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Elephant Trunk Nebula HST

Elephant Trunk Nebula

Elephant Trunk Nebula

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII/SII
Exposure:15×600 Ha and 10×600 OIII/SII all 2bin
25 August 2016

The Elephant’s Trunk nebula is a concentration of interstellar gas and dust within the much larger ionized gas region IC 1396 located in the constellation Cepheus about 2,400 light years away from Earth. The piece of the nebula shown here is the dark, dense globule IC 1396A; it is commonly called the Elephant’s Trunk nebula because of its appearance at visible light wavelengths, where there is a dark patch with a bright, sinuous rim. The bright rim is the surface of the dense cloud that is being illuminated and ionized by a very bright, massive star (HD 206267) that is just to the west of IC 1396A. (In the Figure above, the massive star is just to the left of the edge of the image.) The entire IC 1396 region is ionized by the massive star, except for dense globules that can protect themselves from the star’s harsh ultraviolet rays.
The Elephant’s Trunk nebula is now thought to be a site of star formation, containing several very young (less than 100,000 yr) stars that were discovered in infrared images in 2003. Two older (but still young, a couple of million years, by the standards of stars, which live for billions of years) stars are present in a small, circular cavity in the head of the globule. Winds from these young stars may have emptied the cavity.
The combined action of the light from the massive star ionizing and compressing the rim of the cloud, and the wind from the young stars shifting gas from the center outward lead to very high compression in the Elephant’s Trunk nebula. This pressure has triggered the current generation of protostars@Wiki

La nébuleuse de la trompe est une concentration de gaz interstellaire et de poussières dans la grande région de gaz ionisé IC 1396 situé dans la constellation de Céphée environ 2400 années-lumière de la Terre.
La nébuleuse de la trompe est maintenant considéré comme un site de formation d’étoiles, contenant plusieurs (moins de 100 000 an) étoiles très jeunes.

 

A starless versin of the Elephant Trank nebula

VdB142starless

A two panel mosaic

VdB142_mosa_webVdB142starless

The starless version of the two panel mosaic

VdB142_mosa_starless


Crescent Nebula bicolor

Crescent Nebula bicolor

Crescent Nebula bicolor

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII
Exposure:39×600 Ha and OIII all 2bin
12 August 2016

My second attempt to take a deepsky photo of this nebula. My first attempt

The Crescent Nebula (also known as NGC 6888, Caldwell 27, Sharpless 105) is an emission nebula in the constellation Cygnus, about 5000 light-years away from Earth. It was discovered by Friedrich Wilhelm Herschel in 1792. It is formed by the fast stellar wind from the Wolf-Rayet star WR 136 (HD 192163) colliding with and energizing the slower moving wind ejected by the star when it became a red giant around 250,000 to 400,000[citation needed] years ago. The result of the collision is a shell and two shock waves, one moving outward and one moving inward. The inward moving shock wave heats the stellar wind to X-ray-emitting temperatures.

It is a rather faint object located about 2 degrees SW of Sadr. For most telescopes it requires a UHC or OIII filter to see. Under favorable circumstances a telescope as small as 8 cm (with filter) can see its nebulosity. Larger telescopes (20 cm or more) reveal the crescent or a Euro sign shape which makes some to call it the “Euro sign nebula”.@wiki

La nébuleuse du Croissant (NGC 6888) est une nébuleuse en émission située dans la constellation du Cygne, à environ 5 000 années-lumière2. Elle est issue des rapides vents solaires créés par l’étoile Wolf-Rayet WR 136 (en), qui -par collision- ionisent les vents plus lents de cette même étoile lorsqu’elle était plus jeune et plus petite (de type géante rouge) il y a 400 000 ans. Le front de choc engendre ce que l’on nomme une bulle de Wolf-Rayet.@wiki

A version with stronger backround dust

ngc6888_bicolor

At last a wide field version taken in 2013 with the 180 Epsilon ant the QHY 12 camera.

Crescent Nebula wide field

Crescent Nebula wide field


M27 Dumbbell Nebula

M27 Dumbbell Nebula HST bicolor starless

M27 Dumbbell Nebula
HST bicolor starless

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII/SII
Exposure:30×600 Ha and OIII all 2bin
07 August 2016

The Dumbbell Nebula (also known as Apple Core Nebula, Messier 27, M 27, or NGC 6853) is a planetary nebula in the constellation Vulpecula, at a distance of about 1,360 light-years.
This object was the first planetary nebula to be discovered; by Charles Messier in 1764. At its brightness of visual magnitude 7.5 and its diameter of about 8 arcminutes
The Dumbbell Nebula appears to be shaped like an prolate spheroid and is viewed from our perspective along the plane of its equator. In 1992, Moreno-Corral et al. computed that its rate of expansion in the plane of the sky was no more than 2.3″ per century. From this, an upper limit to the age of 14,600 yr may be determined. In 1970, Bohuski, Smith, and Weedman found an expansion velocity of 31 km/s. Given its semi-minor axis radius of 1.01 ly, this implies that the kinematic age of the nebula is some 9,800 years.@ Wiki

La nébuleuse de l’Haltère est une nébuleuse planétaire située dans la constellation du Petit Renard à environ 264 pc . Cette nébuleuse, découverte par Charles Messier le 12 juillet 1764, est la première nébuleuse planétaire observée de l’histoire de l’astronomie. Elle porte le numéro 27 de son catalogue.
Cet objet est particulièrement brillant et possède un diamètre apparent très large, puisque la partie la plus lumineuse atteint 1/5 de celui de la Lune. Sachant que la vitesse d’expansion atteint 6,8 secondes d’arc par siècle, son âge est estimé à 3000 ou 4000 ans.
L’étoile centrale (à l’origine de la nébuleuse) a une magnitude apparente de 13,5, ce qui la rend difficilement observable pour un astronome amateur. C’est une naine blanche de couleur bleue très chaude (85 000K). Elle est peut-être accompagnée d’une autre étoile, encore plus faible (magnitude 17), à 6,5 secondes d’arc de distance apparente.
La forme particulière de la partie lumineuse a valu à cette nébuleuse le nom de Nébuleuse de l’Haltère (Dumbbell en anglais). On lui connaît également les surnoms de Trognon de pomme, de Sablier (attention à la confusion avec d’autres objets !) voire de Diabolo.

A starless version of the Dumbbell Nebula
M27-starless


NGC 2175 SHO Monkey Head Nebula

NGC2175-SHO

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII/SII
Exposure:14×600 Ha, 7×600 OIII/SII all 2bin
30 January 2016

Open Cluster NGC 2175 (also known as OCL 476 or Cr 84) is an open cluster in the Orion constellation, embedded in a diffusion nebula. It was discovered by Giovanni Batista Hodierna before 1654 and independently discovered by Karl Christian Bruhns in 1857. NGC 2175 is at a distance of about 6,350 light years away from Earth.
The nebula surrounding it is Sharpless catalog Sh 2-252.
There is some equivocation in the use of the identifiers NGC 2174 and NGC 2175. These may apply to the entire nebula, to its brightest knot, or to the star cluster it includes. Burnham’s Celestial Handbook lists the entire nebula as 2174/2175 and does not mention the star cluster. The NGC Project (working from the original descriptive notes) assigns NGC 2174 to the prominent knot at J2000 06h 09m 23.7s, +20° 39′ 34″ and NGC 2175 to the entire nebula, and by extension to the star cluster. Simbad uses NGC 2174 for the nebula and NGC 2175 for the star cluster. @wikipedia

NGC 2175 (également connu sous le nom de nébuleuse de la Tête de singe, OCL 476 ou encore de Cr 84) est un amas ouvert dans la constellation d’Orion. Il a été découvert par Giovanni Battista Hodierna peu avant 1654. De façon indépendante, Karl Christian Bruhns le découvrit en 1857. NGC 2175 se trouve à environ 6 350 années-lumière de la Terre. Il est entouré par la nébuleuse Sh 2-252 @wikipedia


M8 Lagoon Nebula SHO

M8_SHO_neu

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII/SII
Exposure:20×600 Ha, 12×600 OIII/SII all 2bin
14 July 2015

The Lagoon Nebula is estimated to be between 4,000-6,000 light years from the Earth. In the sky of Earth, it spans 90′ by 40′, translates to an actual dimension of 110 by 50 light years. Like many nebulas, it appears pink in time-exposure color photos but is gray to the eye peering through binoculars or a telescope, human vision having poor color sensitivity at low light levels. The nebula contains a number of Bok globules (dark, collapsing clouds of protostellar material), the most prominent of which have been catalogued by E. E. Barnard as B88, B89 and B296. It also includes a funnel-like or tornado-like structure caused by a hot O-type star that emanates ultraviolet light, heating and ionizing gases on the surface of the nebula. The Lagoon Nebula also contains at its centre a structure known as the Hourglass Nebula (so named by John Herschel), which should not be confused with the better known Hourglass Nebula in the constellation of Musca. In 2006 the first four Herbig–Haro objects were detected within the Hourglass, also including HH 870. This provides the first direct evidence of active star formation by accretion within it. @wiki

La nébuleuse a été découverte en 1747 par Guillaume Le Gentil et intégra le catalogue de Messier en 1764. John Herschel découvrit que la région la plus brillante de la nébuleuse avait une forme de sablier. Cette région a été observée par le télescope Hubble en 1997, celle-ci étant considérée comme le lieu de la formation d’étoiles. En 1890, Agnès Clerke lui donna son nom de « nébuleuse de la lagune ».
La nébuleuse de la lagune est un immense nuage d’hydrogène et de poussières éclairé par une supergéante bleue, l’étoile 9 du Sagittaire. La taille de la nébuleuse est d’environ 110 années-lumière et sa distance tourne autour de 5000 années lumière ce qui lui donne un diamètre apparent trois fois plus important que celui de la pleine Lune. La nébuleuse, comme de nombreuses nébuleuses diffuses, contient un bel amas ouvert, NGC 6530, issu de la nébuleuse, d’étoiles jeunes et très chaudes de type O et B âgées de seulement 2 millions d’années. La région du sablier, éclairée par l’étoile Herschel 36, est suspectée d’être le lieu de naissance d’étoiles.
Du fait de sa magnitude 5, la nébuleuse est visible à l’œil nu. La taille apparente très importante de l’objet impose de faire attention au grossissement employé pour l’observer. Si vous avez un télescope ou une lunette astronomique utilisez l’oculaire ayant la distance focale la plus importante (20 mm par exemple). L’utilisation d’un filtre UHC, très efficace pour ce type de nébuleuse, vous permettra sans doute d’observer la nébuleuse avec plus de détails.@wiki


Mosaik of the Soul Nebula

Mosaik of SoulNebula SHO

Mosaik of SoulNebula SHO

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII/SII
Exposure:9×3,5h HA/SII/OIII all 2bin
Oct-Nov 2014

A starless version of the Soul Nebula

SoulNebula starless version

 


Tulip Nebula Sh2-101 SHO

SH2-101-SHO_hp_neu

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII/SII
Exposure:15×600 Ha, 10×600 OIII/SII all2bin
27 September 2014

The Tulip Nebula, or Sharpless 101 (Sh2-101) or the Cygnus Star Cloud is a H II region emission nebula located in the constellation Cygnus. It is so named because it appears to resemble the outline of a tulip when imaged photographically. It was catalogued by astronomer Stewart Sharpless in his 1959 catalog of nebulae. It lies at a distance of about 6,000 light-years (5.7×1016 km; 3.5×1016 mi) from Earth.@wikipedia

La nébuleuse de la tulipe se trouve à 8000 années-lumière en direction de la constellation du Cygne. L’image composite ( SHO ) ci-dessus cartographie l’émission de soufre ionisé (rouge), d’hydrogène (vert) et d’atomes d’oxygène (bleu). Le rayonnement ultraviolet de la jeune étoile HDE 227018 (près de l’arc bleu au centre de l’image) ionise les atomes et alimente l’émission de la nébuleuse de la tulipe.


Crescent Nebula

NGC6888_ha_OIII_hp

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII
Exposure:35x900sec Ha, 27x600sec
18 August 2013

The Crescent Nebula (also known as NGC 6888, Caldwell 27, Sharpless 105) is an emission nebula in the constellation Cygnus, about 5000 light-years away. It was discovered by Friedrich Wilhelm Herschel in 1792. It is formed by the fast stellar wind from the Wolf-Rayet star WR 136 (HD 192163) colliding with and energizing the slower moving wind ejected by the star when it became a red giant around 250,000[3] to 400,000[citation needed] years ago. The result of the collision is a shell and two shock waves, one moving outward and one moving inward. The inward moving shock wave heats the stellar wind to X-ray-emitting temperatures.
It is a rather faint object located about 2 degrees SW of Sadr. For most telescopes it requires a UHC or OIII filter to see. Under favorable circumstances a telescope as small as 8cm (with filter) can see its nebulosity. Larger telescopes (20cm or more) reveal the crescent or a Euro sign shape which makes some to call it the “Euro sign nebula”. @Wikipedia

 

La nébuleuse du Croissant (NGC 6888) est une nébuleuse en émission située dans la constellation du Cygne, à environ 5 000 années-lumière2. Elle est issue des rapides vents solaires créés par l’étoile Wolf-Rayet WR 136, qui -par collision- ionisent les vents plus lents de cette même étoile lorsqu’elle était plus jeune et plus petite (de type géante rouge) il y a 400 000 ans. Le front de choc engendre ce que l’on nomme une bulle de Wolf-Rayet. @Wikipedia


Cocoon Nebula 2014

IC5146_LRGB_web

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonLRGB
Exposure: 10×600 sec Lum/7×300 sec RGB 2xbin
18 August 2014

IC 5146 (also Caldwell 19, Sh 2-125, and the Cocoon Nebula) is a reflection/emission nebula and Caldwell object in the constellation Cygnus. The NGC description refers to IC 5146 as a cluster of 9.5 mag stars involved in a bright and dark nebula. The cluster is also known as Collinder 470. It shines at magnitude +10.0/+9.3/+7.2. Its celestial coordinates are RA 21h 53.5m, dec+47° 16′. It is located near the naked-eye star Pi Cygni, the open cluster NGC 7209 in Lacerta, and the bright open cluster M39.[1][4] The cluster is about 4,000 ly away, and the central star that lights it formed about 100,000 years ago; the nebula is about 12 arcmins across, which is equivalent to a span of 15 light years @Wikipedia

IC 5146 est composé d’une nébuleuse en émission et un amas ouvert situés à environ 4 000 années-lumière de la Terre dans la constellation du Cygne1. Il a un diamètre d’environ 15 années-lumière.
Elle se trouve près du bord Est de la constellation, près de celle du Lézard, en plein dans la Voie lactée, à une heure en AD de la Nébuleuse de l’Amérique du Nord. Elle est située à l’extrémité de la nébuleuse obscure Barnard 1681.
Elle est également une zone de formation d’étoiles @Wikipedia


Soap Bubble Nebula


SoapBubble-web

SoapBubble-crop-web
Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon HA OIII
Exposure: 10×600 sec Ha/OIII 2bin
22 August 2014

The Soap bubble nebula, or PN G75.5+1.7, is a planetary nebula in the constellation Cygnus, near the Crescent Nebula (NGC 6888). It was discovered by amateur astronomer Dave Jurasevich using an Astro-Physics 160 mm refractor telescope who imaged the nebula on June 19, 2007 and on July 6, 2008. The nebula was later independently noted and reported to the International Astronomical Union by Keith. B. Quattrocchi and Mel Helm who imaged PN G75.5+1.7 on July 17, 2008 @Wikipedia

La Nébuleuse de la Bulle de Savon ou PN G75.5 1.7, est une nébuleuse planétaire dans la constellation du Cygne1, dans la Nébuleuse du Croissant (NGC 6888). Elle fut découverte le 5 juillet 2010 par un astronome amateur nommé Dave Jurasevic @Wikipedia


Snapshot of the Orion Nebula

M42_HDR_centre_hf-1440x1339
Optics/mount: 180 Epsilon f2,8 Takahashi Alt-5

Camera/filters: QHY12 OSC

Exposure:10x600sec and 9x10sec , 9 January 2013

The Orion Nebula (also known as Messier 42, M42, or NGC1976) is a diffuse nebula situated south[b] of Orion’s Belt in the constellation of Orion. 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 1,344 ± 20 light years and is the closest region of massive star formation to Earth. The M42 nebula is estimated to be 24 light years across. It has a mass of about 2000 times the mass of the Sun. Older texts frequently refer to the Orion Nebula as the Great Nebula in Orion or the Great Orion Nebula.

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. 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 the hydrogen clouds of the Orion Nebula. Each bullet is ten times the diameter of Pluto’s orbit and tipped with iron atoms glowing bright blue. They were probably formed one thousand years ago from an unknown violent event.

Grand champ

Grand champ

La nébuleuse d’Orion, aussi connue sous le nom de M42 ou NGC 1976, est une nébuleuse en émission/réflexion située au cœur de la constellation d’Orion.

C’est la nébuleuse diffuse la plus brillante : elle est visible à l’œil nu dans un ciel nocturne sans pollution lumineuse et peut être facilement vue avec une paire de jumelles. Elle couvre dans le ciel une zone de 66 × 60 minutes d’arc ; c’est-à-dire quatre fois plus que la pleine lune.

La nébuleuse d’Orion est la partie principale d’un nuage de gaz et de poussières appelé le « nuage d’Orion ». Ce nuage s’étend sur près de la moitié de la constellation et contient aussi la Boucle de Barnard et la célèbre nébuleuse de la Tête de Cheval.

La nébuleuse a une taille d’environ 33 années-lumière. Il aura fallu attendre 2007 pour s’apercevoir que la nébuleuse se trouve à environ 1 350 années-lumière de la Terre au lieu des 1 500 années-lumière jusque-là estimées. Elle contient un amas ouvert très jeune contenant de nombreuses étoiles.


vdB152 Reflection Nebula in Cepheus

VDB152

Optics/mount: 180 Epsilon f2,8 Takahashi Alt-5
Camera/filters: QHY12 OSC
Exposure: 24x900sec / 6.00 h, 16 October 2012

Described as a “dusty curtain” or “ghostly apparition”, mysterious reflection nebula vdB 152 really is very faint. It lies about 1400 light-years away, along the northern Milky Way in the royal constellation Cepheus. Near the edge of a large molecular cloud, pockets of cosmic dust in the region block light from background stars or scatter light from the embedded bright star (top) giving parts of the nebula a characteristic blue color. Ultraviolet light from the star is also thought to cause a dim reddish luminescence in the nebular dust. Though stars do form in molecular clouds, this star seems to have only accidentally wandered into the area, as its measured velocity through interstellar space is very different from the cloud’s velocity. This deep telescopic image spans about 7 light-years at the estimated distance of vdB 152. (http://apod.nasa.gov/apod/ap070614.html)


Iris Nebula Widefield

Iris Nebula

Optics/mount: 180 Epsilon f2,8 Takahashi Alt-5
Camera/filters: QHY12 OSC
exposure: 38×1200 sec / 12,6h

The Iris Nebula, also NGC 7023 and Caldwell 4, is a bright reflection nebula and Caldwell object in the constellation Cepheus. NGC 7023 is actually the cluster within the nebula, LBN 487, and the nebula is lit by a magnitude +7 star, SAO 19158.[1] It shines at magnitude +6.8. It is located near the Mira-type variable star T Cephei, and near the bright magnitude +3.23 variable star Beta Cephei (Alphirk). It lies 1,300 light-years away and is six light-years across.


Veil Nebula NGC6960

Veil Nebula

This image is a combination of LRGB frames and halpha and OIII mixed to the redchannel and the bluechannel


Image in HST-palette

Veilnebula LRGB

This is the “classic LRGB” version

The Veil Nebula is a cloud of heated and ionized gas and dust in the constellation Cygnus. It constitutes the visible portions of the Cygnus Loop (radio source W78, or Sharpless 103), a large but relatively faint supernova remnant. The source supernova exploded some 5,000 to 8,000 years ago, and the remnants have since expanded to cover an area roughly 3 degrees in diameter (about 6 times the diameter, or 36 times the area, of the full moon). The distance to the nebula is not precisely known, but recent evidence from the Far Ultraviolet Spectroscopic Explorer (FUSE) supports a distance of about 1,470 light-year

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB halpha/OIII 5nm
Exposure: 5h LRGB 10min subs all 1xbin Ha/OIII 6h
26/07/2012


Revision of NGC 3718

NGC3718

NGC3718

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB
Exposure: 37×600 Lum, 12×600 RGB all 1bin
23-24 March 2012

I did some changes with the processing to make the background less noisy

Discovered by W. Herschel in April 1789 NGC 3718 is located in the constellation of the big dipper and is to be categorized as a Seyfert galaxy. It holds 8.2 by 3.5 arc minutes and appears to be 10m6 bright for the visual observer. While the galaxy is in a distance of some 52 Mio light years from earth, it’s warped spiral shape is pertubated by the neighbourghing galaxy NGC 3729, which is devided from 3718 by 150000 light years. Both are therefor interacting in a gravitational way, like the fainter galaxy couple south to 3718. These group of galaxies (Hickson 56 by name) is more than 400 Mio lightyears away from our planet.


NGC 4216

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB
Exposure: 49×600 Lum, 9×600 RGB all 1bin
26 March 2012

NGC 4216 is a metal-rich intermediate spiral galaxy located not far from the center of the Virgo Cluster] of galaxies, roughly 40 million light-years away.


NGC3718

NGC3718 alt

NGC3718 alt

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB
Exposure: 37×600 Lum, 12×600 RGB all 1bin
23-24 March 2012

Discovered by W. Herschel in April 1789 NGC 3718 is located in the constellation of the big dipper and is to be categorized as a Seyfert galaxy. It holds 8.2 by 3.5 arc minutes and appears to be 10m6 bright for the visual observer. While the galaxy is in a distance of some 52 Mio light years from earth, it’s warped spiral shape is pertubated by the neighbourghing galaxy NGC 3729, which is devided from 3718 by 150000 light years. Both are therefor interacting in a gravitational way, like the fainter galaxy couple south to 3718. These group of galaxies (Hickson 56 by name) is more than 400 Mio lightyears away from our planet.


M 100 Galaxy

M100_DBE-lrgb-ps_cropM100_DBE-lrgb-ps2
Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB
Exposure: 49×600 Lum, 9×600 RGB all 1bin
16 March 2012

Messier 100 (also known as NGC 4321) is an example of a grand design spiral galaxy located within the southern part of constellation Coma Berenices. It is one of the brightest galaxies in the Virgo cluster, approximately 55 million light-years distant from Earth and has a diameter of 160,000 light years. It was discovered by Pierre Méchain on March 15, 1781 and was subsequently entered in Messier’s catalogue of nebulae and star clusters after Charles Messier made observations of his own on April 13, 1781. The galaxy was one of the first spirals discovered, and was listed as 1 of 14 spiral nebulae by Lord William Parsons of Rosse in 1850. A satellite galaxy named NGC 4323 is present within M100.

Some galaxies near by M100

M100-GX


Hickson 44

Hickson 44

Hickson 44

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB
Exposure: 49×600 Lum, 9×600 RGB all 1bin

Hickson 44 is a cluster of four gravitationally bound galaxies that lie relatively nearby to our own Milky Way. Each of these galaxies shows signs of interaction, such warped disks or a large bright bar. The entire grouping spans 15′, small enough to be seen together in the same field of view. The brightest member is NGC 3190, the smaler Gx are NGC 3193 and NGC 3185 nearly-face-on barred spiral. The faintest member is the 14th magnitude NGC 3187, a spiral galaxy with a bright bar.


Black Eye Galaxy

M64 Black Eye Galaxy

M64 Black Eye Galaxy

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB
Exposure: 10×600 Lum, 5×600 RGB all 1bin
02 March 2012

The Black Eye Galaxy (also called Sleeping Beauty Galaxy; designated Messier 64, M64, or NGC 4826) was discovered by Edward Pigott in March 1779, and independently by Johann Elert Bode in April of the same year, as well as by Charles Messier in 1780. It has a spectacular dark band of absorbing dust in front of the galaxy’s bright nucleus, giving rise to its nicknames of the “Black Eye” or “Evil Eye” galaxy. M64 is well known among amateur astronomers because of its appearance in small telescopes. It is a spiral galaxy in the Coma Berenices constellation

Zoom

M64 Zoom

M64 Zoom


M78 with the 12″ACF

M78-12lrgb-ps_hf

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB
Exposure: 20×600 Lum, 12×600 RGB all 1bin
16/01/2012 – 18/01/2012

M78 (ou NGC 2068) est une nébuleuse diffuse située dans Orion et découverte en 1780 par Pierre Méchain. C’est la nébuleuse diffuse la plus brillante du ciel. Charles Messier l’ajouta à son catalogue le 17 décembre de la même année.@Wikipedia

The nebula Messier 78 (also known as M 78 or NGC 2068) is a reflection nebula in the constellation Orion. It was discovered by Pierre Méchain in 1780 and included by Charles Messier in his catalog of comet-like objects that same year.

M78 is the brightest diffuse reflection nebula of a group of nebulae that include NGC 2064, NGC 2067 and NGC 2071. This group belongs to the Orion Molecular Cloud Complex and is about 1,600 light years distant from Earth. M78 is easily found in small telescopes as a hazy patch and involves two stars of 10th magnitude. These two stars, HD 38563A and HD 38563B, are responsible for making the cloud of dust in M78 visible by reflecting their light.

About 45 variable stars of the T Tauri type, young stars still in the process of formation as well as some 17 Herbig–Haro objects are known in M78.@Wikipedia


NGC 1333 Reflection Nebula

NGC1333-Th-px-ps

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB HA5nm
Exposure: 22×600 Lum, 5×600 RGB all 1bin

NGC 1333 is catalogued as a reflection nebula but is actually a diverse region and part of the Perseus OB2 molecular cloud complex. It is one of the nearest star forming regions and particularly rich in young stellar objects (YSOs). Stellar clusters are born embedded within molecular clouds and during their early evolution as YSOs are often only visible at infrared wavelengths, being heavily obscured by dust. Four classes of young stellar objects have been described. Class I though III objects progress through an evolutionary sequence of being less dust enshrouded, as they develop towards the zero-age main sequence. The earliest and most imbedded stage of star formation is the class 0 YSOs. These earliest protostars are difficult to detect due to their heavily imbedded nature. Less than 50 Class 0 objects are known however 4 of these low mass protostars exist in NGC 1333. Also 36 Herbig-Haro obejects have been identified in NGC 1333 confirming its status as a young active region of star formation. Herbig-Haro objects are collisionally excited nebulae produced by outflows ejected by YSOs. They are produced mainly during the first few hundred thousand years of life of a YSO and are usually highly obscured by the cloud core environment from which they formed.

The gaseous structure of NGC 1333 has been mapped at radio wavelengths and appears to support the large scale star formation observed. Lumpy and filamentary cloud structure exists in NGC 1333 indicative of recent collapse and fragmentation of the parent molecular cloud leading to the clustered mode of star formation observed in the nebula. In addition a series of cavities and shells exist presumably blown out by the outflows of infant protostars. Infrared surveys reveal the presence of YSOs at the edge of these cavities indicating that sequential star formation has occurred there and has been triggered by the effects of the powerful outflows from the first generation of stars. The entire process is extremely recent as the cloud hosting NGC 1333 is less than a million years old.’

NGC 1333 est une nébuleuse par réflexion située dans la constellation de Persée. Elle appartient au nuage moléculaire Persée.
En 2011, des chercheurs ont signalé la découverte de 30 à 40 objets de type naines brunes dans ce nuage et dans le complexe de nuage Rho Ophiuchi@Wikipedia


VDB 141 Ghost nebula

VDB 141

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB HA5nm
Exposure: 20×600 Lum, 8×600 RGB all 1bin

VdB 141 is a reflection nebula located in the constellation Cepheus. Sometimes referred to as the ghost nebula, its awkward name is its catalog number in Sidney van den Bergh’s catalog of reflection nebulae, published in 1966. Several stars are embedded in the nebula. Their light gives it a ghoulish brown color. North is down and East is to the right. Imaged August 28, 2009.


M8 M20 with the QHY12

M8 M20

Optics/mount: 180 Epsilon f2,8 Takahashi Alt-5
Camera/filters: QHY12 OSC
exposure: 22×600 sec

Lagoon nebula (catalogued as Messier 8 or M8, and as NGC 6523) is a giant interstellar cloud in the constellation Sagittarius. It is classified as an emission nebula and as an H II region.

The Lagoon Nebula was discovered by Guillaume Le Gentil in 1747 and is one of only two star-forming nebulae faintly visible to the naked eye from mid-northern latitudes. Seen with binoculars, it appears as a distinct oval cloudlike patch with a definite core. A fragile star cluster appears superimposed on it.

The Trifid Nebul(catalogued as Messier 20 or M20 and as NGC 6514) is an H II region located in Sagittarius. Its name means ‘divided into three lobes’. The object is an unusual combination of an open cluster of stars, an emission nebula (the lower, red portion), a reflection nebula (the upper, blue portion) and a dark nebula (the apparent ‘gaps’ within the emission nebula that cause the trifid appearance; these are also designated Barnard 85). Viewed through a small telescope, the Trifid Nebula is a bright and colorful object, and is thus a perennial favorite of amateur astronomers