Total integration: 40m
Integration per filter:
- Lum/Clear: 10m (5 × 120s)
- R: 10m (5 × 120s)
- G: 10m (5 × 120s)
- B: 10m (5 × 120s)
Equipment:
- Telescope: Planewave CDK17
- Camera: FLI ML16200
- Filters: Astrodon Gen2 E-Series Tru-Balance Blue 50x50 mm, Astrodon Gen2 E-Series Tru-Balance Green 50x50 mm, Astrodon Gen2 E-Series Tru-Balance Red 50x50 mm, Chroma Lum 50 mm
- Software: Adobe Photoshop, Aries Productions Astro Pixel Processor (APP)
For more information and full resolution: https://app.astrobin.com/i/uiw1nw
A barred Seyfert spiral galaxy with a double ring central structure located in the constellation of Horologium, NGC 1433 was first documented by James Dunlop on 28 September 1826. The double ring is actually tightly wrapped spiral arms that wind into an oval shape along the galaxy’s bar.
At 46 million ly from Earth, it has a very bright active galactic nucleus with an intensive region of active star formation. Star formation is also observed in the spiral arms, but not in the large central bar.
Supernova 2026ahvu (indicated) was discovered on November 2, 2026 by the ALTAS asteroid early impact warning system. ATLAS uses four 0.5m telescopes to image the entire night sky several times a night looking for moving objects. In this case, it found a new object in NGC 1433, and after analysis, it was determined to be a Type Ia supernova.
Type Ia supernova occur in binary systems, where one member is a main sequence star and the other is a white dwarf, the exposed core of a dead star. The white dwarf either siphons matter from the companion star (single-degenerate model) or merges/collides with another white dwarf (double-degenerate model). As the white dwarf approaches the Chandrasekhar limit (about 1.44 times the mass of the Sun), its internal temperature surges, triggering a runaway carbon-oxygen nuclear fusion reaction. The reaction completely obliterates the star within seconds, leaving no central compact remnant like a neutron star or black hole.
Because they consistently explode at nearly the same mass limit, Type Ia supernovae have a very uniform peak brightness. This allows astronomers to use them as "standard candles" to measure the distances to other galaxies. These supernovae are a primary source of iron-peak elements (like nickel-56 and iron-56) in the universe. Much of the iron in the universe, including in human blood, traces back these supernovae.
Unlike core-collapse supernovae from massive stars, Type Ia events are much rarer, occurring roughly once every 500 years in our Milky Way galaxy.
submitted by /u/twilightmoons[link] [comments]