Amateur Astrophotographie Landos France


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


M64 Zoom

M64 Zoom

M78 with the 12″ACF


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


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


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 891

Ngc 891

NGC 891

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB HA5nm
Exposure: 4*12×600 Lum,RGB all 1bin

NGC 891 (also known as Caldwell 23) is an edge-on unbarred spiral galaxy about 30 million light-years away in the constellation Andromeda. It was discovered by William Herschel on October 6 1784. The galaxy is a member of the NGC 1023 group of galaxies in the Local Supercluster. It has an H II nucleus.[3]

The object is visible in small to moderate size telescopes as a faint elongated smear of light with a dust lane visible in larger apertures.

In 1999, the Hubble Space Telescope imaged NGC 891 in infrared.

In 2005, due to its attractiveness and scientific interest, NGC 891 was selected to be the first light image of the Large Binocular Telescope.[4]

Supernova SN 1986J was discovered on August 21, 1986 at apparent magnitude 14

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
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.

M33 Triangulum Galaxy




Optics/mount: 180 Epsilon f2,8 Takahashi Mount CI700 Clestron
Camera/filters:QHY 12
exposure: 20×600 sec

The Triangulum Galaxy is a spiral galaxy approximately 3 million light years (ly) from Earth in the constellation Triangulum. It is catalogued as Messier 33 or NGC 598, and is sometimes informally referred to as the Pinwheel Galaxy, a nickname it shares with Messier 101. The Triangulum Galaxy is the third-largest member of the Local Group of galaxies, which includes the Milky Way Galaxy, the Andromeda Galaxy and about 30 other smaller galaxies. It is one of the most distant permanent objects that can be viewed with the naked eye.

M51 Whirlpool Galaxy

The Whirlpool Galaxy
(also known as Messier 51a, M51a, or NGC 5194) is an interacting grand-design spiral galaxy that is estimated to be 23 ± 4 million light-years from the Milky Way Galaxy. in the constellation Canes Venatici. It is one of the most famous galaxies in the sky. The galaxy and its companion (NGC 5195) are easily observed by amateur astronomers, and the two galaxies may even be seen with binoculars. The Whirlpool Galaxy is also a popular target for professional astronomers, who study it to further understand galaxy structure (particularly structure associated with the spiral arms) and galaxy interactions.

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB HA5nm
Exposure: 25×600 Lum, 8×900 ha, 8×600 RGb all 1bin


Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB HA5nm
Exposure: 12×900 Lum, 6×900 RGB all 1bin

This pair of galaxies often goes by the nickname of the “Cocoon Galaxy.” Each “blob” is actually a spiral galaxy that has been distorted by the other. Hints of spiral structure are still evident in the smaller galaxy. These galaxies have already passed their closest approach (perigalacticon) and are now speeding away from each other. A tail of stars stretches between the galaxies which are separated by at least 24,000 light years. All of this action takes place 40-50 million light years away. These interacting galaxies make a good real-world example for astronomers to compare computer models (simulations) of galactic collisions. Note the incredible number of starforming regions that have developed along facing sides of each galaxy.

NGC4631 The Whale

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB HA5nm
Exposure: 12×600 Lum, 6×600 RGB all 1bin

NGC 4631 (also known as the Whale Galaxy or Caldwell 32) is an edge-on spiral galaxy in the constellation Canes Venatici. This galaxy’s slightly distorted wedge shape gives it the appearance of a herring or a whale, whence its nickname.[3] Because this nearby galaxy is seen edge-on from Earth, professional astronomers observe this galaxy to better understand the gas and stars located outside the plane of the galaxy.

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



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.


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

M52 and Bubble widefield

Optics/mount: 180 Epsilon f2,8 Takahashi  Mount Ci700 Celestron
Camera/filters:QHY 12
exposure: 10×600 sec

Messier 52
(also known as M 52 or NGC 7654) is an open cluster in the Cassiopeia constellation. It was discovered by Charles Messier in 1774. M52 can be seen from Earth with binoculars.

Due to interstellar absorption of light, the distance to M 52 is uncertain, with estimates ranging between 3,000 and 7,000 light years. One study identified 193 probable members of the cluster, with the brightest member being magnitude 11. [1]

Messier 52 is evaluated at about 35 million years old.

NGC 7635, also called the Bubble Nebula, Sharpless 162, or Caldwell 11, is a H II region[2] emission nebula in the constellation Cassiopeia. It lies close to the direction of the open cluster Messier 52. The “bubble” is created by the stellar wind from a massive hot, 8.7[2] magnitude young central star, the 15 ± 5 M☉[4] SAO 20575 (BD+60 2522).[7] The nebula is near a giant molecular cloud which contains the expansion of the bubble nebula while itself being excited by the hot central star, causing it to glow.[7] It was discovered in 1787 by Friedrich Wilhelm Herschel.[6] The star SAO 20575 or BD+602522 is thought to have a mass of 10-40 Solar masses.

Flaming Star IC405

Flaming Star

Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB HA5nm
Exposure: 10×600 Lum 6×600 RGB all 1xbin

IC 405 (also known as the Flaming Star Nebula, SH 2-229, or Caldwell 31) is an emission/reflection nebula[1] in the constellation Auriga, surrounding the bluish star AE Aurigae. It shines at magnitude +6.0. Its celestial coordinates are RA 05h 16.2m dec +34° 28′.[2] It surrounds the irregular variable star AE Aurigae and is located near the emission nebula IC 410, the open cluster M38, and the naked-eye K-class star Hassaleh. The nebula measures approximately 37.0′ x 19.0′, and lies about 1,500 light-years away.[2] It is believed that the proper motion of the central star can be traced back to the Orion’s Belt area.[2] The nebula is about 5 light-years across.[1

North America and Pelican Nebula Version HST

NGC 7000, the North America Nebula, is located in the constellation of Cygnus. It is a very large area of emission nebulosity extending some 2.5 degrees to the east of Deneb. The ‘NAN’ is well named for its shape – which is easily recognizeable as resembling the continent of North America. It was discovered in the early 1890s during experiments into wide field astrophotography. Several areas of nebulosity can be seen surrounding NGC 7000 including IC 5070, the Pelican Nebula to the west and IC 5068 to the south. The ‘Skull Nebula’ can also be seen between the North America and the Pelican nebulae.

The Pelican Nebula (also known as IC 5070) is an HII region associated with the North America Nebula. The nebula resembles a pelican in shape, hence the name. The Pelican Nebula is divided from its brighter, larger neighbor, the North America Nebula, by a molecular cloud filled with dark dust. This nebula 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. 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.

Optics/mount: 180 Epsilon f2,8 Takahashi Alt-5
Camera/filters: Atik 11002 Astromik Ha S-II O-III
exposure: 10×600″ ha 6×600 S-II O-III

Helix nebula

NGC 7293

The Helix Nebula (also known as The Helix, NGC 7293, or Caldwell 63) is a large planetary nebula (PN) located in the constellation Aquarius. Discovered by Karl Ludwig Harding, probably before 1824, this object is one of the closest to the Earth of all the bright planetary nebulae. The estimated distance is about 215 parsecs or 700 light-years. It is similar in appearance to the Ring Nebula, whose size, age, and physical characteristics are similar to the Dumbbell Nebula, varying only in its relative proximity and the appearance from the equatorial viewing angle. The Helix has often been referred to as the Eye of God on the Internet, since about 2003.

Optics/mount: 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon HA RGB
exposure: Ha18x900 Lum10x600 RGB10x300 all 2xbin

NGC2903 in the Leo


Optics/mount : 12″ACF 2.7m AP-Reduzer Alt-5
Camera/filters: Atik 11002 Astrodon LRGB
Exposure: 20×600 Lum, 6×600 RGB all 1bin
21 Feb 2012

NGC 2903 is a barred spiral galaxy about 30 million light-years away in the constellation Leo. It was discovered by William Herschel who cataloged it on
November 16, 1784 @Wikipedia

NGC 2903 est une galaxie spirale barrée, située à environ 21 millions d’années-lumière, dans la constellation du Lion. Elle a été découverte par William Herschel le 16 novembre 1784. NGC 2905 est un nœud brillant (nuage d’étoiles) dans cette galaxie.@Wikipedia