1 / 25

Study of cosmic ray shower front and time structure with ARGO-YBJ

Study of cosmic ray shower front and time structure with ARGO-YBJ . A. Karen C. M., Lorenzo Perrone. NEW FEATURES Larger statistics simulations. Allows comparison of simulation to data. Definition of observables. ….from ICRC07.

nyoko
Download Presentation

Study of cosmic ray shower front and time structure with ARGO-YBJ

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Study of cosmic ray shower front and time structure with ARGO-YBJ A. Karen C. M., Lorenzo Perrone

  2. NEW FEATURES Larger statistics simulations Allows comparison of simulation to data

  3. Definition of observables ….from ICRC07 The curvature of the shower front as the mean of time residuals with respect to a planar fit (Td) The thickness of the shower front as the root mean square (RMS) of time residuals with respect to a conical fit(TS)

  4. Definition of observables ….from Kascade-Grande Shower axis - trajectory of the incident primary cosmic ray particle towards the obervation level Shower plane – plane perpendicular to the shower axis R – radial distance from the shower core The shower disk refers to the curved disk of secondary shower particles towards earth

  5. Mean arrival time vs distance to shower core Thickness vs distance to shower core ….from Kascade-Grande

  6. Shower Reconstruction In EAS experiments for an event E the time tEP can be measured on each fired detector unit P, whose position (xP,yP) is well known Primary direction cosines Planar Fit Conical Fit This quantity is not a proper c2 . Indeed the measurement unit is ns2

  7. Data Selection Cuts used for ICRC07 • A successful reconstruction of the global shower observables is required • Nhit > 20 • Reconstructed shower core coordinates are within the central carpet • Sub-sample well reconstructed days 006-007 2009 (new data sample) • Zenith angle less than 15° Room left for more accurate event selection and quality cuts

  8. Data Shower curvature Mean of the time residuals (from Planar fit) profile as a function of the core distance for different pad multiplicities

  9. Data Shower thickness RMS of time residuals (from Conical fit) profile as a function of the core distance for different pad different multiplicities statistical errors :errors on the mean

  10. Larger statistics simulations Production of Corsika showers with Grid - Corsika 6720 - SIBYLL as high energy interaction model - FLUKA as low energy interaction model - dN/dE ~ E-1 300 GeV - 300 TeV - dN/d ~ sincos 0-45° August 2008 - December 2008 Used se : ts.infn.it Used ce : pi.infn.it ba.infn.it na.infn.it (only tested)‏ ihep.ac.cn (only tested)‏ cnaf.infn.it (heavyly used)‏ ~ 107 showers ~ 2.3 Tera

  11. Generated Sample vs Energy-Zenith 100 TeV 10 TeV 1 TeV

  12. Processing through argog at CNAF Generation area: 200× 200 m2 Each shower is used up to 10 times after re-sampling the core position Overall simulated data set ~ 107 events Argog processing time at CNAF: 100 CPU ~36 hours Motivation: cross checking the dependence on hadronic models for the cross-section analysis and time front structure

  13. Simulated Events vs Energy-Angle 100 TeV 10 TeV 1 TeV

  14. Usage of individual showers vs Energy-Angle 100 TeV 10 TeV 1 TeV

  15. Xmax from corsika fit to the longitudinal profiles included in the produced corsika binary files

  16. Summary - The production on GRID relatively smooth (GRID malfunctioning limited to short time windows) - Problems with the ``time bomb'' implemented in FLUKA. This periodically requires a new installation if the production takes longer than few months. (FLUKA doesn't distribute the source code. No way to by-pass this ``feature'' in a clean way). It makes almost impossible to reproduce a given shower generated in the ``past'' Common problem for several experiments. The community is considering to move to UrQMD . It behaves similarly as FLUKA at least in the TeV range (Geisha is not manteined any longer)‏ Showers available at /storage/gpfs_argo1/Production/MC/Corsika6.7201 2.3 Tb

  17. Simulation Shower curvature Mean of the time residuals (from Planar fit) profile as a function of the core distance for pad different multiplicities

  18. Simulation Shower thickness RMS of time residuals (from Conical fit) profile as a function of the core distance at different multiplicities statistical errors :errors on the mean

  19. Comparison data with MC Zenith Angle distribution

  20. Comparison data with MC Mean of the time residuals (from Planar fit) profile: good agreement between data and simulation

  21. Comparison data with MC Mean of the time residuals (from Planar fit) profile: good agreement between data and simulation

  22. Comparison data with MC Mean of the time residuals (from Planar fit) profile: sensible differences between data and simulation for lower pad multiplicities

  23. Comparison data with MC nhit 200-400 RMS of time residuals (from Conical fit) profile: to be investigated

  24. What else can we learn of shower phenomenology….. Observable true value Moderate correlation of conicity with Xmax for protons New fit with alpha free

  25. What’s more….

More Related