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Imaging telescopes or lenses: Takahashi Epsilon 130D
Imaging cameras: Astrel Instruments AST8300
Mounts: 10 Micron GM3000 HPS
Software: PixInsight 1.8 · Zipproth GmbH Straton 2.0
Filters: Astronomik H-Alpha 6nm CCD
Dates:July 29, 2020 , July 30, 2020 , July 31, 2020 , Aug. 4, 2020 , Aug. 5, 2020 , Aug. 6, 2020 , Aug. 7, 2020 , Aug. 8, 2020 , Aug. 10, 2020 , Aug. 18, 2020 , Aug. 28, 2020
Frames:Astronomik H-Alpha 6nm CCD: 264x600" -20C bin 1x1
Integration: 44.0 hours
Darks: ~50
Flats: ~10
Bias: ~200
Avg. Moon age: 16.28 days
Avg. Moon phase: 75.83%
Bortle Dark-Sky Scale: 4.00
Astrometry.net job: 3935397
RA center: 0h 3' 6"
DEC center: +67° 18' 42"
Pixel scale: 2.598 arcsec/pixel
Orientation: 90.502 degrees
Field radius: 1.115 degrees
Resolution: 1950x2398
Locations: Home, Bergisches Land, Germany
Data source: Mix of multiple source
Today I would like to present you the result of my second astro cooperation. Florian Pieper asked me in early spring of this year if I would like to do a joint project. We quickly agreed that we wanted to try to gather at least 100 hours in narrow band for Cederblad 214.
This emission nebula is characterized by an unbelievable richness of structures, globules and dark nebula components. So it should become a deep image that shows many details. :-) Since we both own a very fast telescope with the Takahashi Epsilon and with our cameras we generate almost the same field of view, the decision was made. We spent the time from the end of July to mid of September to take all the data. Flo contributed the data for OIII and SII. The H-Alpha data came from me. A long time passed away for a single image...
So we were even more pleased to see the first interim results and afterwards of course the final raw images in SHO. The processing was a real pleasure for me! I can't remember ever having almost completely abandoned the denoising of my astro images. Here the quality was so good that this was effortlessly possible. :-)
Furthermore, this is my first image using my new mount (a 10 Micron GM3000 HPS). What a magnificent piece of technology! Precision, no backlash and no need for autoguiding. This is fun!
In the technical card I could only store the information of the exposures I made. Here is the complete overview:
* Image Acquisition (Florian Pieper)
SkyWatcher EQ6-AZ + Epsilon 130D + Asi1600mm-c + Astrodon SII,OIII 3mn
08/05 SII 51x300s
08/06 SII 53x300s
08/07 SII 56x300s
08/10 SII 58x300s
08/11 SII 60x300s
08/12 SII 57x300s
08/14 OIII 44x300s
08/15 OIII 50x300s
08/16 OIII 66x300s
09/02 OIII 77x300s
09/15 OIII 29x300s
09/16 OIII 75x300s
Exposure time 56.3 hrs
* Image Acquisition (Frank Breslawski)
10 Micron GM3000 HPS + Epsilon 130D + Astrel 8300 + Astronomik Ha 6nm
07/29 Ha 24x600s
07/30 Ha 29x600s
07/31 Ha 22x600s
08/04 Ha 31x600s
08/05 Ha 31x600s
08/06 Ha 30x600s
08/07 Ha 28x600s
08/08 Ha 11x600s
08/10 Ha 18x600s
08/18 Ha 31x600s
08/28 Ha 9x600s
Exposure time 44.0 hrs
* Overall Integration Time
Total: 100.3 hrs
H-Alpha: 44.0 hrs
OIII: 28.4 hrs
SII: 27.9 hrs
Here you can also find Flo's version: Cederblad 214-NGC 7822 (100h Epsilon) SHO
And last but not least some information about the shown area (Wikipedia):
This area is a young star forming complex in the constellation of Cepheus. The complex encompasses the emission region designated Sharpless 171, and the young cluster of stars named Berkeley 59. The complex is believed to be some 800–1,000 pc distant, with the younger components aged no more than a few million years. The complex also includes one of the hottest stars discovered within 1 kpc of the Sun, namely BD+66 1673, which is an eclipsing binary system consisting of an O5V that exhibits a surface temperature of nearly 45,000 K and a luminosity about 100,000 times that of the Sun. The star is one of the primary sources illuminating the nebula and shaping the complex's famed pillars of creation-type formations, the elephant trunks.
Hope you enjoy our little project! :-) Really looking forward to something like that again in future! :-)
Description: full field of view
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Description: detailed close-up
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