196,152 research outputs found
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>
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
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
Fluorescence detector optical calibration and atmospheric monitoring for the Pierre Auger experiment
No full textJune 30, 2000/Rev. January 5, 200
The Central Laser Facility at the Pierre Auger Observatory
No full textThe Central Laser Facility is located near the middle of the Pierre Auger Observatory in Argentina. It features a UV laser and optics that direct a beam of calibrated pulsed light into the sky. Light scattered from this beam produces tracks in the Auger optical detectors which normally record nitrogen fluorescence tracks from cosmic ray air showers. The Central Laser Facility provides a "test beam" to investigate properties of the atmosphere and the fluorescence detectors. The laser can send light via optical fiber simultaneously to the nearest surface detector tank for hybrid timing analyses. We describe the facility and show some examples of its many uses
Discriminating potential astrophysical sources of the highest energy cosmic rays with the Pierre Auger Observatory
No full textUniversity of Adelaide participants in the Pierre Auger Collaboration: ... K. B. Barber... J. A. Bellido... R. W. Clay... B. R. Dawson... V. C. Holmes... P. Wahrlich... B. J. Whelan... M. G. WinnickWe compare the distribution of arrival directions of the highest energy cosmic rays detected by the Pierre Auger Observatory from 1 January 2004 to 31March 2009 with that of populations of potential astrophysical sources. For this purpose, we use several complementary statistical tests allowing one to describe and quantify the degree of compatibility between data and a given catalogue of sources. We applied these tests to active galactic nuclei detected in X-rays by SWIFT-BAT and to galaxies found in the HI Parkes and in the 2 Micron All-Sky Surveys.Julien Aublin, for the Pierre Auger Collaborationhttp://inspire.ornl.gov/Document/View/a22a2303-94d8-4649-8918-3000fa8eeccd?q=topic%3A%22Physics%2
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No full textpod auger nHoles for the trunnels were bored with a T handled pod auger, a tool like a gigantic gimlet in that it had a long, sharpened gouge ending in a screw or "worm" to carry it into the wood. That tool was the ancestor of the modern and more familiar spiral auger. The expression, 'back in pod auger days,' meaning very old fashioned, refers to the time when pod augers were in use.[Add to DNE pod auger, to P.1979 quot] PRINTED ITEMDNE Sup G. M. StoryAUG 1 1989 WKUsed I and SupUsed I and SupUsed Su
Searches for Ultra-High-Energy Photons at the Pierre Auger Observatory
No full textPublished: 2 November 2022The Pierre Auger Observatory, which is the largest air-shower experiment in the world, offers unprecedented exposure to neutral particles at the highest energies. Since the start of data collection more than 18 years ago, various searches for ultra-high-energy (UHE, E≳1017eV) photons have been performed, either for a diffuse flux of UHE photons, for point sources of UHE photons or for UHE photons associated with transient events such as gravitational wave events. In the present paper, we summarize these searches and review the current results obtained using the wealth of data collected by the Pierre Auger Observatory.The Pierre Auger Collaboration: P. Abreu ... J.A. Bellido ... R.W. Clay ... B.R. Dawson ... T.D. Grubb ... V.M. Harvey ... B.C. Manning ... T. Sudholz ... et al
Le R. P. Mersenne et la physique.
No full textAuger Léon. Le R. P. Mersenne et la physique.. In: Revue d'histoire des sciences et de leurs applications, tome 2, n°1, 1948. pp. 33-52
Reconstruction of events recorded with the surface detector of the Pierre Auger Observatory
No full textInternational audienceCosmic rays arriving at Earth collide with the upper parts of the atmosphere, thereby inducing extensive air showers. When secondary particles from the cascade arrive at the ground, they are measured by surface detector arrays. We describe the methods applied to the measurements of the surface detector of the Pierre Auger Observatory to reconstruct events with zenith angles less than 60ˆ using the timing and signal information recorded using the water-Cherenkov detector stations. In addition, we assess the accuracy of these methods in reconstructing the arrival directions of the primary cosmic ray particles and the sizes of the induced showers
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