If you use the data collection assembled here or the model calculations provided here, please reference our paper:
- L. Dirson and D. Horns* Phenomenological modelling of the Crab Nebula’s broad-band energy spectrum and its apparent extension arXiv:2203.11502_
The data points have been collected from different sources and compiled in a set of files. The files and their are provided as they are without any guarantee that the values are acurate. If you do find inconsistencies or disagreement, please notify us/open an issue.
Within each data file, the units have been adapted to a common format. The units are not identical for the different files. Please find below
additional informations. We have included a sample notebook to read in the files and overplot the best fitting model from the publication for
1972ApJ...171...41M).
-
radio_data.csv: Frequency (in GHz), flux (in Jy), flux uncertainty (in Jy), epoch of observation, reference. Note, the fluxes have not been corrected for secular decline which is typically 0.1% per year. -
ir_data.csv: Wavelength (in Angstrom), flux (in Jy), flux uncertainty (in Jy), reference. -
optical_data.csv: Wavelength (in Angstrom), (corrected) flux (in Jy), absorption (in mag from 1993A&A...270..370V), ref, re-calculated absorption (in mag) from O94 model using$A_v=1.08$ ,$E_{B-V}=0.43$ -
xray_data.csv: Energy (in keV), photoel. absorption corrected energy flux (keV/cm$^2$/s), uncertainty, reference. -
gamma_data.csv: Energy (in GeV), energy flux (in erg/cm$^2$/s), uncertainty, reference. -
sample_plot.ipynb: should be self-explanatory. Req. py3.
In addition to the data, we have included the set of curves shown in Fig. 
as two separate tables synctable.txt for the synchrotron
emission and ictable.txt for the inverse Compton emission.
The first row indicates the sequence of values for
Any additional questions directed to dieter.horns@uni-hamburg.de