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| G184.6-05.8
Common Name: Crab Distance: 2kpc(??)Position of Central Source (J2000): ( 05 34 31.9, 22 00 51.8 )X-ray size: 2.3'x2.1'Description: | |
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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) | 500171
| 1994
| ACIS-7
| 4.2 | 4.2 | 2000-11-03 | ( 05 34 31.6, 22 00 56.4 ) |
500173
| 1996
| ACIS-7
| 4.5 | 4.5 | 2000-11-25 | ( 05 34 31.6, 22 00 56.4 ) |
500173
| 1996
| ACIS-7
| 4.5 | 4.5 | 2000-11-25 | ( 05 34 31.6, 22 00 56.4 ) |
500176
| 1999
| ACIS-7
| 4.1 | 4.1 | 2001-01-09 | ( 05 34 31.6, 22 00 56.4 ) |
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| Exposureuf => Exposure time of unfiltered event file Exposuref => Exposure time of filtered event file | |
| The remnant is covered by chip ACIS-S3(CCD_ID=7).Due to usage of the subarray some part of the remnants are missing in some observation.These observation were done with NO aspect dithering.No background light curve filtering was done.It seems that the central source is strongly affected by pileup.
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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.) | 1994 | 265.6 MB | 265.6 MB | 6.2 MB |
1996 | 300.1 MB | 300.1 MB | 7.1 MB |
1998 | 0.0 MB | 0.0 MB | 0.0 MB |
1999 | 275.3 MB | 275.3 MB | 6.3 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) | Total | 0.3 - 10.0 | 9.591e+06 | 2.328e+03 | 1.72e-08 | 2.88e-08 | 1.37e+37 |
0.3 - 2.1 | 7.048e+06 | 1.710e+03 | 5.08e-09 | 1.62e-08 | 7.73e+36 |
2.1 - 10.0 | 2.570e+06 | 6.236e+02 | 1.22e-08 | 1.26e-08 | 6.01e+36 |
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| NH = 0.4(1022 cm-2) Assumed distance: 2kpc (??) |
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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 | 1994 | |
1996 | |
1998 | |
1999 | |
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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 | |
| Mori et al. 2004, ApJ, 609, 186 : Chandra, PWN spectra Seward et al. 2006, ApJ, 652, : Chandra, dust-scattered halo Seward et al. 2006, ApJ, 636, 873 : Chandra, PWN Weisskopf et al. 2001, ApJ, 536L, 81 :