to a typical planetary nebula. The WFC3 image reveals a complex history of ejections from the star. The star first evolved into a huge red giant, with a diameter of about 1000 times that of our Sun. It then lost its extended outer layers. Some of this gas was cast off from its equator at a relatively slow speed, perhaps as low as 32 000 kilometres per hour, creating the doughnut-shaped ring. Other gas was ejected perpendicular to the ring at higher speeds, producing the elongated "wings" of the butterfly-shaped structure. Later, as the central star heated up, a much faster stellar wind, a stream of charged particles travelling at more than 3.2 million kilometres per hour, ploughed through the existing wing-shaped structure, further modifying its shape. The image also shows numerous finger-like projections pointing back to the star, which may mark denser blobs in the outflow that have resisted the pressure from the stellar wind. The nebula's reddish outer edges are largely due to light emitted by nitrogen, which marks the coolest gas visible in the picture. WFC3 is equipped with a wide variety of filters that isolate light emitted by various chemical elements, allowing astronomers to infer properties of the nebular gas, such as its temperature, density and composition. The white-coloured regions are areas where light is emitted by sulphur. These are regions where fast-moving gas overtakes and collides with slow-moving gas that left the star at an earlier time, producing shock waves in the gas (the bright white edges on the sides facing the central star). The white blob with the crisp edge at upper right is an example of one of those shock waves. NGC 6302 was imaged on 27 July 2009 with Hubble's Wide Field Camera 3 in ultraviolet and visible light. Filters that isolate emissions from oxygen, helium, hydrogen, nitrogen and sulphur from the planetary nebula were used to create this composite image. These Hubble observations of the planetary nebula NGC 6302 are part of the Hubble Servicing Mission 4 Early Release Observations.
Segunda captura da nebulosa da borboleta, ou Bug nebula (NGC 6302). A primeira foi feita há +/- 1 ano e tem menos detalhes. É engraçado que, por ter sido feita agora com uma câmera modificada, não aparece verde na nebulosa, como em uma câmera não modificada. Vocês podem ver a captura anterior rolando as fotos da minha galeria do Instagram. Feita de um local bortle 8 com filtro Optolong L-Pro.
My second capture of the Bug nebula (NGC 6302). The first one was made about a year ago and it has less detail. It's noticeable that, for being made with a modifyed DSLR, you don't see the green that appeared in the capture made with a stock DSLR. You can see the picture that I'm talking about in my Instagram gallery. The picture was taken from a bortle 8 site with an Optolong L-Pro filter.
Canon T3i modified, Sky-Watcher 200p (200/1000mm), ISO 800. Guiding with Asiair and ASI290mc in an adapted finderscope 50mm, Eq5 Sky-watcher mount and AstroEq tracking mod. 18 Ligth Frames of 120s, 26 darks and 50 bias. 36m total exposure. Processing on Pixinsight. Bortle 8.
#astrophotography #astrofotografia #nightsky #astronomy #astromomia #CanonT3i #canon600d #dslrmod #telescopio #skywatcher #skywatcher200p #Eq5 #skywatcherEq5 #AstroEq #bortle8 #bortle8sky #DeepSkyStacker #deepsky #pixinsight #asi290mc #ZwoAsi #zwoasi290mc #asiair #guiding #lpro #optolonglpro #ngc6302 #bugnebula #astfotbr
The Bug Nebula, NGC 6302, is one of the brightest and most extreme planetary nebulae known. At its centre lies a superhot, dying star smothered in a blanket of hailstones. A new Hubble image reveals fresh detail in the wings of this cosmic butterfly. Most planetary nebulae are distinctive, but few are as extreme as NGC 6302, also known as the Bug Nebula. The fiery, dying star at its centre is shrouded by a blanket of icy hailstones.
Hubble (2009-09-09) Bug Nebula, Butterfly Nebula, NGC 6320 (Hubble) - Central star in Bug Nebula found
This celestial object looks like a delicate butterfly. But it is far from serene. What resemble dainty butterfly wings are actually roiling cauldrons of gas heated to nearly 20 000 degrees Celsius. The gas is tearing across space at more than 950 000 kilometres per hour — fast enough to travel from Earth to the Moon in 24 minutes! A dying star that was once about five times the mass of the Sun is at the centre of this fury. It has ejected its envelope of gases and is now unleashing a stream of ultraviolet radiation that is making the cast-off material glow. This object is an example of a planetary nebula, so-named because many of them have a round appearance resembling that of a planet when viewed through a small telescope. The Wide Field Camera 3 (WFC3), a new camera aboard the NASA/ESA Hubble Space Telescope, snapped this image of the planetary nebula, catalogued as NGC 6302, but more popularly called the Bug Nebula or the Butterfly Nebula. WFC3 was installed by NASA astronauts in May 2009, during the Servicing Mission to upgrade and repair the 19-year-old Hubble. NGC 6302 lies within our Milky Way galaxy, roughly 3800 light-years away in the constellation of Scorpius. The glowing gas is the star's outer layers, expelled over about 2200 years. The "butterfly" stretches for more than two light-years, which is about half the distance from the Sun to the nearest star, Proxima Centauri. The central star itself cannot be seen, because it is hidden within a doughnut-shaped ring of dust, which appears as a dark band pinching the nebula in the centre. The thick dust belt constricts the star's outflow, creating the classic "bipolar" or hourglass shape displayed by some planetary nebulae. The star's surface temperature is estimated to be over 220 000 degrees Celsius, making it one of the hottest known stars in our galaxy. Spectroscopic observations made with ground-based telescopes show that the gas is roughly 20 000 degrees Celsius, which is unusually hot compared to a typical planetary nebula. The WFC3 image reveals a complex history of ejections from the star. The star first evolved into a huge red giant, with a diameter of about 1000 times that of our Sun. It then lost its extended outer layers. Some of this gas was cast off from its equator at a relatively slow speed, perhaps as low as 32 000 kilometres per hour, creating the doughnut-shaped ring. Other gas was ejected perpendicular to the ring at higher speeds, producing the elongated "wings" of the butterfly-shaped structure. Later, as the central star heated up, a much faster stellar wind, a stream of charged particles travelling at more than 3.2 million kilometres per hour, ploughed through the existing wing-shaped structure, further modifying its shape. The image also shows numerous finger-like projections pointing back to the star, which may mark denser blobs in the outflow that have resisted the pressure from the stellar wind. The nebula's reddish outer edges are largely due to light emitted by nitrogen, which marks the coolest gas visible in the picture. WFC3 is equipped with a wide variety of filters that isolate light emitted by various chemical elements, allowing astronomers to infer properties of the nebular gas, such as its temperature, density and composition. The white-coloured regions are areas where light is emitted by sulphur. These are regions where fast-moving gas overtakes and collides with slow-moving gas that left the star at an earlier time, producing shock waves in the gas (the bright white edges on the sides facing the central star). The white blob with the crisp edge at upper right is an example of one of those shock waves. NGC 6302 was imaged on 27 July 2009 with Hubble's Wide Field Camera 3 in ultraviolet and visible light. Filters that isolate emissions from oxygen, helium, hydrogen, nitrogen and sulphur from the planetary nebula were used to create this composite image. These Hubble observations of the planetary nebula NGC 6302 are part of the Hubble Servicing Mission 4 Early Release Observations.