Cookie consent

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
Contains:  IC 443
Getting plate-solving status, please wait...
IC443 JellyFish Nebula - HSS, 


            Jerry Macon
IC443 JellyFish Nebula - HSS

IC443 JellyFish Nebula - HSS

Technical card

Imaging telescope or lens:Tele Vue NP127is

Imaging camera:ZWOASI1600M-C

Mount:Losmandy Titan

Guiding telescope or lens:Tele Vue NP127is

Guiding camera:Starlight Xpress Lodestar X2 Mono

Software:Sequence Generator ProPixInsight 1.8PHD Guiding 2

Filters:Baader SIIHa

Accessory:Starlight Xpress SXV-AOFL

Resolution: 3696x2804

Dates:Jan. 14, 2018

Ha: 23x400" (gain: 99.00) -25C bin 1x1
Baader SII: 23x400" (gain: 99.00) -25C bin 1x1

Integration: 5.1 hours

Avg. Moon age: 27.21 days

Avg. Moon phase: 5.98%

Bortle Dark-Sky Scale: 4.00 job: 1902727

RA center: 94.274 degrees

DEC center: 22.500 degrees

Pixel scale: 1.182 arcsec/pixel

Orientation: 269.569 degrees

Field radius: 0.761 degrees

Locations: Dark Star Observatory, Taos, New Mexico, United States


Mapping is:
R: Ha G: (Ha+SIII)/2 B: SIII
Then remove green tint using SCNR.

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 plan 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.

The SNR optical and radio morphology is shell-like, 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.
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.



Jerry Macon
License: Attribution Creative Commons

Sky plot

Sky plot


IC443 JellyFish Nebula - HSS, 


            Jerry Macon