Amateur Astrophotographie Landos France

Nebulas

Eastern Veil Nebula SHO

EasternVeilNebula_match-pick-web

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
04 September 2014

The Veil Nebula itself is a large supernova remnant, the expanding debris cloud from the death explosion of a massive star. While the Veil is roughly circular in shape covering nearly 3 degrees on the sky in the constellation Cygnus, this portion of the eastern Veil spans only 1/2 degree, about the apparent size of the Moon. That translates to 12 light-years at the Veil’s reassuring estimated distance of 1,400 light-years from planet Earth. In the composite of image data recorded through narrow band filters, emission from hydrogen atoms in the remnant is shown in red with strong emission from oxygen atoms in blue-green hues.

NGC 6995 est la partie la plus méridionale de la nébuleuse Cirrus dans la constellation du Cygne. NGC 6995 a une luminosité de 7,00 mag et un diamètre de 12 minutes d’arc.


Pickering’s Triangle SHO

Pickering_triangle-web

 

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII/SII
Exposure:12×600 Ha, 7×600 OIII/SII all2bin
03 September 2014

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 Far Ultraviolet Spectroscopic Explorer (FUSE) data supports a distance of about 1,470 light-years.

In modern usage, the names Veil Nebula, Cirrus Nebula, and Filamentary Nebula generally refer to all the visible structure of the remnant, or even to the entire loop itself. The structure is so large that several NGC numbers were assigned to various arcs of the nebula.[4] There are three main visual components:

The Western Veil (also known as Caldwell 34), consisting of NGC 6960 (the “Witch’s Broom”, “Finger of God”, or “Filamentary Nebula”) near the foreground star 52 Cygni;
The Eastern Veil (also known as Caldwell 33), whose brightest area is NGC 6992, trailing off farther south into NGC 6995 and IC 1340; and
Pickering’s Triangle (or Pickering’s Triangular Wisp), brightest at the north central edge of the loop, but visible in photographs continuing toward the central area of the loop.@wikipedia

Le Triangle de Pickering se trouve quant à lui au nord-ouest de la nébuleuse. Comme son nom l’indique en partie, il s’agit d’un triangle filamenteux allongé en direction du sud sur environ 45 minutes d’arc (pour une base de 25′ de largeur). Il partage avec la Petite Dentelle la désignation de NGC 6960. Le Triangle de Pickering se prolonge par un long filament de plus de deux degrés de long.


The Wall NGC7000 in SHO

The Wall

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII/SII
Exposure:125×600 Ha, 10×600 OIII/SII all2bin
02 September 2014

The North America Nebula (NGC 7000 or Caldwell 20) is an emission nebula in the constellation Cygnus, close to Deneb (the tail of the swan and its brightest star). The remarkable shape of the nebula resembles that of the continent of North America, complete with a prominent Gulf of Mexico. It is sometimes incorrectly called the “North American Nebula.
Cygnus’s Wall is a term for the “Mexico and Central America part” of the North America Nebula. The Cygnus Wall exhibits the most concentrated star formations in the nebula. @wikipedia

La nébuleuse de l’Amérique du Nord (ou NGC 7000 ou nebula North America) est une nébuleuse en émission située à environ 580 pc (1 890 a.l.) dans la constellation du Cygne, près de Alpha Cygni1. Elle a une taille environ 15 pc (48,9 a.l.)
La forme de la nébuleuse fait penser à celle de l’Amérique du Nord, d’où son nom.


Pelican Nebula SHO

Pelikan-SHO_web

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 AstrodonHa/OIII/SII
Exposure:12×600 Ha, 7×600 OIII/SII all2bin
28 August 2014

The Pelican Nebula (also known as IC 5070 and IC 5067) is an H II region associated with the North America Nebula in the constellation Cygnus. The gaseous contortions of this emission nebula bear a resemblance to a pelican, giving rise to its name. The Pelican Nebula is located nearby first magnitude star Deneb, and is divided from its more prominent neighbour, the North America Nebula, by a molecular cloud filled with dark dust.

The Pelican is much studied because it has a particularly active mix of star formation and evolving gas clouds. The light from young energetic stars is slowly transforming cold gas to hot and causing an ionization front gradually to advance outward. Particularly dense filaments of cold gas are seen to still remain, and among these are found two jets emitted from the Herbig–Haro object 555. Millions of years from now this nebula might no longer be known as the Pelican, as the balance and placement of stars and gas will leave something that appears completely different. @wikipedia

IC 5067/70 est une très grande nébuleuse en émission (2,5 fois le diamètre de la pleine Lune). Elle se nomme aussi la ‘nébuleuse du Pélican.
Elle se trouve juste à côté de la très grande et célèbre NGC 7000 (la nébuleuse de l’Amérique du Nord). Elle doit être observée aux jumelles. Attention, sa puissante voisine atténue un peu la beauté de cette nébuleuse.


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.


vdB149-150 Refelction Nebula in Cepheus

VDB149

VDB149

Optics/mount: 180 Epsilon f2,8 Takahashi Alt-5
Camera/filters: QHY12 OSC
Exposure:59x900sec 14,7h


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)


Dark Nebula Banard 171-174

Dark nebula

Optics/mount: 180 Epsilon f2,8 Takahashi Alt-5
Camera/filters: QHY12 OSC
Exposure: 20x900sec / 5.00 h, 9 Sept 2012


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


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


M16 Eagle Nebula

M 16 Eagel Nebula

M16

Optics/mount: 180 Epsilon f2,8 Takahashi Alt-5
Camera/filters: QHY12 OSC
exposure: 14×800 sec

The Eagle Nebula (catalogued as Messier 16 or M16, and as NGC 6611) is a young open cluster of stars in the constellation Serpens, discovered by Jean-Philippe de Cheseaux in 1745-46. Its name derives from its shape which is resemblant of an eagle. It is the subject of the famous “Pillars of Creation” photograph by the Hubble Space Telescope, which shows pillars of star-forming gas and dust within the nebula

 


NGC 7133/ 7129

Reflexions nebula

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

NGC 7129 is a young compact star forming region which displays an unusual patchwork of colorful nebulosity and bright stars contrasted against the dust clouds of the Milky Way. The astronomical correlate of those colors and textures is the rich interplay that occurs between young stars and the surrounding interstellar medium. NGC 7129 contains several bright reflection nebulae including the large blue reflection cloud NGC 7133 and the unusual small yellow reflection cloud LBN497. Also conspicuous in the field are several bright Herbig-Haro objects, the signatures of young stellar objects soon to emerge in the main sequence. The dominant blue reflection nebula,


Witch Head Nebula IC2118

Wich head nebula

Wich head nebula

Optics/mount: 180 Epsilon f2,8 Takahashi Mount Alt-5ADN
Camera/filters:QHY 12
exposure: 20×900 sec

IC 2118 (also known as Witch Head Nebula due to its shape), is an extremely faint reflection nebula believed to be an ancient supernova remnant or gas cloud illuminated by nearby supergiant star Rigel in Orion. It lies in the Eridanus constellation, about 900 light-years from Earth. The nature of the dust particles, reflecting blue light better than red, is a factor in giving the Witch Head its blue color. Radio observations show substantial carbon monoxide emission throughout parts of IC 2118 an indicator of the presence of molecular clouds and star formation in the nebula. In fact candidates for pre-main sequence stars and some classic T-Tauri stars have been found deep within the nebula.[1]

The molecular clouds of IC 2118 are probably juxtaposed to the outer boundaries of the vast Orion-Eridanus bubble, a giant supershell of molecular hydrogen blown by the high mass stars of the Orion OB1 association. As the supershell expands into the interstellar medium favorable circumstances for star formation occur. IC 2118 is located in one such area.The wind blown appearance and cometary shape of the bright reflection nebula is highly suggestive of a strong association with the high mass luminous stars of Orion OB1. The fact that the heads of the cometary clouds of IC2118 point northeast towards the association is strong support of that relationship.


Antares Region

 

The Rho Ophiuchi

Optics/mount: 180 Epsilon f2,8 Takahashi Mount Alt-5ADN
CCD: QHY 12
exposure: mosaic 9x10x600 sec

The Rho Ophiuchi cloud complex is a dark nebula of gas and dust that is located 1° south of the star ρ Ophiuchi of the constellation Ophiuchus. At an estimated distance of 131 ± 3 parsecs, this cloud is one of the closest star-forming regions to the Solar System.

This cloud covers an angular area of 4.5° × 6.5° on the celestial sphere. It consists of two major regions of dense gas and dust. The first contains a star-forming cloud (L1688) and two filaments (L1709 and L1755), while the second has a star-forming region (L1689) and a filament (L1712–L1729). These filaments extend up to 10–17.5 parsecs in length and can be as narrow as 0.24 parsecs in width. Some of the structures within the complex appear to be the result of a shock front passing through the clouds from the direction of the neighboring Sco OB2 association.

Temperatures of the clouds range from 13–22 K, and there is a total of about 3,000 times the mass of the Sun in material. Over half of the mass of the complex is concentrated around the L1688 cloud, and this is the most active star-forming region. There are embedded infrared sources within the complex.[6] A total of 425 infrared sources have been detected near the L1688 cloud. These are presumed to be young stellar objects, including 16 classified as protostars, 123 T Tauri stars with dense circumstellar disks, and 77 weaker T Tauri stars with thinner disks. The last two categories of stars have estimated ages ranging from 100,000 to a million years.

The first brown dwarf to be identified in a star-forming region was Rho Oph J162349.8-242601, located in the Rho Ophiuchi cloud. One of the older objects at the edge of the primary star-forming region was found to be a circumstellar disk seen nearly edge on. It spans a diameter of 300 AU and contains at least twice the mass of Jupiter. The million-year-old star at the center of the disk has a temperature of 3,000 K and is emitting 0.4 times the luminosity of the Sun.


Melotte 15

Melotte15 wide

Melotte15 in the IC1805

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB HA5nm
Exposure: 22x900ha ,22×900 SII 10×900 OIII 1x1bin

The bright star cluster ( “open cluster”) centered in this image is known as Melotte15 after its discover, Philibert Jacques Melotte (1880-1961). Melotte 15 is embedded within and illuminates the central portion of the much larger glowing nebula identified as IC 1805. The interesting structure in the center of the image is a giant area of hydrogen gas that is caused to glow by the intense ultraviolet radiation from the massive stars of the Melotte 15 star cluster. It is estimated that this illuminated gas is more than 50 light years from the Melotte15 stars.

The nebula’s intense red output and its configuration are driven by the radiation emanating from a small group of stars near the nebula’s center. This open cluster of stars known as Melotte 15 contains a few bright stars nearly 50 times the mass of our Sun, and many more dim stars that are only a fraction of our Sun’s mass. The cluster used to contain a microquasar that was expelled millions of years ago.

The Heart Nebula, IC 1805, Sh2-190, lies some 7500 light years away from Earth and is located in the Perseus Arm of the Galaxy in the constellation Cassiopeia. This is an emission nebula showing glowing gas and darker dust lanes. The nebula is formed by plasma of ionized hydrogen and free electrons.@ wikipdia


Sh2-155

SH2.155

Optics/mount: 180 Epsilon f2,8 Takahashi  Mount  CI700 Clestron
Camera/filters:QHY 12
exposure: 35×900 sec

The Cave Nebula, Sh2-155 or Caldwell 9, is a dim and very diffuse bright nebula within a larger nebula complex containing emission, reflection, and dark nebulosity. It is located in the constellation Cepheus.

Visually it is a difficult object, but with adequate exposure, makes a striking image. The nebula gets its name from the dark lane at the eastern side abutting the brightest curve of emission nebulosity which gives the appearance of a deep cave when seen through a telescope visually.


Sh2-115

Optics/mount: 180 Epsilon f2,8 Takahashi Mount Ci700 Celestron
Camera/filters:QHY 12
exposure: 10×900 sec