Monthly Archives: October 2014

NGC 281


NGC 281 is an H II region in the constellation of Cassiopeia and part of the Perseus Spiral Arm. It includes the open cluster IC 1590, the multiple star HD 5005, and several Bok globules. Colloquially, NGC 281 is also known as the Pacman Nebula for its resemblance to the video game character.

The nebula was discovered in August 1883 by E. E. Barnard, who described it as “a large faint nebula, very diffuse.” The multiple star HD 5005, also called \beta1, was discovered by S. W. Burnham. It consists of an 8th-magnitude primary with four companions at distances between 1.4 and 15.7 seconds of arc. There has been no appreciable change in this quintuple system since the first measurements were made in 1875.

The nebula is visible in amateur telescopes from dark sky locations. In his book Deep Sky Wonders, Walter Scott Houston describes the appearance of the nebula in small telescopes

Imaging telescopes or lenses: Altair Astro Wave Series 115 F7 ED Triplet APO
Imaging cameras: Canon EOS 600Da
Mounts: SkyWatcher NEQ6 pro Goto
Guiding telescopes or lenses: Orion Mini 50mm Guide Scope
Guiding cameras: Starshoot Autoguider
Focal reducers: Altair Astro PlanoStar 3″ Flattener
Software: Astrotortilla, DeepSky Stacker 3.3.3 Deep Sky Stacker 3.3.3, Photoshop CS5
Resolution: 4906×3193
Frames: 70×600″
Integration: 11.7 hours
RA center: 13.234 degrees
DEC center: 56.578 degrees
Pixel scale: 1.093 arcsec/pixel
Orientation: 81.918 degrees
Field radius: 0.889 degrees

Astrophotography of the day of  SPONLI, 31.10.2014

The Sun online and activity solar.30.10.2014



Seven M-class flares and six C-class flares were counted since the last bulletin. An M3.5 flare was the largest flare, peaking at 1:35 UT, originating from Catania sunspot group 88 (NOAA AR 2192). Catania group 88 is currently located at the west limb and although it is difficult to determine it’s characteristics, the region seems to have shrinked. All other regions on the front side of the solar disk were relatively stable. Catania group 88 is still capable to produce large flares, mainly at the M-level, with a minor chance for another X-flare. We retain the warning condition for a proton event. No Earth-directed CMEs were observed in coronagraphic imagery.The solar wind speed observed by ACE is low at around 350 km/s. The interplanetary magnetic field has a magnitude of about 5 nT. A sector boundary crossing is observed at about 08:00 UT on October 30 as the phi angle changed from a mostly positive to negative orientation. Mostly quiet geomagnetic conditions are expected, with a chance for an isolated time slot of active conditions (K=4).



Crescent Nebula


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.[2] 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 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.

Imaging telescopes or lenses: Borg 125ED
Imaging cameras: Canon 600D
Mounts: Celestron Advanced VX
Guiding telescopes or lenses: Borg Mini-50
Guiding cameras: SBIG SG-4
Software: Adobe Photoshop 6 CS, Stark Labs Nebulosity
Filters: Astronomik UHC, Baader Ha
Resolution: 2452×1589
Dates: Oct. 18, 2014, Oct. 19, 2014
Locations: Home
Baader Ha: 16×300″ ISO800 bin 1×1
Astronomik UHC: 28×180″ ISO800
Integration: 2.7 hours
Darks: ~50
Avg. Moon age: 24.55 days
Avg. Moon phase: 25.68%
Mean SQM: 18.41
Temperature: 18.00
RA center: 303.165 degrees
DEC center: 38.480 degrees
Orientation: -92.125 degrees
Field radius: 0.903 degrees

Автор: Chris Bernardi

Astrophotography of the day of  SPONLI, 30.10.2014

The Sun online and activity solar.29.10.2014

солнце 29 октября

Solar activity has slightly reduced in the past 24 hours, with three M-class and two C-class flares. Activity mainly originated from  Catania sunspot group 88 (NOAA AR 2192). A narrow CME was observed in SOHO/LASCO-C2 imagery (first measurement at October 28 20:24 UT), with a projected speed of 388 km/s (CACTus estimate). The CME is travelling to the northeast of the Sun-Earth line. The CME is believed to be associated with activity at the backside of the Sun and as such no effect on Earth is expected. Catania group 88 still has potential to produce strong flares up to the X-level. Due to it’s location close to the West limb, a strong eruption may result in a rise of the proton flux. Earth is currently inside a slow solar wind, with solar wind speed decreasing from 450 km/s to currently around 350 km/s. The interplanetary magnetic field has a magnitude of about 5 nT with fluctuating Bz values. Quiet geomagnetic conditions are observed and are expected to continue.

Trifid Nebula

9e2125a425704817e85c0288683b1143.1824x0_q100_watermark_watermark_opacity-10_watermark_position-6_watermark_text-Copyright Rafael Compassi

The Trifid Nebula (catalogued as Messier 20 or M20 and as NGC 6514) is an H II region located in Sagittarius. It was discovered by Charles Messier on June 5, 1764. Its name means ‘divided into three lobes’. The object is an unusual combination of an open cluster ofstars; 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 trifurcated appearance; these are also designated Barnard 85). Viewed through a small telescope, the Trifid Nebula is a bright and peculiar object, and is thus a perennial favorite of amateur astronomers.

Imaging telescopes or lenses: GSO 12″ Reflector GSO 12″ F/5
Imaging cameras: Canon EOS 1000D / Rebel XS
Mounts: Homemade equatorial mount German Equatorial from Darío Pires
Software: Adobe Photoshop CS6, DeepSky Stacker 3.3.2 DeepSkyStacker V 3.2.2
Resolution: 3888×2592
Dates: Oct. 20, 2014
Locations: Eimer Sternen Observatory
Frames: 17×30″
Integration: 0.1 hours
Avg. Moon age: 25.89 days
Avg. Moon phase: 14.28%
RA center: 270.641 degrees
DEC center: -22.979 degrees
Pixel scale: 0.780 arcsec/pixel
Orientation: -59.289 degrees
Field radius: 0.506 degrees

Аuthor: RCompassi
Astrophotography of the day of SPONLI, 29.10.2014

The Sun online and activity solar.28.10.2014



Another X-class flare was produced by Catania sunspot group 88 (NOAA AR 2192); an X2.1 flare peaked at 14:47 UT on October 27. Also three M-class and several C-class flares were added to the activity list of this region. No associated CME was observed, nor was there an increase in proton flux. The region Lf-nh7 retains its area and magnetic complexity and has still high potential to produce additional flares up to the X-level. It is currently located close to the West limb and a strong eruption may result in a rise of the proton flux.  The extended filament in the northern hemisphere has the potential to lift off and produce an Earth-directed CME.  Earth is inside a slow solar wind, with a speed near 400 km/s. The interplanetary magnetic field magnitude reaches values up to 8 nT, with an often southward oriented Bz. Mostly quiet geomagnetic conditions are observed, with a few isolated time slots of active (K=4, measured at Dourbes) conditions. Quiet to active conditions are  expected to continue.

Equipment: Coronado 90 +  Imaging Source DMK  + LX75
Processing: Photoshop, Avistack 300 frames
Date: 28/10/14
Exposure 1/500 sec.


Flame Nebula


The Flame Nebula, designated as NGC 2024 and Sh2-277, is an emission nebula in the constellation Orion. It is about 900 to 1,500 light-years away.

The bright star Alnitak (ζ Ori), the easternmost star in the Belt of Orion, shines energetic ultraviolet light into the Flame and this knocks electrons away from the great clouds of hydrogen gas that reside there. Much of the glow results when the electrons and ionized hydrogen recombine. Additional dark gas and dust lies in front of the bright part of the nebula and this is what causes the dark network that appears in the center of the glowing gas. The Flame Nebula is part of the Orion Molecular Cloud Complex, a star-forming region that includes the famous Horsehead Nebula.

Imaging telescopes or lenses: Orion USA 102ED F7.0
Imaging cameras: Canon 550D, Atik 314L+
Mounts: Skywatcher HEQ5 SynScan
Guiding telescopes or lenses: Orion USA 50mm Guide Scope
Guiding cameras: Imaging Source DBK41AU02.AS
Software: DeepSky Imaging DeepSky Stacker
Filters: Orion H‑Alpha 7nm
Resolution: 1351×999
Dates: Oct. 19, 2014
Locations: Apartment, Brazilian Astrophotography Meeeting
Frames: 30×300″
Integration: 2.5 hours
Avg. Moon age: 24.99 days
Avg. Moon phase: 21.56%

Аuthor: Rodrigo Andolfato

Astrophotography of the day of SPONLI, 28.10.2014

Eagle Nebula


The Eagle Nebula (catalogued as Messier 16 or M16, and as NGC 6611, and also known as the Star Queen Nebula) 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 that is thought to resemble an eagle. It contains several active star-forming gas and dust regions, including the famous “Pillars of Creation”, photographed by the Hubble Space Telescope.

The Eagle Nebula is part of a diffuse emission nebula, or H II region, which is catalogued as IC 4703. This region of active current star formation is about 7000 light-years distant. The tower of gas that can be seen coming off the nebula is approximately 9.5 light-years or about 90 trillion kilometers long.

Imaging telescopes or lenses: GSO 10″ RC 10
Imaging cameras: QSI 583 wsg
Mounts: Astro-Physics 1200 GTO
Guiding cameras: Starlight Xpress Lodestar
Software: Adobe Photoshop CC, PixInsight, DC-3 Dreams ACP Observatory Control Software
Filters: Astrodon RGB filter set
Resolution: 2451×1770
Dates: Oct. 19, 2014
Locations: Deep Sky Observatory
Frames: 9×600″
Integration: 1.5 hours
Avg. Moon age: 24.99 days
Avg. Moon phase: 21.56%
RA center: 274.702 degrees
DEC center: -13.792 degrees
Pixel scale: 0.744 arcsec/pixel
Orientation: -179.374 degrees
Field radius: 0.312 degrees

Аuthor: Dean Salman, 27.10.2010

Astrophotography of the day of  SPONLI

The Sun online and activity solar.26.10.2014



In the past 24 hours, Catania sunspot group 88 (NOAA AR 2192) produced two
X-class flares: X1.0 peaking at 17:08 UT yesterday and X2.0 peaking at
10:56 UT today. Neither of the flares seems to be associated with an
Earth-directed CME. The area of the Catania sunspot group 88 increases
again, and it maintains the beta-gamma-delta configuration of its
photospheric magnetic field, so we expect the flaring activity up to
X-level from this sunspot group. As the Catania sunspot group 88 is
currently situated in the western solar hemisphere, a major eruption in
this active region may lead to a proton event. A long filament in the
northern hemisphere is continuing its passage across the solar central
meridian. Its possible eruption may lead to an Earth-directed CME. The
Earth is currently inside a slow (around 370 km/s) solar wind flow with
slightly elevated (around 7 nT) interplanetary magnetic field magnitude.
The geomagnetic conditions are quiet and are expected to remain  so, with
isolated intervals of active (K = 4) geomagnetic conditions possible but
not very likely.

Equipment: Coronado 90 +  Imaging Source DMK  + LX75
Processing: Photoshop, Avistack 300 frames
Date: 26/10/14
Exposure 1/500 sec.

Observatory Sponli

Veil Nebula


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.

The Hubble Space Telescope captured several images of the nebula. The analysis of the emissions from the nebula indicate the presence of oxygen, sulfur, and hydrogen. This is also one of the largest, brightest features in the x-ray sky.

Imaging telescopes or lenses: Explore Scientific ES102ED APO
Imaging cameras: Canon EOS T3i DSLR 600D
Mounts: Celestron CGEM DX Mount
Guiding cameras: Orion Awesome 80mm Refractor Starshoot Autoguider
Software: GIMP
Resolution: 1303×869
Dates: Oct. 15, 2014
Locations: The Sky’s the Limit
Frames: 33×240″
Integration: 2.2 hours
Avg. Moon age: 21.41 days
Avg. Moon phase: 57.78%
RA center: 314.075 degrees
DEC center: 31.706 degrees
Orientation: -74.439 degrees
Field radius: 1.099 degrees

Аuthor: astronomynut, 26.10.2014

Аstrophotography of the day of SPONLI