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Name / Constellation

IC 443

Other: Sh2-248


Coordinates AR: 06h 17m 13s - Dec: +22° 31′ 05″
Optics Takahashi FSQ 106N APO Fluorite F5 - 60/220 guiding refractor
Camera-Mount SBIG STF8300M - Orion StarShot Guider - 10Micron GM2000 QCI Mount
Filters Baader Ha - Oxy3
  • H alpha
  • Oxy 3
  • 13 x 900 sec - 3 hours 15 min
  • 16 x 900 sec - 4 hours
Location / Date Promiod (Valle D'Aosta-Italy) "TLP" Remote Observatory - 27 oct 2019 (Ha) - 06 dec 2019 (O3)
Seeing About 4" @ 2.1 arcosec/pixel unbinned
Note Bi-color palette Oxy3 - Ha
Acquisition MaxIm DL - CCD Autopilot 5
Processing Adobe Photoshop CC-

IC 443 (also known as the Jellyfish Nebula and Sharpless 248 (Sh2-248)) is a galactic supernova remnant(SNR) in the constellation Gemini. On the plane of the sky, it is located near the star Eta Geminorum. Its distance is roughly 5,000 light years from Earth. 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. C 443 is an extended source, having an angular diameter of 50 arcmin(by comparison, the full moon is 30 arcmin across). At the estimated distance of 5,000 ly (1,500 parsec) from Earth, it corresponds to a physical size of roughly 70 light years (20 parsec). The SNR optical and radio morphology is shell-like (e.g. a prototypical shell-like SNR is SN 1006), consisting of two connected sub-shells with different centers and radii. A third, larger sub-shell—initially attributed to IC 443—is now recognized as a different and older (100,000 years) SNR, called G189.6+3.3.
Notably, IC 443 X-ray morphology is centrally peaked and a very soft X-ray shell is barely visible. Unlike plerion remnants, e.g. the Crab Nebula, the inner X-ray emission is not dominated by the central pulsar wind nebula. It has indeed a thermal origin. IC 443 shows very similar features to the class of mixed morphology SNRs. Both optical and X-ray emission are heavily absorbed by a giant molecular cloud in the foreground, crossing the whole remnant body from northwest to southeast. The remnant's age is still uncertain. There is some agreement that the progenitor supernova happened between 3,000 and 30,000 years ago. Recent Chandra and XMM-Newton observations identified a plerion nebula, close to the remnant southern rim. The point source near the apex of the nebula is a neutron star, relic of a SN explosion. The location in a star forming region and the presence of a neutron star favor a Type II supernova, the ultimate fate of a massive star, as the progenitor explosion.