MAGIC Gamma Telescope
Donated on 4/30/2007
Data are MC generated to simulate registration of high energy gamma particles in an atmospheric Cherenkov telescope
Dataset Characteristics
Multivariate
Subject Area
Physics and Chemistry
Associated Tasks
Classification
Feature Type
Real
# Instances
19020
# Features
10
Dataset Information
Additional Information
The data are MC generated (see below) to simulate registration of high energy gamma particles in a ground-based atmospheric Cherenkov gamma telescope using the imaging technique. Cherenkov gamma telescope observes high energy gamma rays, taking advantage of the radiation emitted by charged particles produced inside the electromagnetic showers initiated by the gammas, and developing in the atmosphere. This Cherenkov radiation (of visible to UV wavelengths) leaks through the atmosphere and gets recorded in the detector, allowing reconstruction of the shower parameters. The available information consists of pulses left by the incoming Cherenkov photons on the photomultiplier tubes, arranged in a plane, the camera. Depending on the energy of the primary gamma, a total of few hundreds to some 10000 Cherenkov photons get collected, in patterns (called the shower image), allowing to discriminate statistically those caused by primary gammas (signal) from the images of hadronic showers initiated by cosmic rays in the upper atmosphere (background). Typically, the image of a shower after some pre-processing is an elongated cluster. Its long axis is oriented towards the camera center if the shower axis is parallel to the telescope's optical axis, i.e. if the telescope axis is directed towards a point source. A principal component analysis is performed in the camera plane, which results in a correlation axis and defines an ellipse. If the depositions were distributed as a bivariate Gaussian, this would be an equidensity ellipse. The characteristic parameters of this ellipse (often called Hillas parameters) are among the image parameters that can be used for discrimination. The energy depositions are typically asymmetric along the major axis, and this asymmetry can also be used in discrimination. There are, in addition, further discriminating characteristics, like the extent of the cluster in the image plane, or the total sum of depositions. The data set was generated by a Monte Carlo program, Corsika, described in: D. Heck et al., CORSIKA, A Monte Carlo code to simulate extensive air showers, Forschungszentrum Karlsruhe FZKA 6019 (1998). http://rexa.info/paper?id=ac6e674e9af20979b23d3ed4521f1570765e8d68 The program was run with parameters allowing to observe events with energies down to below 50 GeV.
Has Missing Values?
No
Variables Table
| Variable Name | Role | Type | Description | Units | Missing Values |
|---|---|---|---|---|---|
| fLength | Feature | Continuous | major axis of ellipse | mm | no |
| fWidth | Feature | Continuous | minor axis of ellipse | mm | no |
| fSize | Feature | Continuous | 10-log of sum of content of all pixels | #phot | no |
| fConc | Feature | Continuous | ratio of sum of two highest pixels over fSize | no | |
| fConc1 | Feature | Continuous | ratio of highest pixel over fSize | no | |
| fAsym | Feature | Continuous | distance from highest pixel to center, projected onto major axis | no | |
| fM3Long | Feature | Continuous | 3rd root of third moment along major axis | mm | no |
| fM3Trans | Feature | Continuous | 3rd root of third moment along minor axis | mm | no |
| fAlpha | Feature | Continuous | angle of major axis with vector to origin | deg | no |
| fDist | Feature | Continuous | distance from origin to center of ellipse | mm | no |
0 to 10 of 11
Additional Variable Information
1. fLength: continuous # major axis of ellipse [mm] 2. fWidth: continuous # minor axis of ellipse [mm] 3. fSize: continuous # 10-log of sum of content of all pixels [in #phot] 4. fConc: continuous # ratio of sum of two highest pixels over fSize [ratio] 5. fConc1: continuous # ratio of highest pixel over fSize [ratio] 6. fAsym: continuous # distance from highest pixel to center, projected onto major axis [mm] 7. fM3Long: continuous # 3rd root of third moment along major axis [mm] 8. fM3Trans: continuous # 3rd root of third moment along minor axis [mm] 9. fAlpha: continuous # angle of major axis with vector to origin [deg] 10. fDist: continuous # distance from origin to center of ellipse [mm] 11. class: g,h # gamma (signal), hadron (background) g = gamma (signal): 12332 h = hadron (background): 6688 For technical reasons, the number of h events is underestimated. In the real data, the h class represents the majority of the events. The simple classification accuracy is not meaningful for this data, since classifying a background event as signal is worse than classifying a signal event as background. For comparison of different classifiers an ROC curve has to be used. The relevant points on this curve are those, where the probability of accepting a background event as signal is below one of the following thresholds: 0.01, 0.02, 0.05, 0.1, 0.2 depending on the required quality of the sample of the accepted events for different experiments.
Dataset Files
| File | Size |
|---|---|
| magic04.data | 1.4 MB |
| magic04.names | 5.3 KB |
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pip install ucimlrepo
from ucimlrepo import fetch_ucirepo # fetch dataset magic_gamma_telescope = fetch_ucirepo(id=159) # data (as pandas dataframes) X = magic_gamma_telescope.data.features y = magic_gamma_telescope.data.targets # metadata print(magic_gamma_telescope.metadata) # variable information print(magic_gamma_telescope.variables)
Bock, R. (2004). MAGIC Gamma Telescope [Dataset]. UCI Machine Learning Repository. https://doi.org/10.24432/C52C8B.
Creators
R. Bock
DOI
License
This dataset is licensed under a Creative Commons Attribution 4.0 International (CC BY 4.0) license.
This allows for the sharing and adaptation of the datasets for any purpose, provided that the appropriate credit is given.