https://github.com/dieterhorns/crab_pheno

Spectral information used for Crab Nebula modelling
https://github.com/dieterhorns/crab_pheno

astrophysics crab gamma-ray multi-wavelength physics

Last synced: 2 months ago
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Spectral information used for Crab Nebula modelling

• Host: GitHub
• URL: https://github.com/dieterhorns/crab_pheno
• Owner: dieterhorns
• Created: 2022-06-21T18:45:08.000Z (over 2 years ago)
• Default Branch: main
• Last Pushed: 2022-11-14T14:10:15.000Z (about 2 years ago)
• Last Synced: 2023-03-05T08:17:59.831Z (almost 2 years ago)
• Topics: astrophysics, crab, gamma-ray, multi-wavelength, physics
• Language: Jupyter Notebook
• Homepage:
• Size: 208 KB
• Stars: 3
• Watchers: 1
• Forks: 0
• Open Issues: 0
• Metadata Files:
  • Readme: README.md

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README

        
# crab_pheno

[![DOI](https://zenodo.org/badge/505965067.svg)](https://zenodo.org/badge/latestdoi/505965067)

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

$\alpha=0.51$. Each line carries a reference code of the paper in the form used by ADS (sth like `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.  ![sed_varalpha (1)](https://user-images.githubusercontent.com/12654998/201674660-6a3d7529-718f-4379-a892-f38653bff8ce.png)

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 $\alpha$ used. First column is the energy in eV, following columns is $I_\nu$ in ergs/s for

the value of alpha indicated in the first row.

Any additional questions directed to [email protected]