Wednesday, February 13, 2013
IC 443, supernova remnant as a closeup
I have shot several times this supernova remnant in Gemini. In this image, there are three different exposure sets combined, first from the year 2010 and two others from this season. Total exposure time is now around 20h. Latest images for this target are shot at 11.02 this week, 3h of H-alpha emission.
A Gemini SNR, IC 443, the "Jellyfish Nebula"
Ra 06h 17m 13s Dec +22° 31′ 05′′
Image is in HST-palette, from the emission of ionized elements, R=Sulfur, G=Hydrogen and B=Oxygen.
INFO
IC 443 (also known as the Jellyfish Nebula and Sharpless 248 (Sh2-248)) is a Galactic supernova remnant (SNR) in the constellation Gemini. It locates visually near the star Eta Geminorum at distance of about 5000 light years.
IC 443 may be the remains of a supernova that 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 cases of supernova remnants interacting with surrounding molecular clouds
Source Wikipedia, http://en.wikipedia.org/wiki/IC_443
IC 443 in visual colors
A natural color composition from the emission of ionized elements.
R=80%Hydrogen+20%Sulfur, G=100%Oxygen and B=85%Oxygen+15% Hydrogen to compensate otherwise missing H-beta emission. This composition is very close to a visual spectrum.
Older wide field images of the same target
Click for large images
A wide field image from Spring season 2012, Image info in the blog post here:
Two panel mosaic
A two panel mosaic, info in the original blogpost here:
A study about the apparent scale in the sky
Click for a large image
Note. A Moon size circle as a scale.
Technical details
Processing work flow:
Image acquisition, MaxiDL v5.07.
Stacked and calibrated in CCDStack2.
Levels, curves and color combine in PS CS3.
Optics, Meade LX200 GPS 12" @ f5
Camera, QHY9
Guiding, SXV-AO, an active optics unit, and Lodestar guide camera 8Hz
Image Scale, ~0,8 arc-seconds/pixel
Exposures for the H-alpha, emission of ionized Hydrogen = 20h
Narrowband cahnnels for ionized Oxygen and Sulfur are taken from an older wide field image.
A single unprocessed 1200 second frame of H-a emission
A single 20 min. frame, just calibrated and stretched. Imaged with the QHY9 camera, Baader 7nm H-alpha filter and Meade LX200 12" telescope.
Tuesday, February 12, 2013
A two frame mosaic of IC 1805
This is a two frame mosaic of IC 1805, the Heart Nebula. Image shows a detail, from much large nebula complex, in natural colors. Colors are combined to a visual spectrum from emissions of ionized elements.
A detail of IC 1805 emission nebula
Natural color composition from the emission of ionized elements.
R=80%Hydrogen+20%Sulfur, G=100%Oxygen and B=85%Oxygen+15% Hydrogen to compensate otherwise missing H-beta emission. This composition is very close to a visual spectrum.
This image in a HST-palette and technical details can be found from my previous post
http://astroanarchy.blogspot.fi/2013/02/black-lace-detail-of-ic-1805-heart.html
A study about the apparent scale in the sky
Moon size circle as a scale
Note. a Moon size circle in images as a scale.
The apparent size of the full Moon is ~30 arc minutes, that's equal to ~0.5 degrees.
Thursday, February 7, 2013
Black Lace, a detail of IC 1805, the Heart Nebula
This have been one of the worst winters for astrophotographing up here 65N. Somehow I managed to shoot six hours of H-alpha light for this target under a bad transparency, seeing was kind of good though.
Generally I'll like to shoot two or three times more exposures per target but if I'll do so, I might get only four new images per year... For the same reasons I have used my older, wide field, images as a source of color data. Naturally it's better to shoot all the color channel at same focal length but ones again, weather up here is too volatile for that.
OK, enough whining here. I proudly present the new image of IC 1805 from 5. January,
Black Lace, a detail of IC 1805, the Heart nebula
A closeup of IC 1805 in mapped colors. Edges of the triangle shape, at middle right, looks like a black lace.
Buy a photographic print from HERE
Buy a photographic print from HERE
A mosaic with Melotte 15
Since this new image of mine was overlapping with the Melotte 15 image, I made a two frame mosaic out of them.
A mapped color mosaic image shows the Melotte 15 at upper right corner.
Buy a photographic print from HERE
Black Lace in natural colors
Natural color composition from the emission of ionized elements.
R=80%Hydrogen+20%Sulfur, G=100%Oxygen and B=85%Oxygen+15% Hydrogen to compensate otherwise missing H-beta emission. This composition is very close to a visual spectrum.
Buy a photographic print from HERE
Buy a photographic print from HERE
Orientation in the Heart Nebula
The area of interest is marked with a white rectangle.
Buy a photographic print from HERE
INFO
The "Heart Nebula", IC1805 locates about 7500 light years away in constellation Cassiopeia. This is an emission nebula showing glow of ionized elements in a gas cloud and some darker dust lanes.
In a very center of the nebula, lays Melotte 15, it contains few very bright stars, nearly 50 times mass of our Sun, and many dim ones. The solar wind, a radiation pressure, from massive stars makes the gas twist to a various shapes.
Technical details
Processing work flow:
Image acquisition, MaxiDL v5.07.
Stacked and calibrated in CCDStack2.
Levels, curves and color combine in PS CS3.
Optics, Meade LX200 GPS 12" @ f5
Camera, QHY9
Guiding, SXV-AO, an active optics unit, and Lodestar guide camera 8Hz
Image Scale, ~0,8 arc-seconds/pixel
18 x 1200s exposures for the H-alpha, emission of ionized Hydrogen = 6h
Narrowband cahnnels for ionized Oxygen and Sulfur are taken from an older wide field images.
A single unprocessed 1200 second frame of H-a emission
single 20 min. frame, just calibrated and stretched. Imaged with the QHY9 camera, Baader 7nm H-alpha filter and Meade LX200 12" telescope.
Wednesday, February 6, 2013
3D-study of Messier 27, the Dumbbell nebula
This is an experimental test with a 3D-conversion of my astronomical images. Only real elements from my image are used, there is nothing added but the volumetric information!
(In this image, two of the stars are enhanced for a visual reasons)
NOTE. This is a personal vision about shapes and volumes, based on some scientific data and an artistic impression.
Dumbbell Nebula, M27, 3D-model
This is a looped video, click to start and stop. Original movie is in HD1080p resolution.
Large movie in Vimeo service
(HD720p)
https://vimeo.com/59052389
NOTE. Right click the video to turn HD and Loop on!
Large movie in Vimeo service
(HD720p)
https://vimeo.com/59052389
NOTE. Right click the video to turn HD and Loop on!
Original 2D-image of the Messier 27
More images and technical details in this blog post:
Buy a photographic print from HERE
Info about the technique used
Due to huge distances, real parallax can't be imaged in most of the astronomical objects.
I have developed an experimental technique to convert my astropics to a artificial volumetric models.
My 3-D experiments are a mixture of science and an artistic impression. I collect distance and other information before I do my 3-D conversion. Usually there are known stars, coursing the ionization, so I can place them at right relative distance. If I know a distance to the nebula, I can fine tune distances of the stars so, that right amount of stars are front and behind of the object.
I use a “rule of thumb” method for stars: brighter is closer, but if a real distance is known, I'm using that. Many 3-D shapes can be figured out just by looking carefully the structures in nebula, such as dark nebulae must be at front of the emission nebulae in order to show up etc...
The general structure of many star forming regions is very same, there is a group of young stars, as an open cluster inside of the nebula. The stellar wind from the stars is then blowing the gas away around the cluster and forming a kind of cavitation – or a hole — around it. The pillar-like formations in the nebula must point to a source of stellar wind, for the same reason.
How accurate the final model is, depends how much I have known and guessed right. The motivation to make those 3-D-studies is just to show, that objects in the images are not like paintings on the canvas but really three dimensional objects floating in the three dimensional space. This generally adds a new dimension to my hobby as an astronomical imager. (Pun intended)
Monday, February 4, 2013
3D-study of the Rosette Nebula
This is an experimental test with a 3D-conversion of my astronomical images. Only real elements from my image are used, there is nothing added but the volumetric information!
NOTE. This is a personal vision about shapes and volumes, based on some scientific data and an artistic impression.
Rosette Nebula 3D-model I
Original 2D-image of the Rosetta Nebula
http://astroanarchy.blogspot.fi/2012/12/caldwell-49-rosette-nebula-reprocessed.html
Rosette Nebula 3D-model II
Info about the technique used
Due to huge distances, real parallax can't be imaged in most of the astronomical objects.
I have developed an experimental technique to convert my astropics to a artificial volumetric models.
My 3-D experiments are a mixture of science and an artistic impression. I collect distance and other information before I do my 3-D conversion. Usually there are known stars, coursing the ionization, so I can place them at right relative distance. If I know a distance to the nebula, I can fine tune distances of the stars so, that right amount of stars are front and behind of the object.
I use a “rule of thumb” method for stars: brighter is closer, but if a real distance is known, I'm using that. Many 3-D shapes can be figured out just by looking carefully the structures in nebula, such as dark nebulae must be at front of the emission nebulae in order to show up etc...
The general structure of many star forming regions is very same, there is a group of young stars, as an open cluster inside of the nebula. The stellar wind from the stars is then blowing the gas away around the cluster and forming a kind of cavitation – or a hole — around it. The pillar-like formations in the nebula must point to a source of stellar wind, for the same reason.
How accurate the final model is, depends how much I have known and guessed right. The motivation to make those 3-D-studies is just to show, that objects in the images are not like paintings on the canvas but really three dimensional objects floating in the three dimensional space. This generally adds a new dimension to my hobby as an astronomical imager. (Pun intended)
A 3D-study of the Simeis 147 supernova remnant
This is an experimental test with a 3D-conversion of my astronomical images. Only real elements from my image are used, there is nothing added but the volumetric information!
NOTE. This is a personal vision about shapes and volumes, based on some scientific data and an artistic impression.
Simeis 147 3D-model as a"fast fly trough"
Original 2D-image of Simeis 147
http://astroanarchy.blogspot.fi/2012/02/siemis-147-new-data-added.html
Simeis 147 3D-model as a looped rotation
Info about the technique used
Due to huge distances, real parallax can't be imaged in most of the astronomical objects.
I have developed an experimental technique to convert my astropics to a artificial volumetric models.
My 3-D experiments are a mixture of science and an artistic impression. I collect distance and other information before I do my 3-D conversion. Usually there are known stars, coursing the ionization, so I can place them at right relative distance. If I know a distance to the nebula, I can fine tune distances of the stars so, that right amount of stars are front and behind of the object.
I use a “rule of thumb” method for stars: brighter is closer, but if a real distance is known, I'm using that. Many 3-D shapes can be figured out just by looking carefully the structures in nebula, such as dark nebulae must be at front of the emission nebulae in order to show up etc...
The general structure of many star forming regions is very same, there is a group of young stars, as an open cluster inside of the nebula. The stellar wind from the stars is then blowing the gas away around the cluster and forming a kind of cavitation – or a hole — around it. The pillar-like formations in the nebula must point to a source of stellar wind, for the same reason.
How accurate the final model is, depends how much I have known and guessed right. The motivation to make those 3-D-studies is just to show, that objects in the images are not like paintings on the canvas but really three dimensional objects floating in the three dimensional space. This generally adds a new dimension to my hobby as an astronomical imager. (Pun intended)
Wednesday, January 30, 2013
A 3D-study of the Pac-Man Nebula, NGC 281
This is an experimental test with a 3D-conversion of my astronomical images. I have published some animated GIF files, this time I have done a short movie out of the model. Even though this is just a looped tip tilt movie, I'm able to do any movements with this kind of model.
Only real elements from my image are used, there is nothing added but the volumetric information!
NOTE. This is a personal vision about shapes and volumes, based on some scientific data and an artistic impression.
NOTE. This is a personal vision about shapes and volumes, based on some scientific data and an artistic impression.
A 3D study of NGC 281
Movie is in natural colors
In YouTube you can see this image at a full screen and resolution:
(Click the gear symbol to select 720p )
Info about the technique used
My 3-D experiments are a mixture of science and an artistic impression. I collect distance and other information before I do my 3-D conversion. Usually there are known stars, coursing the ionization, so I can place them at right relative distance. If I know a distance to the nebula, I can fine tune distances of the stars so, that right amount of stars are front and behind of the object.
I use a “rule of thumb” method for stars: brighter is closer, but if a real distance is known, I'm using that. Many 3-D shapes can be figured out just by looking carefully the structures in nebula, such as dark nebulae must be at front of the emission nebulae in order to show up etc...
The general structure of many star forming regions is very same, there is a group of young stars, as an open cluster inside of the nebula. The stellar wind from the stars is then blowing the gas away around the cluster and forming a kind of cavitation – or a hole — around it. The pillar-like formations in the nebula must point to a source of stellar wind, for the same reason.
How accurate the final model is, depends how much I have known and guessed right. The motivation to make those 3-D-studies is just to show, that objects in the images are not like paintings on the canvas but really three dimensional objects floating in the three dimensional space. This generally adds a new dimension to my hobby as an astronomical imager. (Pun intended)
Original 2D-image
Only elements form this image are used for the animation above
A blog post about this new image of mine can be seen here:
NGC 281, the Pac-Man Nebula
A new image from the last week, NGC 281, I spend four nights imaging but the bad seeing and some thin upper clouds ruined majority of my frames. I managed to get enough exposures for two images, the Soul Nebula detail and this shot of Pac-Man Nebula.
NGC 281, in Cassiopeia
Ra 00h 52m 59.3s Dec +56° 37′ 19″
Image is in mapped colors from the emission of ionized elements, R=Sulfur, G=Hydrogen and B=Oxygen.
Star colors are shot with a QHY8 color camera, Tokina 300mm f2.8 optics and the Baader UHCs filter.
Image is taken at 21. Jan. and there are 23x20min H-alpha light collected for it, color data is borrowed from my older image of the NGC 281. This is the third time for my tandem camera system, Star and natural color of the nebula are shot at the same time, as the closeup image, with the QHY8 color camera and the Baader UHCs-filter. This filter delivers real colors for the stars, even though it's kind of narrowband filter.
INFO
NGC 281 is an H II region in the constellation of Cassiopeia. It includes the open cluster IC 1590 and several Bok globules (dark doo-dads at center of the Blue area). NGC 281 is also known as the Pac-Man Nebula for its resemblance to the video game character from early 80's.
NGC281 spans over 80 light years at its estimated distance of 9500 light years.
An experimental 3D study of NGC 281
This is a link to a 3D-movie, please, have a look:
NGC 281 in visual colors
Image is in visual spectrum and dominated by the red light emitted by ionized Hydrogen, H-alpha. Blueish hues are from ionized Oxygen, O-III. Colors are shot simultaneously with H-a emission by using QHY8 color camera, Tokina AT-X 300mm f2.8 camera lens and Baader UHCs-filter.
Buy a photographic print from HERE
A study about the shapes
Lines in the image are showing, how the pillar-like formations are all pointing to the source of solar wind and ionization, the open cluster IC 1590, inside the Pack_man Nebula.
There are some denser material at tip of the pillar like formations and it's able to resist the radiation pressure from the open cluster IC 1590, at the middle of the nebula. Typically those tips are future homes for newly born stars, as well as dark globules seen in the image. The same open cluster is coursing the ionization in Pac-Man Nebula by its radiation. each ionized element in the nebula emits light at the typical wave length.
Technical details:
Processing work flow:
Image acquisition, MaxiDL v5.07.
Stacked and calibrated in CCDStack2.
Levels, curves and color combine in PS CS3.
Optics, Meade LX200 GPS 12" @ f5
Camera, QHY9
Guiding, SXV-AO, an active optics unit, and Lodestar guide camera 12Hz
Image Scale, ~0,8 arc-seconds/pixel
24 x 1200s exposures for the H-alpha, emission of ionized Hydrogen = 8h
Optics and exposures used for colors
Tokina AT-X 300mm at f2.8
QHY8, a cooled single shot color camera
Baader UHC-s filter
Baader IR-cut filter
16x900s = 4h
Color channels for a mapped-palette image, O-III and S-II, are from an older image of mine.
A single unprocessed 1200 second frame of H-a emission
A single 20 min. frame, just calibrated and stretched. Imaged with the QHY9 camera, Baader 7nm H-alpha filter and Meade LX200 12" telescope.
Monday, January 28, 2013
A 3D-study of The Soul nebula detail
This is my new test with a 3d-conversion of my astronomical images. I have published some animated GIF files, this time I have done a short movie out of the model. Even though this is just a looped tip tilt movie, I'm abel to do any movements with this new kind of model.
Only real elements from my image are used, there is nothing added but the volumetric information!
A 3D study of IC 1848
Image is in mapped colors.
Pay attention to a transparent 3d-shapes, they usually are very difficult to animate.
In YouTube you can see this image at a full screen and resolution:
(Click the gear symbol to select 720p )
Info about the technique used
My 3-D experiments are a mixture of science and an artistic impression. I collect distance and other information before I do my 3-D conversion. Usually there are known stars, coursing the ionization, so I can place them at right relative distance. If I know a distance to the nebula, I can fine tune distances of the stars so, that right amount of stars are front and behind of the object.
I use a “rule of thumb” method for stars: brighter is closer, but if a real distance is known, I'm using that. Many 3-D shapes can be figured out just by looking carefully the structures in nebula, such as dark nebulae must be at front of the emission nebulae in order to show up etc...
The general structure of many star forming regions is very same, there is a group of young stars, as an open cluster inside of the nebula. The stellar wind from the stars is then blowing the gas away around the cluster and forming a kind of cavitation – or a hole — around it. The pillar-like formations in the nebula must point to a source of stellar wind, for the same reason.
How accurate the final model is, depends how much I have known and guessed right. The motivation to make those 3-D-studies is just to show, that objects in the images are not like paintings on the canvas but really three dimensional objects floating in the three dimensional space. This generally adds a new dimension to my hobby as an astronomical imager. (Pun intended)
Original 2D-image
Only elements form this image are used for the animation above
A blog post about this new image of mine can be seen here:
Sunday, January 27, 2013
Soul Nebula detail, IC 1848
I was able to shoot through four nights at last week. Unfortunately three of those night was ruined by a bad seeing, FWHM around 7, and nearly invisible thin clouds ate out the weaker signals. However, I had enough good data for couple of new images, here is the first one, IC 1848.
A closeup of IC 1848, the "Soul Nebula"
Ra 02h 51m 36.24s Dec +60° 26′ 53.9"
Image is in mapped colors from the emission of ionized elements, R=Sulfur, G=Hydrogen and B=Oxygen.
Star colors are shot with a QHY8 color camera, Tokina 300mm f2.8 optics and the Baader UHCs filter.
The open cluster IC 1848 can be seen at upper right edge of the image. (Two bright stars surrounded by a group of dimmer stars.)
The open cluster IC 1848 can be seen at upper right edge of the image. (Two bright stars surrounded by a group of dimmer stars.)
There are 14x20min H-alpha light collected for this image, color data is borrowed from my older wide field image of the Soul Nebula. This is the second time for my tandem camera system, Star colors are shot at the same time, as the closeup image, with the QHY8 color camera and the Baader UHCs-filter. This filter delivers real colors for the stars, even though it's kind of narrowband filter.
INFO
Soul Nebula, (Sh2-199, LBN 667) is an emission nebula in constellation Cassiopeia. IC 1848 is a cluster inside Soul Nebula. Distance is about 7.500 light years. This complex is a Eastern neighbor of IC 1805, the "Heart Nebula" and they are often mentioned together as Heart and Soul.
A study about the apparent scale
IC 1848 in visual colors
Image is in visual spectrum and dominated by the red light emitted by ionized Hydrogen, H-alpha. Blueish hues are from ionized Oxygen, O-III. Colors are shot simultaneously with H-a emission by using QHY8 color camera, Tokina AT-X 300mm f2.8 camera lens and Baader UHCs-filter.
Orientation and colors
The area of interest is marked with a white rectangle. Mapped colors, in up most image, are from this one.
This UHCs filtered image was shot simultaneously with H-a emission by using QHY8 color camera, Tokina AT-X 300mm f2.8 camera lens and Baader UHCs-filter.
Colors in visual color image, second from the top, are taken from this image, as well as the star colors in both versions.
Technical details:
Processing work flow:
Image acquisition, MaxiDL v5.07.
Stacked and calibrated in CCDStack2.
Levels, curves and color combine in PS CS3.
Optics, Meade LX200 GPS 12" @ f5
Camera, QHY9
Guiding, SXV-AO, an active optics unit, and Lodestar guide camera 12Hz
Image Scale, ~0,8 arc-seconds/pixel
15 x 1200s exposures for the H-alpha, emission of ionized Hydrogen = 5h
Optics and exposures used for colors
Optics and exposures used for colors
Tokina AT-X 300mm at f2.8
QHY8, a cooled single shot color camera
Baader UHC-s filter
Baader IR-cut filter
16x900s = 4h
16x900s = 4h
Color channels for a mapped-palette image, O-III and S-II, are from an older wide field image.
A single calibrated 1200 second frame of H-a emission
A single 20 min. frame, just calibrated and stretched. Imaged with the QHY9 camera, Baader 7nm H-alpha filter and Meade LX200 12" telescope.
Saturday, January 12, 2013
A heavenly velvet, IC 405
A new image from the night of 10.01.
IC 405, the Flaming Star Nebula
In constellation Auriga
This is a first time when I used two optics and the cameras at the same time.
H-a is shot with my old Meade LX200 12", Baader H-alpha filter and a cooled gray scale astrocamera, QHY9.
Colors are shot at the same time by using a Tokina AT-X 300mm camera lens, Baader UHC-s filter and the cooled single shot color astrocam, QHY8. Tokina system was at back of the Meade telescope.
Image with Tokina AT-X 300mm camera lens, Baader UHC-s filter and QHY8 cooled color camera.
This image was shot at the same time as narrower field H-alpha shot with Meade LX200 12" and QHY9 astro camera.
INFO
IC 405 locates in constellation Auriga and it's an emission/reflection nebula. Reflection component can't be seen in my image, since I'm shooting only narrowband data and reflection part is broadband target.
Distance from Oulu, Finland, is about 1500 light years. Nebula is about 5 light years across.
IC 405, mapped colors in HST-palette
Click for a large image.
Orientation
In a wider field image
The area of interest is marked with a white rectangle.
Wide field images of the area
A twelve panel mosaic of the constellation Auriga in HST-mapped colors.
Note. a largish image, 2.75MB and 2000x1100 pixels.
A blog post about this image, with technical details, can be seen here: http://astroanarchy.blogspot.fi/2012/03/auriga-panorama-gets-bigger-12-panels.html
A central portion of the mosaic above.
Technical details:
Processing work flow:
Image acquisition, MaxiDL v5.07.
Stacked and calibrated in CCDStack2.
Levels, curves and color combine in PS CS3.
Optics, Meade LX200 GPS 12" @ f5
Camera, QHY9
Guiding, SXV-AO, an active optics unit, and Lodestar guide camera 5Hz
Image Scale, ~0,8 arc-seconds/pixel
12 x 1200s exposures for the H-alpha, emission of ionized Hydrogen = 4h
Optics and exposures used for colors
Tokina AT-X 300mm at f2.8
QHY8, a cooled single shot color camera
Baader UHC-s filter
36x300s = 3h
Optics and exposures used for colors
Tokina AT-X 300mm at f2.8
QHY8, a cooled single shot color camera
Baader UHC-s filter
36x300s = 3h
Color channels for HST-palette image, O-III and S-II, are from an older wide field image.
Friday, January 11, 2013
NGC 1491, the project finalized
I was able to finalize this imaging project since I found an older wide field color image of mine from this area.
I used colors from this wider field image and it seems to work fine. naturally the resolution is much lower in other than H-alpha channel but it doesn't harm the image too much since there are not much details in O-III and S-II channels in this case.
NGC 1491
in constellation Perseus
Colors are mapped to a HST-palette, R=Sulfur, G=Hydrogen and B=Oxygen
Click for a large image.
INFO
NGC 1491 is an emission nebula, in the constellation Perseus, at the distance of about 10700 light years. The ultraviolet light from the newly born stars makes elements in the nebula glow. There is an an 11th magnitude star in its center. The solar wind, a radiation pressure, from the central star is blowing a bubble in the gas surrounding it. This is a dim one, seven hours of exposures was barely enough to reveal it.
A closeup
NGC 1491 in natural colors
Combined from the emission lines of H-a, S-II and O-III
A wide field image
Shot at Spring 2012
The large nebula at center is Sharpless 205 (Sh2-205), NGC 1491 can be seen at upper left corner..
Some info about the wide field image
This Sharpless object is very dim and difficult to shoot (as they usually are). The bright, peanut shape, area at middle is known as Sh2-205, bright nebula, at top left, is NGC 1491. Image spans about 5,5 degrees horizontally, that's 11 full Moons side by side. There are very few images around out of this object. Total exposure time, with a fast 200mm f1.8 optics, is 12h from three nights between 28.01 - 02.02. 2012.
Technical details:
Processing work flow:
Image acquisition, MaxiDL v5.07.
Stacked and calibrated in CCDStack2.
Levels, curves and color combine in PS CS3.
Optics, Meade LX200 GPS 12" @ f5
Camera, QHY9
Guiding, SXV-AO, an active optics unit, and Lodestar guide camera 5Hz
Image Scale, ~0,8 arc-seconds/pixel
21 x 1200s exposures for the H-alpha, emission of ionized Hydrogen = 7h
Color channels for O-III and S-II are from an older wide field image.
Ps.
A popular shape in our local universe
While processing the image, I noticed a familiar shape in the center portion of the image.
It seems to repeat itself in various targets. My guess is, that it's coursed by the solar wind from the open cluster usually locates in center of the emission nebula of this type.
A collection of targets with same type of shapes as can be seen in center of the this new image.
The top most two images are from NGC 1491.
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