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| G189.1+03.0C
Common Name: IC 443 Distance: 1.5kpc( )Position of Central Source (J2000): ( 06 18 04.3, 22 27 24.1 )X-ray size: 0.4'x0.4'Description: bright region within IC 443 | |
| Not available | 
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Radio | X-Ray |
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| Summary of Chandra Observations
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Sequence | Obs. ID | Detectors Used | Exposure uf
(ks) | Exposure f
(ks) | Date
Observed | Aimpoint (J2000)
(RA, Dec) | | 500494
| 4675
| ACIS-235678
| 58.6 | 58.4 | 2004-04-12 | ( 06 18 04.3, 22 27 32.8 ) |
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 | Exposureuf => Exposure time of unfiltered event file
Exposuref => Exposure time of filtered event file | |
| This a bright region within the large remnant IC 443.(IC 443 is 45' in diameter)This region contains a knot (just resolved). A point source contribution from PSR is possible.
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| Chandra Event File
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 Click left mouse button on hyperlink below to download file | |
Obs. ID | Event 2 FITS File
(un-filtered) | Event 2 FITS File
(filtered) | AUX file
(asol, badpix etc.) | | 4675 | 55.5 MB | 15.1 MB | 15.0 MB |
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| Chandra Counts and Fluxes
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Region | Energy Range
(keV) | Signal
(counts) | Rate
(counts s-1) | FabsX
(ergs cm-2s-1) | FX
(ergs cm-2s-1) | LX
(ergs s-1) | | | 0.3 - 10.0 | 2.942e+03 | 5.042e-02 | 7.35e-13 | 9.43e-13 | 2.53e+32 |
| 0.3 - 2.1 | 1.635e+03 | 2.802e-02 | 1.20e-13 | 3.09e-13 | 8.29e+31 |
| 2.1 - 10.0 | 1.361e+03 | 2.332e-02 | 6.17e-13 | 6.35e-13 | 1.70e+32 |
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| NH = 0.4(1022 cm-2) Assumed distance: 1.5kpc ( ) |
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| Chandra Images
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| Images in Several Energy BandsTrue Color ImageEquivalent Width Map
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Chandra Spectra | |
| Spectra of Several Regions
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Other Wavelengths | |
| Radio ImagesSurvey Missions
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Compact Sources | |
Obs. ID | Position (J2000) | Size | Net Count | Count rate | Note | | 4675 | |
| ( 06 17 59.3, 22 27 38.9 ) | < 1.0" | 320.0 | 5.46e-03 | |
| ( 06 18 04.3, 22 27 24.1 ) | < 1.0" | 205.0 | 3.50e-03 | pulsar? |
| ( 06 18 04.6, 22 27 31.8 ) | < 1.0" | 135.0 | 2.30e-03 | star? |
| ( 06 18 06.5, 22 28 28.3 ) | < 1.0" | 1000.0 | 1.71e-02 | |
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This list is not complete. Sources are obvious and usually within or close to the remnant. The size refers to the appearance of the source and can be larger for off-axis sources.
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References | |
| Bykov et al. 2005, ApJ, 624, L41 : Chandra
