SH2-132 22h.14m.24s +56.04.21 N
During the 1950s Stewart Sharpless cataloged many Nebulae, this object is one of Stewart's objects, Located in the Constellation of Cepheus it is often over look by astrophotographers due to the
proximity of IC1396 the Elephant Trunk Nebula, it is quite a nice nebula with many dark globules and shock fronts
Camera Canon 350d Modified Baader IR/UV
Astrononmik CLS EOS Broadband Filter
Scope Carbon Fibre Celestron C8 w. 6.3 reducer
Mount Celestron CGE
4 hrs Exposure from light polluted skies
Captured 12-1-08, 12-2-08, 12-3-08
total of 40 6 Minute Subs
captured using CGE 800 (XLT)
submitted by John_Buonomo
Messier 106 (also known as NGC 4258) is a spiral galaxy about in the constellation Canes Venatici. It was discovered by Pierre M�chain in 1781. M106 is at a distance of about 22 to 25 million
light-years away from Earth. It is also a Seyfert II galaxy, which means that due to x-rays and unusual emission lines detected, it is suspected that part of the galaxy is falling into a
supermassive black hole in the center.[7] NGC 4217 is a possible companion galaxy of Messier 106.[6]
Desc- Wiki.org
captured using CGE 800 (XLT)
submitted by John_Buonomo
The Orion Nebula (also known as Messier 42, M42, or NGC 1976) is a diffuse nebula situated south[b] of Orion's Belt. It is one of the brightest nebulae, and is visible to the naked eye in the
night sky. M42 is located at a distance of 1,270�76 light years[2] and is the closest region of massive star formation to Earth. The M42 nebula is estimated to be 24 light years across. Older
texts frequently referred to the Orion Nebula as the Great Nebula in Orion or the Great Orion Nebula. Yet older, astrological texts refer to it as Ensis (Latin for "sword"), which was also the
name given to the star Eta Orionis, which can be seen close to the nebula from Earth.[5]
The Orion Nebula is one of the most scrutinized and photographed objects in the night sky, and is among the most intensely studied celestial features.[6] The nebula has revealed much about the
process of how stars and planetary systems are formed from collapsing clouds of gas and dust. Astronomers have directly observed protoplanetary disks, brown dwarfs, intense and turbulent motions
of the gas, and the photo-ionizing effects of massive nearby stars in the nebula.There are also supersonic bullets of gas piercing through the dense hydrogen clouds of the Orion Nebula. Each
bullet is ten times the diameter of Pluto's orbit and are tipped with iron atoms glowing bright blue.They were probably formed one thousand years ago from an unkown violent event.
-Desc -Wiki.org
captured using CGE 800 (XLT)
submitted by John_Buonomo
The Horsehead Nebula (also known as Barnard 33 in bright nebula IC 434) is a dark nebula in the Orion constellation. The nebula is located just below Alnitak, the star furthest left on Orion's
Belt, and is part of the much larger Orion Molecular Cloud Complex. It is approximately 1500 light years from Earth. It is one of the most identifiable nebulae because of the shape of its
swirling cloud of dark dust and gases, which is similar to that of a horse's head. The shape was first noticed in 1888 by Williamina Fleming on photographic plate B2312 taken at the Harvard
College Observatory.
The red glow originates from hydrogen gas predominantly behind the nebula, ionized by the nearby bright star Sigma Orionis. The darkness of the Horsehead is caused mostly by thick dust, although
the lower part of the Horsehead's neck casts a shadow to the left. Streams of gas leaving the nebula are funneled by a strong magnetic field. Bright spots in the Horsehead Nebula's base are young
stars just in the process of forming.
Desc- Wiki.org
captured using CGE 800 (XLT)
submitted by John_Buonomo
The Orion Nebula (also known as Messier 42, M42, or NGC 1976) is a diffuse nebula situated south[b] of Orion's Belt. It is one of the brightest nebulae, and is visible to the naked eye in the
night sky. M42 is located at a distance of 1,270�76 light years[2] and is the closest region of massive star formation to Earth. The M42 nebula is estimated to be 24 light years across. Older
texts frequently referred to the Orion Nebula as the Great Nebula in Orion or the Great Orion Nebula. Yet older, astrological texts refer to it as Ensis (Latin for "sword"), which was also the
name given to the star Eta Orionis, which can be seen close to the nebula from Earth.[5]
The Orion Nebula is one of the most scrutinized and photographed objects in the night sky, and is among the most intensely studied celestial features.[6] The nebula has revealed much about the
process of how stars and planetary systems are formed from collapsing clouds of gas and dust. Astronomers have directly observed protoplanetary disks, brown dwarfs, intense and turbulent motions
of the gas, and the photo-ionizing effects of massive nearby stars in the nebula. There are also supersonic bullets of gas piercing through the dense hydrogen clouds of the Orion Nebula. Each
bullet is ten times the diameter of Pluto's orbit and are tipped with iron atoms glowing bright blue. They were probably formed one thousand years ago from an unknown violent event.
-Wiki Desc
captured using CGE 800 (XLT)
submitted by John_Buonomo
IC 443 (also known as the Jellyfish Nebula) is a Galactic supernova remnant (SNR) in the constellation Gemini. On the plan of the sky, it is located near the star Eta Geminorum. Its distance is
roughly 5,000 light years (~5�1016 km) from Earth.
IC 443 is thought to be the remains of a supernova occurred 3,000 - 30,000 years ago. The same supernova event likely created the neutron star CXOU J061705.3+222127, the collapsed remnant of the
stellar core.
IC 443 is one of the best-studied case of supernova remnant interacting with surrounding molecular clouds.
captured using CGE 800 (XLT)
submitted by John_Buonomo
NGC 2264 is sometimes referred to as the Christmas Tree Cluster and the Cone Nebula. However, the designation of NGC 2264 in the New General Catalogue refers to both objects and not the cluster
alone.
captured using CGE 800 (XLT)
submitted by John_Buonomo
The Rosette Nebula is a large, circular H II region located near one end of a giant molecular cloud in the Monoceros region of the Milky Way Galaxy. The open cluster NGC 2244 is closely
associated with the nebulosity, the stars of the cluster having been formed from the nebula's matter.
captured using CGE 800 (XLT)
submitted by John_Buonomo
Section of the Constellation Auriga which Includes a few Intresting Objects
At the Top are the Tadpoles of IC410, In the Middle is IC417 and the Clusters at the bottom are Messier 38 and NGC1907
captured using CGE 800 (XLT)
submitted by John_Buonomo
NGC 2174 is an H II emission nebula located in the constellation Orion and is associated with the open star cluster NGC 2175 It is thought to be located about 6400 light-years away from earth.
The nebula may have formed through hierarchical collapse, To the lower part of the image is a SuperNova Remenant cataloged by Stewart Sharpless in the 1950s as catalog entry, sh2-247
captured using CGE 800 (XLT)
submitted by John_Buonomo
Magnitude: 7.30
Luminosit� surfacique: 11.20
Description: !!vB,vL,bi-N,IE,Dumbbell Neb
PK60-3.1;Lord Rosse drew 18* invl
captured using CGE 925 (XLT)
submitted by satlocenr
NGC 2841, a nice galaxy and a difficult target.
captured using CGE 925 (XLT)
submitted by hgg
alaxie M 101 (NGC 5457)
Constellation: Grande Ourse
Dimension: 28.5'x 28.3' / Magnitude: 7.90
Luminosit� surfacique: 14.90
J2000 RA: 14h03m12.00s DE:+54�20'60.0"
Date RA: 14h03m31.80s DE:+54�18'19.3"
D�PART DE LA S�ANCE : Azimut : +65�49' / Altitude :+69�45'
FIN DE LA S�ANCE : Azimut : +255�13' / Altitude : +80�59'
Culmination : 23h45m
captured using CGE 925 (XLT)
submitted by satlocenr
One of the most beautiful star clusters of the nothern hemisphere!
captured using CGE 925 (XLT)
submitted by hgg
This was shot with 300mm zoom piggybaked. One 5 min. shot before dew invaded my lenses.
captured using CGE 925 (XLT)
submitted by Ed_Malm
This is a combination of 3 Different images with 3 different cameras and focal lenghs combined in Registar
captured using CGE 1100 (XLT)
submitted by Les T
This is my standard Star Party portable equipment. I've built a computer hutch which folds flat for transport, and all the equipment fits into my Chevy Blazer. The computer is a home built 2.4
GHz Athlon tower with MaximDL, Celestron's NexRemote and PEC (both fantastic), TheSky6, Maxpoint, and Photoshop CS3.
captured using CGE 1100 (XLT)
submitted by drpdmartin
Texas Star Party 2009
Fantastic seeing
Hyperstar 3/QHY8:
FOV=2.4 X 1.6 arc min
Inset is M88 enlarged to show the detail present in the image
captured using CGE 1100 (XLT)
submitted by drpdmartin
Io can be seen clearly above the NEB. The GRS, red Junior and the new red spot all grace this image. A wonderful night.
captured using CGE 1400 (XLT)
submitted by Paul_Haese
This image was taken from 35 degrees South at a time when Saturn was near its most northern declination. Saturn was at 44 degrees from the horizon.
captured using CGE 1400 (XLT)
submitted by Paul_Haese
Callisto can be seen here with detail showing as it moves onto the limb of Jupiter. The new spots near the GRS can also be seen well too.
captured using CGE 1400 (XLT)
submitted by Paul_Haese
A new photo putting only the phone camera on a new eyepiece, testing to wiew a full moon image without focal reducer
captured using CGE 1400 Fastar (XLT)
submitted by marcdica
Messier 82 (also known as NGC 3034 or the Cigar Galaxy) is the prototype[3] nearby starburst galaxy about 12 million light-years away in the constellation Ursa Major. The starburst galaxy is five
times as bright as the whole Milky Way and one hundred times as bright as our galaxy's center.[3]
In 2005, the Hubble revealed 197 young massive clusters in the starburst core.[3] The average mass of these clusters is around 2�105 M⊙, hence the starburst core is a very energetic and
high-density environment.[3] Throughout the galaxy's center, young stars are being born 10 times faster than they are inside our entire Milky Way Galaxy.[4]
captured using CGE Computerized Mount
submitted by John_Buonomo
NGC 2903 is a barred spiral galaxy about 20.5 million light-years away in the constellation Leo. It was discovered by William Herschel who cataloged it as on November 16, 1784. NGC 2905 is a
bright knot (star cloud) within this galaxy.
captured using CGE Computerized Mount
submitted by John_Buonomo
Messier 46 (also known as M 46 or NGC 2437) is an open cluster in the constellation of Puppis. It was discovered by Charles Messier in 1771. Dreyer described it as "very bright, very rich, very
large." M46 is about 5,500 light-years away with an estimated age on the order of several 100 million years.[1]
The planetary nebula NGC 2438 appears to lie within the cluster near its northern edge (the faint smudge at the top center of the image), but it is most likely unrelated since it does not share
the cluster's radial velocity.[1][2] The case is yet another example of a superposed pair, joining the famed case of NGC 2818. [3][1]
M46 is about a degree east of M47 in the sky, so the two fit well in a binocular or wide-angle telescope field.
- Wiki
captured using CGE Computerized Mount
submitted by John_Buonomo
The Eskimo Nebula (NGC 2392), also known as the Clownface Nebula,[4] is a bipolar[2] double-shell[5] planetary nebula (PN). It was discovered by astronomer William Herschel in 1787. From the
ground, it resembles a person's head surrounded by a parka hood. In 2000, the Hubble Space Telescope produced an image of it. From space, the nebula displays gas clouds so complex that they are
not fully understood.
Its inner shell measures 18″ � 15″ and is bright and elliptical and marked on its south rim by two blister-like protrusions. Its outer shell is nearly circular measuring 24″ radius and contains a
set of complex low-ionization features. It is observed to have high-dispersion spectra of optical nebular lines which indicate a fast collimated outflow with a velocity along our line of sight of
nearly 200 km/s producing dynamic interaction with nebular material. As of 2003, it is estimated to be only ≥1060 years old. The earth's perspective is almost along its axis of symmetry. Its
knots have a highly developed symmetry along a radius vector from the PN's central star, except their tails are somewhat irregular. The tails are well developed and frequently of a discernible
optical thickness in the visual spectrum. The knots are bright rimmed and have low ionization (as compared to those found in NGC 7293) which indicates their location being inside the ionized zone
yet close to the boundary. The knots' heads have local photoionization fronts which appear as bright cusps. At the cusps, the knots become optically thick to Lyc photons from the central
star.
It is surrounded by gas that composed the outer layers of a Sun-like star. The visible inner filaments are ejected by strong wind of particles from the central star. The outer disk contains
unusual light-year long orange filaments.
NGC 2392 lies about 3000 light-years away and is visible with a small telescope in the constellation of Gemini.
- Wiki
captured using CGE Computerized Mount
submitted by John_Buonomo
The Crab Nebula (catalogue designations M1, NGC 1952, Taurus A) is a supernova remnant and pulsar wind nebula in the constellation of Taurus. The nebula was first observed by John Bevis, and
corresponds to a bright supernova recorded by Chinese and Arab astronomers in 1054. Located at a distance of about 6,500 light-years (2 kpc) from Earth, the nebula has a diameter of 11 ly (3.4
pc) and expands at a rate of about 1,500 kilometers per second.
At the center of the nebula lies the Crab Pulsar, a rotating neutron star, which emits pulses of radiation from gamma rays to radio waves with a spin rate of 30.2 times per second. The nebula was
the first astronomical object identified with a historical supernova explosion.
The nebula acts as a source of radiation for studying celestial bodies that occult it. In the 1950s and 1960s, the Sun's corona was mapped from observations of the Crab's radio waves passing
through it, and more recently, the thickness of the atmosphere of Saturn's moon Titan was measured as it blocked out X-rays from the nebula.
- WIKI
captured using CGE Computerized Mount
submitted by John_Buonomo
NGC 4244, also Caldwell 26, is an edge-on loose Spiral galaxy and Caldwell object in the constellation Canes Venatici. It shines at magnitude +10.2/+10.6. Its celestial cooridinates are RA 12h
17.5m, dec +37� 49′. It is located near a naked-eye G-class star Beta Canum Venaticorum, barred spiral galaxy NGC 4151, and irregular galaxy NGC 4214. The galaxy lies approximately 6.5
million[1]/14 million[2] light years away, with a redshift of +243/493[1] km/s. A nuclear star cluster and halo is located at the centre of this galaxy.[2][3]
- Wiki
captured using CGE Computerized Mount
submitted by John_Buonomo
Messier 3 (also known as M3 or NGC 5272) is a globular cluster in the constellation Canes Venatici. It was discovered by Charles Messier in 1764, and resolved into stars by William Herschel
around 1784. This cluster is one of the largest and brightest, and is made up of around 500,000 stars. It is located at a distance of about 33,900 light-years away from Earth. M3 has an apparent
magnitude of 6.2, making it visible to the naked eye under dark conditions. From a moderate-sized telescope, the cluster is fully defined.
- Wiki
captured using CGE Computerized Mount
submitted by John_Buonomo
Messier 67 (also known as M67 or NGC 2682) is an open cluster, or galactic cluster, in the constellation Cancer. M67's Trumpler class is variously given as II 2 r, II 2 m, or II 3 r. It was
discovered by Johann Gottfried Koehler in 1779. Its age is estimated at between 3.2 and 5 billion years. The most recently estimated age of four billion years appears to be the most
reliable[citation needed]; thus the stars of M67 are most likely slightly younger than the Sun.
M67 is not the oldest known open cluster, but there are very few in the galaxy known to be older. M67 is an important laboratory for studying stellar evolution, since all its stars are at the
same distance and age, except for approximately 30 anomalous blue stragglers[1], whose origins are not fully understood.
M67 is one of the most-studied open clusters, yet estimates of its physical parameters such as age, mass, and number of stars of a given type, vary substantially. Richer et al. [2] estimate its
age to be 4 Gyr, its mass to be 1080 solar masses, and the number of white dwarfs to be 150. Hurley et al. [3] estimate its current mass to be 1400 solar masses and its initial mass to be
approximately 10 times as great.
M67 has more than 100 stars similar to the Sun, and many red giants. The total star count has been estimated at over 500[citation needed]. The cluster contains no main sequence stars bluer than
spectral type F, other than perhaps some of the blue stragglers, since the brighter stars of that age have already left the main sequence. In fact, when the stars of the cluster are plotted on
the Hertzsprung-Russell diagram, there is a distinct "turn-off" representing the stars which are just about to leave the main sequence and become red giants. As the cluster ages, the turn-off
will move down the main sequence.
It appears that M67 does not contain an unbiased sample of stars. One cause of this is mass segregation, the process by which lighter stars (actually, systems) gain speed at the expense of more
massive stars during close encounters, which causes the lighter stars to be at a greater average distance from the center of the cluster or to escape altogether[4
- WIKI
captured using CGE Computerized Mount
submitted by John_Buonomo
M65 and M66 galaxies with Edge HD8 on CGE guided with MetaGuide OAG. Un-Mod Canon 20d. Capture and processing with ImagesPlus
captured using CGE Computerized Mount
submitted by FrankMG