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Pierre Auger Observatory Open Data
No full text<p>The Pierre Auger Collaboration is releasing 10% of the data recorded since 2004 using the world's largest cosmic ray detector, the Pierre Auger Observatory, located in Argentina, in the Province of Mendoza. The release also includes 100% of weather and space-weather data collected until 31 December 2020. These data are being made available publicly with the expectation that they will be used by a wide and diverse community including professional and citizen-scientists and for educational and outreach initiatives.</p>
<p>Operation of the Pierre Auger Observatory, by a Collaboration of about 400 scientists from over 90 institutions in 18 countries across the world, has enabled the properties of the highest-energy cosmic rays to be determined with unprecedented precision. These cosmic rays are predominantly the nuclei of the common elements and reach the Earth from astrophysical sources. The data from the Observatory have been used to show that the highest-energy particles have an extra-galactic origin.</p>
<p>Cosmic rays are observed indirectly, through extensive air-showers of secondary particles produced by the interaction of the incoming cosmic ray with the atmosphere. The Surface Detector of the Observatory covers 3000 km<sup>2</sup> and comprises an array of ~1600 particle detectors, separated by 1500 m. The low energy extension features an array of 71 stations spread apart by 750 m and covering about 27 km<sup>2</sup>. The area is overlooked by a set of telescopes that compose the Fluorescence Detector which is sensitive to the auroral-like light emitted as the air-shower develops, while the Surface Detector is sensitive to muons, electrons and photons that reach the ground.</p>
<p>The Open Data released here include those from these instruments. They have been subjected to the same selection and reconstruction procedures used by the Collaboration in recent publications. They amount to more than 80000 showers measured with the surface-detector arrays and more than 3000 showers recorded simultaneously by the surface and fluorescence detectors. Data are available as pseudo-raw (JSON) format and as a summary CSV file containing the reconstructed shower parameters. Simplified codes derived from the ones used for published analyses are also provided, by means of Python notebooks that have been prepared to guide the reader to an understanding of the physics results. An outreach section dedicated to the general public, and in particular to school students, is also available and includes simple tools to enjoy our data. To get more details about the Observatory and the Open Data, you can visit <a href="https://opendata.auger.org/">the dedicated website</a>.</p>
<p><strong>About the Auger Open Data</strong></p>
<p>Downloadable datasets</p>
<ul>
<li> Cosmic-ray data:
<ul>
<li>Pseudo-raw data: for each event, a list of SD stations, with their relevant PMT traces, is available. If an event is detected simultaneously with the SD and FD it is called a hybrid event and a list of FD telescopes with a camera view is also provided. The main parameters from the SD and FD reconstruction are also given. The 'ready-to-use' Event Display is a good way to become familiar with the Open Data.</li>
<li>Reconstructed data: for each event, only 'high-level' information is provided. Different parameters are extracted from the pseudo-raw dataset to be used in physics analysis. Examples on how to use them can be found in the Analysis page.</li>
</ul>
</li>
<li>Atmospheric data:
<ul>
<li>Pseudo-raw data: the values of different atmospheric state-variables, recorded using each of the five weather stations, are available.</li>
<li>Processed data: the values of the different atmospheric state- variables, obtained by merging the information from the different weather stations, are provided.</li>
</ul>
</li>
<li>Scaler data: the counting rate of the surface detectors over 15 minutes, averaged over the active detectors, is provided.</li>
<li>Auxiliary data: these are additional data necessary for a full physics analysis but that are not extracted directly from the raw data. They include the position of the SD stations, the position of the FD pixels, the SD exposure, the FD acceptance.</li>
</ul>
<p>Pseudo-raw and reconstructed data are provided in JSON format. Reconstructed data are also available in CSV format, representing a “summary” of the JSON files and containing the information that is needed for analysis. Similarly, auxiliary data are in CSV format. Format description is available on <a href="https://opendata.auger.org/">the dedicated website</a>.</p>
<p>Tools</p>
<ul>
<li><a href="https://opendata.auger.org/display.php">Ready-to-use event display</a></li>
<li><a href="https://opendata.auger.org/analysis.php">Simple software</a>, reading the JSON and CSV files and producing examples of basic histograms of different data parameters</li>
<li><a href="https://opendata.auger.org/analysis.php">Analysis examples</a>, reading the reconstructed data and producing derived data and graphs</li>
</ul>
<p>Other Auger Open Data</p>
<ul>
<li>All <a href="https://auger.org/index.php/science/journal-articles">Auger publications</a> are available as Open Access. Some of them also include Open Data in the form of additional tables, plots, graphs.</li>
</ul>
<p>Disclaimer</p>
<ul>
<li>The Open Data are released under the (<a href="http://creativecommons.org/licenses/by-sa/4.0/">CC BY-SA 4.0</a>) International License.</li>
<li>All datasets have a unique DOI that you are requested to cite in any applications or publications.</li>
<li>The Auger Collaboration does not endorse any work, scientific or otherwise, produced using these data, even if available on, or linked from, this portal.</li>
<li>The spreadsheet-based datasets allow the user to undertake basic analyses. More complex analyses however require some knowledge of the underlying physics and of the instruments.</li>
<li>The analysis methods, including the reconstruction of the data, have evolved over time, and will continue to evolve. The reconstructed Open Data are processed with the most up-to-date software. Updates are thus foreseen, for either the reconstructed data or the software needed to analyse them. These will be detailed in later releases.</li>
<li>If you are interested in joining or working with the Auger Collaboration, please contact [email protected].</li>
</ul>
<p>Policy </p>
<p>The policy of the Auger Collaboration on Data Release and Open Access can be found <a href="https://opendata.auger.org/AugerOpenDataPolicy.pdf">here</a>.</p>
<p><strong>Contact</strong></p>
<p>For any question/doubt about these data, feel free to check the <a href="https://opendata.auger.org/about.php">contact page</a> of our website or directly write to [email protected].</p>
<p> </p>
Pierre Auger Observatory 2021 Open Data
No full textThe Pierre Auger Collaboration is releasing 10% of the data recorded since 2004 using the world's largest cosmic ray detector, the Pierre Auger Observatory, located in Argentina, in the Province of Mendoza. The release also includes 100% of weather and space-weather data collected until 31 December 2020. These data are being made available publicly with the expectation that they will be used by a wide and diverse community including professional and citizen-scientists and for educational and outreach initiatives.
Operation of the Pierre Auger Observatory, by a Collaboration of about 400 scientists from over 90 institutions in 18 countries across the world, has enabled the properties of the highest-energy cosmic rays to be determined with unprecedented precision. These cosmic rays are predominantly the nuclei of the common elements and reach the Earth from astrophysical sources. The data from the Observatory have been used to show that the highest-energy particles have an extra-galactic origin.
Cosmic rays are observed indirectly, through extensive air-showers of secondary particles produced by the interaction of the incoming cosmic ray with the atmosphere. The Surface Detector of the Observatory covers 3000 km2 and comprises an array of particle detectors, separated by 1500 m. The area is overlooked by a set of telescopes that compose the Fluorescence Detector which is sensitive to the auroral-like light emitted as the air-shower develops, while the Surface Detector is sensitive to muons, electrons and photons that reach the ground.
The Open Data released here include those from these two instruments. They have been subjected to the same selection and reconstruction procedures used by the Collaboration in recent publications. They amount to more than 20000 showers measured with the surface-detector array and more than 3000 showers recorded simultaneously by the surface and fluorescence detectors. Data are available as pseudo-raw (JSON) format and as a summary CSV file containing the reconstructed shower parameters. Simplified codes derived from the ones used for published analyses are also provided, by means of Python notebooks that have been prepared to guide the reader to an understanding of the physics results. An outreach section dedicated to the general public, and in particular to school students, is also available and includes simple tools to enjoy our data. To get more details about the Observatory and the Open Data, you can visit the dedicated website.
About the Auger Open Data
Downloadable datasets
Cosmic-ray data:
Pseudo-raw data: for each event, a list of SD stations, with their relevant PMT traces, is available. If an event is detected simultaneously with the SD and FD it is called a hybrid event and a list of FD telescopes with a camera view is also provided. The main parameters from the SD and FD reconstruction are also given. The 'ready-to-use' Event Display is a good way to become familiar with the Open Data.
Reconstructed data: for each event, only 'high-level' information is provided. Different parameters are extracted from the pseudo-raw dataset to be used in physics analysis. Examples on how to use them can be found in the Analysis page.
Atmospheric data:
Pseudo-raw data: the values of different atmospheric state-variables, recorded using each of the five weather stations, are available.
Processed data: the values of the different atmospheric state- variables, obtained by merging the information from the different weather stations, are provided.
Scaler data: the counting rate of the surface detectors over 15 minutes, averaged over the active detectors, is provided.
Auxiliary data: these are additional data necessary for a full physics analysis but that are not extracted directly from the raw data. They include the position of the SD stations, the position of the FD pixels, the SD exposure, the FD acceptance.
Pseudo-raw and reconstructed data are provided in JSON format. Reconstructed data are also available in CSV format, representing a “summary” of the JSON files and containing the information that is needed for analysis. Similarly, auxiliary data are in CSV format. Format description is available on the dedicated website.
Tools
Ready-to-use event display
Simple software, reading the JSON and CSV files and producing examples of basic histograms of different data parameters
Analysis examples, reading the reconstructed data and producing derived data and graphs
Other Auger Open Data
All Auger publications are available as Open Access. Some of them also include Open Data in the form of additional tables, plots, graphs.
Disclaimer
The Open Data are released under the (CC BY-SA 4.0) International License.
All datasets have a unique DOI that you are requested to cite in any applications or publications.
The Auger Collaboration does not endorse any work, scientific or otherwise, produced using these data, even if available on, or linked from, this portal.
The spreadsheet-based datasets allow the user to undertake basic analyses. More complex analyses however require some knowledge of the underlying physics and of the instruments.
The analysis methods, including the reconstruction of the data, have evolved over time, and will continue to evolve. The reconstructed Open Data are processed with the most up-to-date software. Updates are thus foreseen, for either the reconstructed data or the software needed to analyse them. These will be detailed in later releases.
If you are interested in joining or working with the Auger Collaboration, please contact [email protected].
Policy
The policy of the Auger Collaboration on Data Release and Open Access can be found here.
Contact
For any question/doubt about these data, feel free to check the contact page of our website or directly write to [email protected]
Anisotropy studies around the galactic centre at EeV energies with the Auger Observatory
No full textData from the Pierre Auger Observatory are analyzed to search for anisotropies near the direction of the Galactic Centre at EeV energies. The exposure of the surface array in this part of the sky is already significantly larger than that of the fore-runner experiments. Our results do not support previous findings of localized excesses in the AGASA and SUGAR data. We set an upper bound on a point-like flux of cosmic rays arriving from the Galactic Centre which excludes several scenarios predicting sources of EeV neutrons from Sagittarius A. Also the events detected simultaneously by the surface and fluorescence detectors (the ‘hybrid’ data set), which have better pointing accuracy but are less numerous than those of the surface array alone, do not show any significant localized excess from this direction.http://www.elsevier.com/wps/find/journaldescription.cws_home/523319/description#descriptio
Symmetry characterization of unoccupied states in thick alkaline layers by spin-resolved Auger electron spectroscopy using primary excitation by circularly polarized light
No full textStoppmanns P, David R, Müller N, Heinzmann U, Grieb H, Noffke J. Symmetry characterization of unoccupied states in thick alkaline layers by spin-resolved Auger electron spectroscopy using primary excitation by circularly polarized light. Journal of physics: condensed matter. 1994;6(23):4225-4232.CVV Auger electrons emitted from K, Rb and Cs layers are studied using spin-resolved spectroscopy. Oriented 3p, 4p and 5p hole states are excited by circularly polarized radiation in normal incidence. The photon energies range from 12 to 24 eV. With all three materials, the degree and sign of the Auger electron spin polarization vary with the photon energy. As an atomic model of the Auger process predicts, and as a comparison of measurements with the calculated densities of states shows, the spin polarization is essentially determined by the symmetry of the final states reached in the primary (photo)excitation. Just above the excitation threshold, the preferential spin direction of the Auger electrons is measured to be parallel to the spin of the exciting photons corresponding to a predominantly s-like symmetry of the unoccupied final states reached by the excitation. At higher photon energies the preferential spin direction changes to be antiparallel to the photon spin, corresponding to the mainly d-like symmetry of unoccupied states reached by the excitation
Results from the Pierre Auger Observatory
No full texthe Pierre Auger Observatory has been designed to investigate the origin and the nature of Ultra High Energy Cosmic Rays using a hybrid detection technique. It islocated in the Province of Mendoza, Argentina, and consists of a surface array of about 3000 km2 overlooked by 27 air fluorescence telescopes grouped in four sites, which together provide a powerful instrument for air shower reconstruction. The combination of information from the surface array, measuring the lateral distributions of secondary particles at the ground, and the fluorescence telescopes, observing the longitudinal profile, enhances the reconstruction capability with respect to the individual detector components. Ultra High Energy Cosmic Rays offer also the unique chance of investigating particle interactions over an energy range well beyond the one covered by present and future ground-based particle accelerators. A review of selected results is presented with the emphasis given to the measurement of energy spectrum, arrival directions, chemical composition and the search for photons and neutrinos as primary particles
Multiparametric topological analysis (MTA) for the study of the primary CR composition: Performances with Auger simulated data
No full textWe describe the application of a multiparametric analysis to estimate the UHE Cosmic Rays composition. The proposed method, MTA (Multiparametric Topological Analysis), is based on the study of the correlations among different shower observables. This technique is designed to fully exploit the complementarity of Auger fluorescence and ground array data. In the present work, we report the results of the application to Conex showers, fully simulated through the Auger detector, using only parameters describing the longitudinal development of air showers as recorded by fluorescence detector for hybrid data
Antennas for the detection of radio emission pulses from cosmic-ray induced air showers at the Pierre Auger Observatory
No full textThe Pierre Auger Observatory is exploring the potential of the radio detection technique to study extensive air showers induced by ultra-high energy cosmic rays. The Auger Engineering Radio Array (AERA) addresses both technological and scientific aspects of the radio technique. A first phase of AERA has been operating since September 2010 with detector stations observing radio signals at frequencies between 30 and 80 MHz. In this paper we present comparative studies to identify and optimize the antenna design for the final configuration of AERA consisting of 160 individual radio detector stations. The transient nature of the air shower signal requires a detailed description of the antenna sensor. As the ultra-wideband reception of pulses is not widely discussed in antenna literature, we review the relevant antenna characteristics and enhance theoretical considerations towards the impulse response of antennas including polarization effects and multiple signal reflections. On the basis of the vector effective length we study the transient response characteristics of three candidate antennas in the time domain. Observing the variation of the continuous galactic background intensity we rank the antennas with respect to the noise level added to the galactic signal
The Rapid Atmospheric Monitoring System of the Pierre Auger Observatory
No full textThe Pierre Auger Observatory is a facility built to detect air showers produced by cosmic rays above 1017 eV. During clear nights with a low illuminated moon fraction, the UV fluorescence light produced by air showers is recorded by optical telescopes at the Observatory. To correct the observations for variations in atmospheric conditions, atmospheric monitoring is performed at regular intervals ranging from several minutes (for cloud identification) to several hours (for aerosol conditions) to several days (for vertical profiles of temperature, pressure, and humidity). In 2009, the monitoring program was upgraded to allow for additional targeted measurements of atmospheric conditions shortly after the detection of air showers of special interest, e. g., showers produced by very high-energy cosmic rays or showers with atypical longitudinal profiles. The former events are of particular importance for the determination of the energy scale of the Observatory, and the latter are characteristic of unusual air shower physics or exotic primary particle types. The purpose of targeted (or "rapid") monitoring is to improve the resolution of the atmospheric measurements for such events. In this paper, we report on the implementation of the rapid monitoring program and its current status. The rapid monitoring data have been analyzed and applied to the reconstruction of air showers of high interest, and indicate that the air fluorescence measurements affected by clouds and aerosols are effectively corrected using measurements from the regular atmospheric monitoring program. We find that the rapid monitoring program has potential for supporting dedicated physics analyses beyond the standard event reconstruction
Fluorescence detector optical calibration and atmospheric monitoring for the Pierre Auger experiment
No full textJune 30, 2000/Rev. January 5, 200
Muons in air showers at the Pierre Auger Observatory: mean number in highly inclined events
No full textWe present the first hybrid measurement of the average muon number in air showers at ultrahigh energies, initiated by cosmic rays with zenith angles between 62° and 80°. The measurement is based on 174 hybrid events recorded simultaneously with the surface detector array and the fluorescence detector of the Pierre Auger Observatory. The muon number for each shower is derived by scaling a simulated reference profile of the lateral muon density distribution at the ground until it fits the data. A 1019??????eV shower with a zenith angle of 67°, which arrives at the surface detector array at an altitude of 1450 m above sea level, contains on average (2.68±0.04±0.48(sys))×107 muons with energies larger than 0.3 GeV. The logarithmic gain dlnN??/dlnE of muons with increasing energy between 4×1018??????eV and 5×1019??????eV is measured to be (1.029±0.024±0.030(sys))
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