AstroBin saves small pieces of text information (cookies) on your device in order to deliver better content and for statistical purposes. You can disable the usage of cookies by changing the settings of your browser. By browsing AstroBin without changing the browser settings, you grant us permission to store that information on your device.I agree
The Image Index is a system based on likes received on images, that incentivizes the most active and liked members of the community. Learn more.
The Contribution Index (beta) is system to reward informative, constructive, and valuable commentary on AstroBin. Learn more.
Imaging telescopes or lenses: Explore Scientific 152 mm Carbon Fiber
Guiding telescopes or lenses: Orion 80mm Short Tube
Software: PHD2 · Sequence Generator Pro · PixInsight · Photoshop CS5 · SkySafari Pro
Astrodon Blue Tru-Balance E-Series Gen 2: 20x60" (gain: 0.00) -20C bin 1x1
Astrodon Green Tru-Balance E-Series Gen 2: 20x60" (gain: 0.00) -20C bin 1x1
Astrodon Ha 5nm: 783x120" (gain: 200.00) -20C bin 1x1
Astrodon OIII 3nm: 976x120" (gain: 200.00) -20C bin 1x1
Astrodon Red Tru-Balance E-Series Gen 2: 20x60" (gain: 0.00) -20C bin 1x1
Integration: 59.6 hours
Avg. Moon age: 15.12 days
Avg. Moon phase: 61.82%
Bortle Dark-Sky Scale: 8.00
Astrometry.net job: 3328890
RA center: 11h 14' 47"
DEC center: +55° 1' 8"
Pixel scale: 0.325 arcsec/pixel
Orientation: 52.980 degrees
Field radius: 0.164 degrees
Locations: Backyard White Zone Observatory, Taylor, MI, Michigan, United States
Data source: Backyard
This proved to be a very challenging object to process. Not only did I want to capture the OIII being ejected out, but also the details of the core. I combined 12 hours of data in Ha and OIII from 2019 with data I just captured in 2020 in HaOIIIRGB. RGB was only captured for the stars.
The Owl Nebula (also known as Messier 97, M97 or NGC 3587) is a planetary nebula located approximately 2,030 light years away in the constellation Ursa Major. It was discovered by French astronomer Pierre Méchain on February 16, 1781. When William Parsons, 3rd Earl of Rosse, observed the nebula in 1848, his hand-drawn illustration resembled an owl's head. It has been known as the Owl Nebula ever since.
The nebula is approximately 8,000 years old. It is approximately circular in cross-section with a little visible internal structure. It was formed from the outflow of material from the stellar wind of the central star as it evolved along the asymptotic giant branch. The nebula is arranged in three concentric shells, with the outermost shell being about 20–30% larger than the inner shell. The owl-like appearance of the nebula is the result of an inner shell that is not circularly symmetric, but instead forms a barrel-like structure aligned at an angle of 45° to the line of sight.
The nebula holds about 0.13 solar masses of matter, including hydrogen, helium, nitrogen, oxygen, and sulfur; all with a density of less than 100 particles per cubic centimeter. Its outer radius is around 0.91 ly (0.28 pc) and it is expanding with velocities in the range of 27–39 km/s into the surrounding interstellar medium.
The 14th magnitude central star has since reached the turning point of its evolution where it condenses to form a white dwarf. It has 55–60% of the Sun's mass, 41–148 times the brightness of the Sun, and an effective temperature of 123,000 K. The star has been successfully resolved by the Spitzer Space Telescope as a point source that does not show the infrared excess characteristic of a circumstellar disk.
|You have no new notifications.|
This page or operation is not available at the moment, because AstroBin is in READ ONLY mode. For more information, please check out our Twitter feed: https://twitter.com/AstroBin_com
This feature is only offered at higher membership levels.
Would you be interested in upgrading? AstroBin is a very small business and your support would mean a lot!
If this user has been harassing you, and you shadow-ban them, all their activities on your content will be invisible to everyone except themselves.
They will not know that they have been shadow-banned, and the goal is that eventually they will get bored while having caused no harm, since nobody saw what they posted.
You will remove your shadow-ban on this user, and their comments, messages, etc, will appear again on your content.
Such limitation improves the website as a whole by discouraging people from creating fake accounts to like their own content. Thank you for understanding!
Currently, your Image Index is .
To learn more about the Image Index, please visit the FAQ page. Thanks!